Benjamin J Weiner

Interests

Research

Benjamin Weiner's research investigates the nature and evolution of star-forming and active galaxies from the present day back to half the age of the universe ago. His recent projects grow out of large redshift surveys combined with multi-wavelength data, including far-IR measurements from Spitzer and Herschel, to measure infrared luminosities and star formation rates, and optical spectroscopy to measure redshifts and make detailed analyses of galaxy properties.

Courses

No activities entered.

Scholarly Contributions

Journals/Publications

• Chen, Y., Jones, T., Sanders, R. L., Fadda, D., Sutter, J., Minchin, R., Prusinski, N. Z., Rhoades, S., Keerthi Vasan, G. C., Steidel, C. C., Huntzinger, E., Kelly, P., Berg, D. A., Bresolin, F., Herrera-Camus, R., Rickards Vaught, R. J., Roberts-Borsani, G., Senchyna, P., Spilker, J. S., , Stark, D. P., et al. (2026). Joint Optical and Infrared Observations of Nitrogen and Oxygen Reveal the Dust-obscured Gas in Haro 3. Astrophysical Journal, 1000(Issue 1). doi:10.3847/1538-4357/ae473e
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  Accurate chemical compositions of star-forming regions provide a critical diagnostic tool for characterizing the star formation history and gas flows that regulate galaxy formation. However, the abundance discrepancy factor (ADF) between measurements derived from the “direct” optical electron temperature (Te ) method and those from recombination lines (RLs) introduces a ∼0.2 dex systematic uncertainty in the oxygen abundance. The degree of uncertainty for other elements is unknown. We conduct a comprehensive analysis of O++ and N+ ion abundances using optical and far-infrared (far-IR) spectra of a star-forming region within the nearby dwarf galaxy Haro 3, which exhibits a typical ADF. Assuming homogeneous conditions, the far-IR emission indicates an oxygen abundance higher than that derived using the Te method and consistent with the RL value, as expected from temperature fluctuations, whereas the far-IR nitrogen abundance is too large to be explained by temperature fluctuations. A two-phase analytical model reveals that differential dust obscuration associated with temperature inhomogeneity is likely required to explain all the emission-line ratios, and that the total oxygen metallicity of two phases is consistent with the RL metallicity. Our findings underscore the critical importance of resolving the cause of abundance discrepancies and understanding the biases between different metallicity methods. This work presents a promising methodology, and we identify further approaches to address the dominant sources of uncertainty.
• Asali, Y., Geha, M., Kado-Fong, E., Mao, Y. Y., Wechsler, R. H., De los Reyes, M. A., Pasha, I., Kallivayalil, N., Nadler, E. O., Tollerud, E. J., Wang, Y., Weiner, B., & Wu, J. F. (2025). The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments. Astrophysical Journal, 995(Issue 1). doi:10.3847/1538-4357/ae147d
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  We investigate how Milky Way (MW)–like environments influence the sizes and structural properties of low-mass galaxies by comparing satellites of MW analogs from the Satellites Around Galactic Analogs (SAGA) Survey with two control samples: an environmentally agnostic population from the SAGA background sample and isolated galaxies from the Sloan Digital Sky Survey NASA-Sloan Atlas. All sizes and structural parameters are measured uniformly using pysersic to ensure consistency across samples. We find the half-light sizes of SAGA satellites are systematically larger than those of isolated galaxies, with the magnitude of the offset ranging from 0.05 to 0.12 dex (10%–24%) depending on the comparison sample and completeness cuts. This corresponds to physical size differences between 85 and 200 pc at log 10 (M ⋆ / M ⊙) = 7.5 and 220–960 pc at log 10 (M ⋆ / M ⊙) = 10. This offset persists among star-forming galaxies, suggesting that environment can influence the structure of low-mass galaxies even before it impacts quenching. The intrinsic scatter in the size–mass relation is lower for SAGA satellites than isolated galaxies, and the Sérsic index distributions of satellites and isolated galaxies are similar. In comparison to star-forming satellites, quenched SAGA satellites have a slightly shallower size–mass relation and rounder morphologies at low mass, suggesting that quenching is accompanied by structural transformation and that the processes responsible differ between low- and high-mass satellites. Our results show that environmental processes can imprint measurable structural differences on satellites in MW-mass halos.
• Cole, J. W., Papovich, C., Finkelstein, S. L., Bagley, M. B., Dickinson, M., Iyer, K. G., Yung, L. Y., Ciesla, L., Amorín, R. O., Arrabal Haro, P., Bhatawdekar, R., Calabrò, A., Cleri, N. J., de la Vega, A., Dekel, A., Endsley, R., Gawiser, E., Giavalisco, M., Hathi, N. P., , Hirschmann, M., et al. (2025). CEERS: Increasing Scatter along the Star-forming Main Sequence Indicates Early Galaxies Form in Bursts. Astrophysical Journal, 979(Issue 2). doi:10.3847/1538-4357/ad9a6a
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  We present the star formation rate-stellar mass (SFR-M*) relation for galaxies in the Cosmic Evolution Early Release Science survey at 4.5 ≤ z ≤ 12. We model the JWST and Hubble Space Telescope rest-UV and rest-optical photometry of galaxies with flexible star formation histories (SFHs) using BAGPIPES. We consider SFRs averaged from the SFHs over 10 Myr (SFR10) and 100 Myr (SFR100), where the photometry probes SFRs on these timescales, effectively tracing nebular emission lines in the rest-optical (on ~10 Myr timescales) and the UV/optical continuum (on ~100 Myr timescales). We measure the slope, normalization and intrinsic scatter of the SFR-M* relation, taking into account the uncertainty and the covariance of galaxy SFRs and M*. From z ~ 5 to 9 there is larger scatter in the SFR10-M* relation, with σ ( log S F R 100 ) = 0.4 dex, compared to the SFR100-M* relation, with σ ( log S F R 10 ) = 0.1 dex. This scatter increases with redshift and increasing stellar mass, at least out to z ~ 7. These results can be explained if galaxies at higher redshift experience an increase in star formation variability and form primarily in short, active periods, followed by a lull in star formation (i.e., “napping” phases). We see a significant trend in the ratio RSFR = SFR10/SFR100 in which, on average, RSFR decreases with increasing stellar mass and increasing redshift. This yields a star formation “duty cycle” of ~40% for galaxies with log M * / M ⊙ ≥ 9.3 at z ~ 5, declining to ~20% at z ~ 9. Galaxies also experience longer lulls in star formation at higher redshift and at higher stellar mass, such that galaxies transition from periods of higher SFR variability at z ≳ 6 to smoother SFR evolution at z ≲ 4.5.
• Finkelstein, S. L., Bagley, M. B., Arrabal Haro, P., Dickinson, M., Ferguson, H. C., Kartaltepe, J. S., Kocevski, D. D., Koekemoer, A. M., Lotz, J. M., Papovich, C., Pérez-González, P. G., Pirzkal, N., Somerville, R. S., Trump, J. R., Yang, G., Yung, L. Y., Fontana, A., Grazian, A., Grogin, N. A., , Kewley, L. J., et al. (2025). The Cosmic Evolution Early Release Science Survey (CEERS). Astrophysical Journal Letters, 983(Issue 1). doi:10.3847/2041-8213/adbbd3
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  We present the Cosmic Evolution Early Release Science (CEERS) Survey, a 77.2 hr Director’s Discretionary Early Release Science Program. CEERS demonstrates, tests, and validates efficient extragalactic surveys using coordinated, overlapping parallel observations with the JWST instrument suite, including NIRCam and MIRI imaging, NIRSpec low- (R ∼ 100) and medium- (R ∼ 1000) resolution spectroscopy, and NIRCam slitless grism (R ∼ 1500) spectroscopy. CEERS targets the Hubble Space Telescope-observed region of the Extended Groth Strip field, supported by a rich set of multiwavelength data. CEERS facilitated immediate community science in both of the extragalactic core JWST science drivers “First Light” and “Galaxy Assembly,” including: (1) the discovery and characterization of large samples of galaxies at z ≳ 10 from ∼90 arcmin2 of NIRCam imaging, constraining their abundance and physical nature; (2) deep spectra of >1000 galaxies, including dozens of galaxies at 6 < z < 10, enabling redshift measurements and constraints on the physical conditions of star formation and black hole growth via line diagnostics; (3) quantifying the first bulge, bar, and disk structures at z > 3; and (4) characterizing galaxy mid-IR emission with MIRI to study dust-obscured star formation and supermassive black hole growth at z ∼ 1-3. As a legacy product for the community, the CEERS team has provided several data releases, accompanied by detailed notes on the data reduction procedures and notebooks to aid in reproducibility. In addition to an overview of the survey and the quality of the data, we provide science highlights from the first two years with CEERS data.
• Franz, N., Subrayan, B., Kilpatrick, C. D., Hosseinzadeh, G., Sand, D. J., Alexander, K. D., Fong, W. F., Christy, C. T., Pearson, J., Laskar, T., Hsu, B., Rastinejad, J., Lundquist, M. J., Berger, E., Bostroem, K. A., Bom, C. R., Darc, P., Gurwell, M., Schimpf, S. H., , Keating, G. K., et al. (2025). Optimizing Kilonova Searches: A Case Study of the Type IIb SN2025ulz in the Localization Volume of the Low-significance Gravitational Wave Event S250818k. Astrophysical Journal Letters, 994(Issue 2). doi:10.3847/2041-8213/ae17a8
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  Kilonovae, the ultraviolet/optical/infrared counterparts to binary neutron star mergers, are an exceptionally rare class of transients. Optical follow-up campaigns are plagued by contaminating transients, which may mimic kilonovae but do not receive sufficient observations to measure the full photometric evolution. In this work, we present an analysis of the multiwavelength dataset of supernova (SN) 2025ulz, a proposed kilonova candidate following the low-significance detection of gravitational waves originating from the potential binary neutron star merger S250818k. Despite an early rapid decline in brightness, our multiwavelength observations of SN 2025ulz reveal that it is a type IIb SN. As part of this analysis, we demonstrate the capabilities of a novel quantitative scoring algorithm to determine the likelihood that a transient candidate is a kilonova, based primarily on its three-dimensional location and light-curve evolution. We also apply our scoring algorithm to other transient candidates in the localization volume of S250818k and find that, at all times after the discovery of SN 2025ulz, there are ≽4 candidates with a score comparable to SN 2025ulz, indicating that the kilonova search may have benefited from the additional follow-up of other candidates. During future kilonova searches, this type of scoring algorithm will be useful to rule out contaminating transients in real time, optimizing the use of valuable telescope resources.
• Kado-Fong, E., Mao, Y. Y., Asali, Y., Geha, M., Wechsler, R. H., De los Reyes, M. A., Wang, Y., Nadler, E. O., Kallivayalil, N., Tollerud, E. J., & Weiner, B. (2025). SAGAbg. III. Environmental Stellar Mass Functions, Self-quenching, and the Stellar-to-halo Mass Relation in the Dwarf Galaxy Regime. Astrophysical Journal, 994(Issue 2). doi:10.3847/1538-4357/ae102d
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  Recent efforts have extended our view of the number and properties of satellite galaxies beyond the Local Group firmly down to M⋆ ∼ 106 M⊙. A similarly complete view of the field dwarf population has lagged behind. Using the background galaxy sample from the Satellites Around Galactic Analogs (SAGA) survey at z < 0.05, we take inventory of the dwarf population down to M⋆ ∼ 5 × 106 M⊙ using three metrics: the stellar mass function (SMF) as a function of environment, the stellar-to-halo mass relation (SHMR) of dwarf galaxies inferred via abundance matching, and the quenched fraction of highly isolated dwarfs. We find that the low-mass SMF shape shows minimal environmental dependence, with the field dwarf SMF described by a low-mass power-law index of α 1 = −1.44 ± 0.09 down to M ⋆ ∼ 5 × 106 M⊙, and that the quenched fraction of isolated dwarfs drops monotonically to fq ∼ 10−3 at M⋆ ∼ 108.5 M⊙. Though slightly steeper than estimates from H i kinematic measures, our inferred SHMR agrees with literature measurements of satellite systems, consistent with minimal environmental dependence of the SHMR in the probed mass range. Finally, although most contemporary cosmological simulations against which we compare accurately predict the SAGAbg-SMF SHMR, we find that big-box cosmological simulations largely overpredict isolated galaxy quenched fractions via a turnaround in fq(M⋆) at 108 ≲ M⋆/M⊙ ≲ 109, underscoring the complexities in disentangling the drivers of galaxy formation and the need for systematic multidimensional observations of the dwarf population across environments.
• Geha, M., Mao, Y., Wechsler, R. H., Asali, Y., Kado-Fong, E., Kallivayalil, N., Nadler, E. O., Tollerud, E. J., Weiner, B., Reyes, M. A., Wang, Y., & Wu, J. F. (2024). The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way\textendashmass Galaxies. \apj, 976(1), 118.
• Kado-Fong, E., Geha, M., Mao, Y., Reyes, M. A., Wechsler, R. H., Asali, Y., Kallivayalil, N., Nadler, E. O., Tollerud, E. J., & Weiner, B. (2024). SAGAbg. I. A Near-unity Mass-loading Factor in Low-mass Galaxies via Their Low-redshift Evolution in Stellar Mass, Oxygen Abundance, and Star Formation Rate. \apj, 966(1), 129.
• Kado-Fong, E., Geha, M., Mao, Y., Reyes, M. A., Wechsler, R. H., Weiner, B., Asali, Y., Kallivayalil, N., Nadler, E. O., Tollerud, E. J., & Wang, Y. (2024). SAGAbg. II. The Low-mass Star-forming Sequence Evolves Significantly between 0.05 < z < 0.21. \apj, 976(1), 83.
• Mao, Y., Geha, M., Wechsler, R. H., Asali, Y., Wang, Y., Kado-Fong, E., Kallivayalil, N., Nadler, E. O., Tollerud, E. J., Weiner, B., Reyes, M. A., & Wu, J. F. (2024). The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way\textendashmass Galaxies. \apj, 976(1), 117.
• Shrestha, M., Pearson, J., Wyatt, S., Sand, D. J., Hosseinzadeh, G., Bostroem, K. A., Andrews, J. E., Dong, Y., Hoang, E., Janzen, D., Jencson, J. E., Lundquist, M., Mehta, D., Retamal, N. M., Valenti, S., Rastinejad, J. C., Daly, P., Porter, D., Hinz, J., , Self, S., et al. (2024). Evidence of Weak Circumstellar Medium Interaction in the Type II SN 2023axu. \apj, 961(2), 247.
• Thornton, J., Amon, A., Wechsler, R. H., Adhikari, S., Mao, Y., Myles, J., Geha, M., Kallivayalil, N., Tollerud, E., & Weiner, B. (2024). The mass profiles of dwarf galaxies from Dark Energy Survey lensing. \mnras, 535(1), 1-20.
• Wang, Y., Nadler, E. O., Mao, Y., Wechsler, R. H., Abel, T., Behroozi, P., Geha, M., Asali, Y., Reyes, M. A., Kado-Fong, E., Kallivayalil, N., Tollerud, E. J., Weiner, B., & Wu, J. F. (2024). The SAGA Survey. V. Modeling Satellite Systems around Milky Way\textendashMass Galaxies with Updated UNIVERSEMACHINE. \apj, 976(1), 119.
• Alexander, D. M., Davis, T. M., Chaussidon, E., Fawcett, V., X., G. A., Lan, T., Y{\`eche}, C., Ahlen, S., Aguilar, J., Armengaud, E., Bailey, S., Brooks, D., Cai, Z., Canning, R., Carr, A., Chabanier, S., Cousinou, M., Dawson, K., Macorra, A., , Dey, A., et al. (2023). The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra. \aj, 165(3), 124.
• Arrabal, H. P., Dickinson, M., Finkelstein, S. L., Fujimoto, S., Fern{\'andez}, V., Kartaltepe, J. S., Jung, I., Cole, J. W., Burgarella, D., Chworowsky, K., Hutchison, T. A., Morales, A. M., Papovich, C., Simons, R. C., Amor{\'\in}, R. O., Backhaus, B. E., Bagley, M. B., Bisigello, L., Calabr{\`o}, A., , Castellano, M., et al. (2023). Spectroscopic Confirmation of CEERS NIRCam-selected Galaxies at z ??? 8-10. \apjl, 951(1), L22.
• Arrabal, H. P., Dickinson, M., Finkelstein, S. L., Kartaltepe, J. S., Donnan, C. T., Burgarella, D., Carnall, A. C., Cullen, F., Dunlop, J. S., Fern{\'andez}, V., Fujimoto, S., Jung, I., Krips, M., Larson, R. L., Papovich, C., P{\'erez-Gonz\'alez}, P. G., Amor{\'\in}, R. O., Bagley, M. B., Buat, V., , Casey, C. M., et al. (2023). Confirmation and refutation of very luminous galaxies in the early Universe. \nat, 622(7984), 707-711.
• Chen, Y., Jones, T., Sanders, R., Fadda, D., Sutter, J., Minchin, R., Huntzinger, E., Senchyna, P., Stark, D., Spilker, J., Weiner, B., & Roberts-Borsani, G. (2023). Accurate oxygen abundance of interstellar gas in Mrk 71 from optical and infrared spectra. Nature Astronomy, 7, 771-778.
• Cleri, N. J., Yang, G., Papovich, C., Trump, J. R., Backhaus, B. E., Estrada-Carpenter, V., Finkelstein, S. L., Giavalisco, M., Hutchison, T. A., Ji, Z., Jung, I., Matharu, J., Momcheva, I., Olivier, G. M., Simons, R., & Weiner, B. (2023). CLEAR: High-ionization [Ne V] \ensuremath{\lambda}3426 Emission-line Galaxies at 1.4 < z < 2.3. \apj, 948(2), 112.
• Cleri, N. J., Yang, G., Papovich, C., Trump, J. R., Backhaus, B. E., Estrada-Carpenter, V., Finkelstein, S. L., Giavalisco, M., Hutchison, T. A., Ji, Z., Jung, I., Matharu, J., Momcheva, I., Olivier, G. M., Simons, R., & Weiner, B. (2023). CLEAR: High-ionization [Ne v] λ3426 Emission-line Galaxies at 1.4 < z < 2.3. Astrophysical Journal, 948(Issue 2). doi:10.3847/1538-4357/acc1e6
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  We analyze a sample of 25 [Ne v] (λ3426) emission-line galaxies at 1.4 < z < 2.3 using Hubble Space Telescope/Wide Field Camera 3 G102 and G141 grism observations from the CANDELS Lyα Emission at Reionization (CLEAR) survey. [Ne v] emission probes extremely energetic photoionization (creation potential of 97.11 eV) and is often attributed to energetic radiation from active galactic nuclei (AGNs), shocks from supernovae, or an otherwise very hard ionizing spectrum from the stellar continuum. In this work, we use [Ne v] in conjunction with other rest-frame UV/optical emission lines ([O ii] λ λ3726, 3729, [Ne iii] λ3869, Hβ, [O iii] λ λ4959, 5007, Hα+[N ii] λ λ6548, 6583, [S ii] λ λ6716, 6731), deep (2-7 Ms) X-ray observations (from Chandra), and mid-infrared imaging (from Spitzer) to study the origin of this emission and to place constraints on the nature of the ionizing engine. The majority of the [Ne v]-detected galaxies have properties consistent with ionization from AGNs. However, for our [Ne v]-selected sample, the X-ray luminosities are consistent with local (z ≲ 0.1) X-ray-selected Seyferts, but the [Ne v] luminosities are more consistent with those from z ∼ 1 X-ray-selected QSOs. The excess [Ne v] emission requires either reduced hard X-rays or a ∼0.1 keV excess. We discuss possible origins of the apparent [Ne v] excess, which could be related to the “soft (X-ray) excess” observed in some QSOs and Seyferts and/or be a consequence of a complex/anisotropic geometry for the narrow-line region, combined with absorption from a warm, relativistic wind ejected from the accretion disk. We also consider implications for future studies of extreme high-ionization systems in the epoch of reionization (z ≳ 6) with the James Webb Space Telescope.
• Darragh-Ford, E., Wu, J. F., Mao, Y., Wechsler, R. H., Geha, M., Forero-Romero, J. E., Hahn, C., Kallivayalil, N., Moustakas, J., Nadler, E. O., Nowotka, M., Peek, J., Tollerud, E. J., Weiner, B., Aguilar, J., Ahlen, S., Brooks, D., Cooper, A., Macorra, A., , Dey, A., et al. (2023). Target Selection and Sample Characterization for the DESI LOW-Z Secondary Target Program. \apj, 954(2), 149.
• Estrada-Carpenter, V., Papovich, C., Momcheva, I., Brammer, G., Simons, R. C., Cleri, N. J., Giavalisco, M., Matharu, J., Trump, J. R., Weiner, B., & Ji, Z. (2023). CLEAR: The Morphological Evolution of Galaxies in the Green Valley. \apj, 951(2), 115.
• Finkelstein, S. L., Bagley, M. B., Ferguson, H. C., Wilkins, S. M., Kartaltepe, J. S., Papovich, C., Yung, L. A., Arrabal, H. P., Behroozi, P., Dickinson, M., Kocevski, D. D., Koekemoer, A. M., Larson, R. L., Le, B. A., Morales, A. M., P{\'erez-Gonz\'alez}, P. G., Burgarella, D., Dav{\'e}, R., Hirschmann, M., , Somerville, R. S., et al. (2023). CEERS Key Paper. I. An Early Look into the First 500 Myr of Galaxy Formation with JWST. \apjl, 946(1), L13.
• Fujimoto, S., Finkelstein, S. L., Burgarella, D., Carilli, C. L., Buat, V., Casey, C. M., Ciesla, L., Tacchella, S., Zavala, J. A., Brammer, G., Fudamoto, Y., Ouchi, M., Valentino, F., Cooper, M., Dickinson, M., Franco, M., Giavalisco, M., Hutchison, T. A., Kartaltepe, J. S., , Koekemoer, A. M., et al. (2023). ALMA FIR View of Ultra-high-redshift Galaxy Candidates at z \ensuremath{\sim} 11-17: Blue Monsters or Low-z Red Interlopers?. \apj, 955(2), 130.
• Hahn, C., Kwon, K., Tojeiro, R., Siudek, M., Canning, R. E., Mezcua, M., Tinker, J. L., Brooks, D., Doel, P., Fanning, K., Gazta{\~naga}, E., Kehoe, R., Landriau, M., Meisner, A., Moustakas, J., Poppett, C., Tarle, G., Weiner, B., & Zou, H. u. (2023). The DESI PRObabilistic Value-added Bright Galaxy Survey (PROVABGS) Mock Challenge. \apj, 945(1), 16.
• Lan, T., Tojeiro, R., Armengaud, E., Prochaska, J. X., Davis, T., Alexander, D. M., Raichoor, A., Zhou, R., Y{\`eche}, C., Balland, C., BenZvi, S., Berti, A., Canning, R., Carr, A., Chittenden, H., Cole, S., Cousinou, M. -., Dawson, K., Dey, B., , Douglass, K., et al. (2023). The DESI Survey Validation: Results from Visual Inspection of Bright Galaxies, Luminous Red Galaxies, and Emission-line Galaxies. \apj, 943(1), 68.
• Larson}, R. L., Finkelstein, S. L., Kocevski, D. D., Hutchison, T. A., Trump, J. R., Arrabal, H. P., Bromm, V., Cleri, N. J., Dickinson, M., Fujimoto, S., Kartaltepe, J. S., Koekemoer, A. M., Papovich, C., Pirzkal, N., Tacchella, S., Zavala, J. A., Bagley, M., Behroozi, P., Champagne, J. B., , Cole, J. W., et al. (2023). A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars. \apjl, 953(2), L29.
• Napolitano, L., Pandey, A., Myers, A. D., Lan, T., Anand, A., Aguilar, J., Ahlen, S., Alexander, D. M., Brooks, D., Canning, R., Circosta, C., De, L., Doel, P., Eftekharzadeh, S., Fawcett, V. A., Font-Ribera, A., Garcia-Bellido, J., Gontcho, A., Le Guillou, L., , Guy, J., et al. (2023). Detecting and Characterizing Mg II Absorption in DESI Survey Validation Quasar Spectra. \aj, 166(3), 99.
• Papovich, C., Cole, J. W., Yang, G., Finkelstein, S. L., Barro, G., Buat, V., Burgarella, D., P{\'erez-Gonz\'alez}, P. G., Santini, P., Seill{\'e}, L., Shen, L. u., Arrabal, H. P., Bagley, M. B., Bell, E. F., Bisigello, L., Calabr{\`o}, A., Casey, C. M., Castellano, M., Chworowsky, K., , Cleri, N. J., et al. (2023). CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear\textendashCharacterizing Galaxy Stellar Populations from Rest-frame \ensuremath{\sim}1 \ensuremath{\mu}m Imaging. \apjl, 949(2), L18.
• Papovich, C., Cole, J. W., Yang, G., Finkelstein, S. L., Barro, G., Buat, V., Burgarella, D., Pérez-González, P. G., Santini, P., Seillé, L. M., Shen, L., Haro, P. A., Bagley, M. B., Bell, E. F., Bisigello, L., Calabrò, A., Casey, C. M., Castellano, M., Chworowsky, K., , Cleri, N. J., et al. (2023). CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear-Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging. Astrophysical Journal Letters, 949(Issue 2). doi:10.3847/2041-8213/acc948
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  We present results from the Cosmic Evolution Early Release Survey on the stellar population parameters for 28 galaxies with redshifts 4 < z < 9 using imaging data from the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) combined with data from the Hubble Space Telescope and the Spitzer Space Telescope. The JWST/MIRI 5.6 and 7.7 μm data extend the coverage of the rest-frame spectral energy distribution to nearly 1 μm for galaxies in this redshift range. By modeling the galaxies’ SEDs the MIRI data show that the galaxies have, on average, rest-frame UV (1600 Å)—I-band colors 0.4 mag bluer than derived when using photometry that lacks MIRI. Therefore, the galaxies have lower ratios of stellar mass to light. The MIRI data reduce the stellar masses by 〈 Δ log M * 〉 = 0.25 dex at 4 < z < 6 and 0.37 dex at 6 < z < 9. This also reduces the star formation rates (SFRs) by 〈ΔlogSFR〉 = 0.14 dex at 4 < z < 6 and 0.27 dex at 6 < z < 9. The MIRI data also improve constraints on the allowable stellar mass formed in early star formation. We model this using a star formation history that includes both a “burst” at z f = 100 and a slowly varying (“delayed-τ”) model. The MIRI data reduce the allowable stellar mass by 0.6 dex at 4 < z < 6 and by ≈1 dex at 6 < z < 9. Applying these results globally, this reduces the cosmic stellar-mass density by an order of magnitude in the early Universe (z ≈ 9). Therefore, observations of rest-frame ≳1 μm are paramount for constraining the stellar-mass buildup in galaxies at very high redshifts.
• Shen, L. u., Papovich, C., Yang, G., Matharu, J., Wang, X., Magnelli, B., Elbaz, D., Jogee, S., Alavi, A., Arrabal, H. P., Backhaus, B. E., Bagley, M. B., Bell, E. F., Bisigello, L., Calabr{\`o}, A., Cooper, M., Costantin, L., Daddi, E., Dickinson, M., , Finkelstein, S. L., et al. (2023). CEERS: Spatially Resolved UV and Mid-infrared Star Formation in Galaxies at 0.2 < z < 2.5: The Picture from the Hubble and James Webb Space Telescopes. \apj, 950(1), 7.
• Simons, R. C., Papovich, C., Momcheva, I. G., Brammer, G., Estrada-Carpenter, V., Finkelstein, S. L., Gosmeyer, C. M., Matharu, J., Trump, J. R., Backhaus, B. E., Cheng, Y., Cleri, N. J., Ferguson, H. C., Finlator, K., Giavalisco, M., Ji, Z., Jung, I., Lotz, J. M., O'Brien, R., , Skelton, R. E., et al. (2023). CLEAR: Survey Overview, Data Analysis, and Products. \apjs, 266(1), 13.
• Trump, J. R., Arrabal, H. P., Simons, R. C., Backhaus, B. E., Amor{\'\in}, R. O., Dickinson, M., Fern{\'andez}, V., Papovich, C., Nicholls, D. C., Kewley, L. J., Brunker, S. W., Salzer, J. J., Wilkins, S. M., Almaini, O., Bagley, M. B., Berg, D. A., Bhatawdekar, R., Bisigello, L., Buat, V., , Burgarella, D., et al. (2023). The Physical Conditions of Emission-line Galaxies at Cosmic Dawn from JWST/NIRSpec Spectroscopy in the SMACS 0723 Early Release Observations. \apj, 945(1), 35.
• Zavala, J. A., Buat, V., Casey, C. M., Finkelstein, S. L., Burgarella, D., Bagley, M. B., Ciesla, L., Daddi, E., Dickinson, M., Ferguson, H. C., Franco, M., Jiménez-Andrade, E. F., Kartaltepe, J. S., Koekemoer, A. M., Bail, A. L., Murphy, E. J., Papovich, C., Tacchella, S., Wilkins, S. M., , Aretxaga, I., et al. (2023). Dusty Starbursts Masquerading as Ultra-high Redshift Galaxies in JWST CEERS Observations. Astrophysical Journal Letters, 943(Issue 2). doi:10.3847/2041-8213/acacfe
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  Lyman-break galaxy (LBG) candidates at z ≳ 10 are rapidly being identified in James Webb Space Telescope (JWST)/NIRCam observations. Due to the (redshifted) break produced by neutral hydrogen absorption of rest-frame UV photons, these sources are expected to drop out in the bluer filters while being well detected in redder filters. However, here we show that dust-enshrouded star-forming galaxies at lower redshifts (z ≲ 7) may also mimic the near-infrared (near-IR) colors of z > 10 LBGs, representing potential contaminants in LBG candidate samples. First, we analyze CEERS-DSFG-1, a NIRCam dropout undetected in the F115W and F150W filters but detected at longer wavelengths. Combining the JWST data with (sub)millimeter constraints, including deep NOEMA interferometric observations, we show that this source is a dusty star-forming galaxy (DSFG) at z ≈ 5.1. We also present a tentative 2.6σ SCUBA-2 detection at 850 μm around a recently identified z ≈ 16 LBG candidate in the same field and show that, if the emission is real and associated with this candidate, the available photometry is consistent with a z ∼ 5 dusty galaxy with strong nebular emission lines despite its blue near-IR colors. Further observations on this candidate are imperative to mitigate the low confidence of this tentative submillimeter emission and its positional uncertainty. Our analysis shows that robust (sub)millimeter detections of NIRCam dropout galaxies likely imply z ∼ 4-6 redshift solutions, where the observed near-IR break would be the result of a strong rest-frame optical Balmer break combined with high dust attenuation and strong nebular line emission, rather than the rest-frame UV Lyman break. This provides evidence that DSFGs may contaminate searches for ultra-high redshift LBG candidates from JWST observations.
• Zavala}, J. A., Buat, V., Casey, C. M., Finkelstein, S. L., Burgarella, D., Bagley, M. B., Ciesla, L., Daddi, E., Dickinson, M., Ferguson, H. C., Franco, M., Jim{\'enez-Andrade}, E., Kartaltepe, J. S., Koekemoer, A. M., Le, B. A., Murphy, E., Papovich, C., Tacchella, S., Wilkins, S. M., , Aretxaga, I., et al. (2023). Dusty Starbursts Masquerading as Ultra-high Redshift Galaxies in JWST CEERS Observations. \apjl, 943(2), L9.
• Backhaus, B. E., Trump, J. R., Cleri, N. J., Simons, R., Momcheva, I., Papovich, C., Estrada-Carpenter, V., Finkelstein, S. L., Matharu, J., Ji, Z., Weiner, B., Giavalisco, M., & Jung, I. (2022). CLEAR: Emission-line Ratios at Cosmic High Noon. \apj, 926(2), 161.
• Cleri, N. J., Trump, J. R., Backhaus, B. E., Momcheva, I., Papovich, C., Simons, R., Weiner, B., Estrada-Carpenter, V., Finkelstein, S. L., Giavalisco, M., Ji, Z., Jung, I., Matharu, J., Martinez, F., & Sturm, M. R. (2022). CLEAR: Paschen- β Star Formation Rates and Dust Attenuation of Low-redshift Galaxies. Astrophysical Journal, 929(Issue 1). doi:10.3847/1538-4357/ac5a4c
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  We use Paschen-β (Paβ; 1282 nm) observations from the Hubble Space Telescope G141 grism to study the star formation and dust-attenuation properties of a sample of 29 low-redshift (z < 0.287) galaxies in the CANDELS Lyα Emission at Reionization survey. We first compare the nebular attenuation from Paβ/Hα with the stellar attenuation inferred from the spectral energy distribution, finding that the galaxies in our sample are consistent with an average ratio of the continuum attenuation to the nebular gas of 0.44, but with a large amount of excess scatter beyond the observational uncertainties. Much of this scatter is linked to a large variation between the nebular dust attenuation as measured by (space-based) Paβ to (ground-based) Hα to that from (ground-based) Hα/Hβ. This implies there are important differences between attenuation measured from grism-based/wide-aperture Paβ fluxes and the ground-based/slit-measured Balmer decrement. We next compare star formation rates (SFRs) from Paβ to those from dust-corrected UV. We perform a survival analysis to infer a census of Paβ emission implied by both detections and nondetections. We find evidence that galaxies with lower stellar mass have more scatter in their ratio of Paβ to attenuation-corrected UV SFRs. When considering our Paβ detection limits, this observation supports the idea that lower-mass galaxies experience "burstier"star formation histories. Together, these results show that Paβ is a valuable tracer of a galaxy's SFR, probing different timescales of star formation and potentially revealing star formation that is otherwise missed by UV and optical tracers.
• Cleri, N. J., Trump, J. R., Backhaus, B. E., Momcheva, I., Papovich, C., Simons, R., Weiner, B., Estrada-Carpenter, V., Finkelstein, S. L., Giavalisco, M., Ji, Z., Jung, I., Matharu, J., Martinez, F., & Sturm, M. R. (2022). CLEAR: Paschen-\ensuremath{\beta} Star Formation Rates and Dust Attenuation of Low-redshift Galaxies. \apj, 929(1), 3.
• Cooper, J. R., Rudnick, G. H., Brammer, G. G., Desjardins, T., Mann, J. L., Weiner, B. J., Arag{\'on-Salamanca}, A., De, L. G., Desai, V., Finn, R. A., Jablonka, P., Jaff{\'e}, Y. L., Moustakas, J., Sp{\'erone-Longin}, D., Teplitz, H. I., Vulcani, B., & Zaritsky, D. (2022). H \ensuremath{\alpha}-based star formation rates in and around z 0.5 EDisCS clusters. \mnras, 509(4), 5382-5398.
• Finkelstein}, S. L., Bagley, M. B., Arrabal, H. P., Dickinson, M., Ferguson, H. C., Kartaltepe, J. S., Papovich, C., Burgarella, D., Kocevski, D. D., Huertas-Company, M., Iyer, K. G., Koekemoer, A. M., Larson, R. L., P{\'erez-Gonz\'alez}, P. G., Rose, C., Tacchella, S., Wilkins, S. M., Chworowsky, K., Medrano, A., , Morales, A. M., et al. (2022). A Long Time Ago in a Galaxy Far, Far Away: A Candidate z \ensuremath{\sim} 12 Galaxy in Early JWST CEERS Imaging. \apjl, 940(2), L55.
• Matharu, J., Papovich, C., Simons, R. C., Momcheva, I., Brammer, G., Ji, Z., Backhaus, B. E., Cleri, N. J., Estrada-Carpenter, V., Finkelstein, S. L., Finlator, K., Giavalisco, M., Jung, I., Muzzin, A., Nelson, E. J., Pillepich, A., Trump, J. R., & Weiner, B. (2022). CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 \ensuremath{\lesssim} z \ensuremath{\lesssim} 1.7 Using H\ensuremath{\alpha} Emission Line Maps. \apj, 937(1), 16.
• Matharu, J., Papovich, C., Simons, R. C., Momcheva, I., Brammer, G., Ji, Z., Backhaus, B. E., Cleri, N. J., Estrada-Carpenter, V., Finkelstein, S. L., Finlator, K., Giavalisco, M., Jung, I., Muzzin, A., Nelson, E. J., Pillepich, A., Trump, J. R., & Weiner, B. (2022). CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between 0.5 ≲ z ≲ 1.7 Using Hα Emission Line Maps. Astrophysical Journal, 937(Issue 1). doi:10.3847/1538-4357/ac8471
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  Using spatially resolved Hα emission line maps of star-forming galaxies, we study the spatial distribution of star formation over a wide range in redshift (0.5 ≲ z ≲ 1.7). Our z ∼ 0.5 measurements come from deep Hubble Space Telescope (HST) Wide Field Camera 3 G102 grism spectroscopy obtained as part of the CANDELS Lyα Emission at Reionization Experiment. For star-forming galaxies with log(M */M ⊙) ≥ 8.96, the mean Hα effective radius is 1.2 ± 0.1 times larger than that of the stellar continuum, implying inside-out growth via star formation. This measurement agrees within 1σ with those measured at z ∼ 1 and z ∼ 1.7 from the 3D-HST and KMOS3D surveys, respectively, implying no redshift evolution. However, we observe redshift evolution in the stellar mass surface density within 1 kpc (Σ1kpc). Star-forming galaxies at z ∼ 0.5 with a stellar mass of log(M */M ⊙) = 9.5 have a ratio of Σ1kpc in Hα relative to their stellar continuum that is lower by (19 ± 2)% compared to z ∼ 1 galaxies. Σ1kpc,Hα /Σ1kpc,Cont decreases toward higher stellar masses. The majority of the redshift evolution in Σ1kpc,Hα /Σ1kpc,Cont versus stellar mass stems from the fact that log(Σ1kpc,Hα ) declines twice as much as log(Σ1kpc,Cont) from z ∼ 1 to 0.5 (at a fixed stellar mass of log(M */M ⊙) = 9.5). By comparing our results to the TNG50 cosmological magneto-hydrodynamical simulation, we rule out dust as the driver of this evolution. Our results are consistent with inside-out quenching following in the wake of inside-out growth, the former of which drives the significant drop in Σ1kpc,Hα from z ∼ 1 to z ∼ 0.5.
• Papovich, C., Simons, R. C., Estrada-Carpenter, V., Matharu, J., Momcheva, I., Trump, J. R., Backhaus, B. E., Brammer, G., Cleri, N. J., Finkelstein, S. L., Giavalisco, M., Ji, Z., Jung, I., Kewley, L. J., Nicholls, D. C., Pirzkal, N., Rafelski, M., & Weiner, B. (2022). CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3. \apj, 937(1), 22.
• Wang, W., Kassin, S. A., Faber, S., Koo, D. C., Cunningham, E. C., Yesuf, H. M., Barro, G., Guhathakurta, P., Weiner, B. J., Vega, A., Guo, Y., Heckman, T. M., Pacifici, C., Wang, B., & Welker, C. (2022). The Baltimore Oriole's Nest: Cool Winds from the Inner and Outer Parts of a Star-forming Galaxy at z = 1.3. \apj, 930(2), 146.
• Wu, J. F., Peek, J., Tollerud, E. J., Mao, Y., Nadler, E. O., Geha, M., Wechsler, R. H., Kallivayalil, N., & Weiner, B. J. (2022). Extending the SAGA Survey (xSAGA). I. Satellite Radial Profiles as a Function of Host-galaxy Properties. \apj, 927(1), 121.
• Alberts, S., Lee, K., Pope, A., Brodwin, M., Chiang, Y., McKinney, J., Xue, R., Huang, Y., Brown, M., Dey, A., Eisenhardt, P. R., Jannuzi, B. T., Popescu, R., Ramakrishnan, V., Stanford, S. A., & Weiner, B. J. (2021). Measuring the total infrared light from galaxy clusters at z = 0.5-1.6: connecting stellar populations to dusty star formation. \mnras, 501(2), 1970-1998.
• Aragón-Salamanca, A., Brammer, G. G., Cooper, J. R., Desai, V., Desjardins, T., De Lucia, G., Finn, R. A., Jablonka, P., Jaffé, Y. L., Mann, J. L., Moustakas, J., Rudnick, G. H., Spérone-Longin, D., Teplitz, H. I., Vulcani, B., Weiner, B. J., & Zaritsky, D. (2021). H α-based star formation rates in and around z ∼ 0.5 EDisCS clusters. Monthly Notices of the Royal Astronomical Society, 509(4), 5382-5398. doi:10.1093/mnras/stab3184
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  We investigate the role of environment on star-formation rates of galaxies at various cosmic densities in well-studied clusters. We present the star-forming main sequence for 163 galaxies in four EDisCS clusters in the range 0.4 $ $ 10$^{9.75}$M\textsubscript{\(\odot\)} show little dependence on environment. At face value, the similarities in the star-formation rate distributions in the three environments may indicate that the process of finally shutting down star formation is rapid, however, the depth of our data and size of our sample make it difficult to conclusively test this scenario. Despite having significant H$\alpha$ emission, 21 galaxies are classified as {\em UVJ}-quiescent and may represent a demonstration of the quenching of star formation caught in the act.
• Mao, Y., Geha, M., Wechsler, R. H., Weiner, B., Tollerud, E. J., Nadler, E. O., & Kallivayalil, N. (2021). The SAGA Survey. II. Building a Statistical Sample of Satellite Systems around Milky Way-like Galaxies. \apj, 907(2), 85.
• Paterson, K., Lundquist, M., Rastinejad, J., Fong, W., Sand, D., Andrews, J., Amaro, R., Eskandari, O., Wyatt, S., Daly, P., Bradley, H., Zhou-Wright, S. .., Valenti, S., Yang, S., Christensen, E., Gibbs, A., Shelly, F., Bilinski, C., Chomiuk, L., , Corsi, A., et al. (2021). Searches after Gravitational Waves Using ARizona Observatories (SAGUARO): Observations and Analysis from Advanced LIGO/Virgo's Third Observing Run. \apj, 912(2), 128.
• Simons, R. C., Papovich, C., Momcheva, I., Trump, J. R., Brammer, G., Estrada-Carpenter, V., Backhaus, B. E., Cleri, N. J., Finkelstein, S. L., Giavalisco, M., Ji, Z., Jung, I., Matharu, J., & Weiner, B. (2021). CLEAR: The Gas-phase Metallicity Gradients of Star-forming Galaxies at 0.6 < z < 2.6. \apj, 923(2), 203.
• Williams, C. C., Spilker, J. S., Whitaker, K. E., Dav{\'e}, R., Woodrum, C., Brammer, G., Bezanson, R., Narayanan, D., & Weiner, B. (2021). ALMA Measures Rapidly Depleted Molecular Gas Reservoirs in Massive Quiescent Galaxies at z \ensuremath{\sim} 1.5. \apj, 908(1), 54.
• Alberts, S., Brodwin, M., Brown, M., Chiang, Y., Dey, A., Eisenhardt, P. R., Huang, Y., Jannuzi, B. T., Lee, K., McKinney, J., Pope, A., Popescu, R., Ramakrishnan, V., Stanford, S. A., Weiner, B. J., & Xue, R. (2020). Measuring the total infrared light from galaxy clusters at z = 0.5–1.6: connecting stellar populations to dusty star formation. Monthly Notices of the Royal Astronomical Society, 501(2), 1970-1998. doi:10.1093/mnras/staa3357
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  ABSTRACT Massive galaxy clusters undergo strong evolution from z ∼ 1.6 to z ∼ 0.5, with overdense environments at high-z characterized by abundant dust-obscured star formation and stellar mass growth which rapidly give way to widespread quenching. Data spanning the near- to far-infrared (IR) can directly trace this transformation; however, such studies have largely been limited to the massive galaxy end of cluster populations. In this work, we present ‘total light’ stacking techniques spanning $3.4\!-\!500\, \mu$m aimed at revealing the total cluster emission, including low-mass members and potential intracluster dust. We detail our procedures for WISE, Spitzer, and Herschel imaging, including corrections to recover the total stacked emission in the case of high fractions of detected galaxies. We apply our techniques to 232 well-studied log$\, M_{200}/\mathrm{M}_{\odot }\sim 13.8$ clusters in multiple redshift bins, recovering extended cluster emission at all wavelengths. We measure the averaged IR radial profiles and spectral energy distributions (SEDs), quantifying the total stellar and dust content. The near-IR profiles are well described by an NFW model with a high (c ∼ 7) concentration. Dust emission is similarly concentrated, albeit suppressed at $r\lesssim 0.3\,$Mpc. The measured SEDs lack warm dust, consistent with the colder SEDs of low-mass galaxies. We derive total stellar masses consistent with the theoretical Mhalo−M⋆ relation and specific star formation rates that evolve strongly with redshift, echoing that of log$\, M_{\star }/\mathrm{M}_{\odot }\gtrsim 10$ cluster galaxies. Separating out the massive population reveals the majority of cluster far-IR emission ($\sim 70\!-\!80{{\ \rm per\ cent}}$) is provided by the low-mass constituents, which differs from field galaxies. This effect may be a combination of mass-dependent quenching and excess dust in low-mass cluster galaxies.
• Chen, H. W., Zahedy, F. S., Boettcher, E., Cooper, T. M., Johnson, S. D., Rudie, G. C., Chen, M. C., Walth, G. L., Cantalupo, S., Cooksey, K. L., Faucher-Giguère, C. A., Greene, J. E., Lopez, S., Mulchaey, J. S., Penton, S. V., Petitjean, P., Putman, M. E., Rafelski, M., Rauch, M., , Schaye, J., et al. (2020). The cosmic ultraviolet baryon survey (CUBS) - I. overview and the diverse environments of lyman limit systems at z < 1. Monthly Notices of the Royal Astronomical Society, 497(Issue 1). doi:10.1093/mnras/staa1773
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  We present initial results from the Cosmic Ultraviolet Baryon Survey (CUBS). CUBS is designed to map diffuse baryonic structures at redshift z ≲ 1 using absorption-line spectroscopy of 15 UV-bright QSOs with matching deep galaxy survey data. CUBS QSOs are selected based on their NUV brightness to avoid biases against the presence of intervening Lyman limit systems (LLSs) at zabs < 1. We report five new LLSs of log N(H I)/cm−2 ≳ 17.2 over a total redshift survey path-length of ΔzLL = 9.3, and a number density of n(z) = 0.43+−002618. Considering all absorbers with log N(H I)/cm−2 > 16.5 leads to n(z) = 1.08+−003125 at zabs < 1. All LLSs exhibit a multicomponent structure and associated metal transitions from multiple ionization states such as C II, C III, Mg II, Si II, Si III, and O VI absorption. Differential chemical enrichment levels as well as ionization states are directly observed across individual components in three LLSs. We present deep galaxy survey data obtained using the VLT-MUSE integral field spectrograph and the Magellan Telescopes, reaching sensitivities necessary for detecting galaxies fainter than 0.1 L∗ at d ≲ 300 physical kpc (pkpc) in all five fields. A diverse range of galaxy properties is seen around these LLSs, from a low-mass dwarf galaxy pair, a co-rotating gaseous halo/disc, a star-forming galaxy, a massive quiescent galaxy, to a galaxy group. The closest galaxies have projected distances ranging from d = 15 to 72 pkpc and intrinsic luminosities from ≈0.01 L∗ to ≈3 L∗. Our study shows that LLSs originate in a variety of galaxy environments and trace gaseous structures with a broad range of metallicities.
• Chen, H., Zahedy, F. S., Boettcher, E., Cooper, T. M., Johnson, S. D., Rudie, G. C., Chen, M. C., Walth, G. L., Cantalupo, S., Cooksey, K. L., Faucher-Gigu{\`ere}, C., Greene, J. E., Lopez, S., Mulchaey, J. S., Penton, S. V., Petitjean, P., Putman, M. E., Rafelski, M., Rauch, M., , Schaye, J., et al. (2020). The Cosmic Ultraviolet Baryon Survey (CUBS) - I. Overview and the diverse environments of Lyman limit systems at z < 1. \mnras, 497(1), 498-520.
• Estrada-Carpenter, V., Papovich, C., Momcheva, I., Brammer, G., Simons, R., Bridge, J., Cleri, N. J., Ferguson, H., Finkelstein, S. L., Giavalisco, M., Jung, I., Matharu, J., Trump, J. R., & Weiner, B. (2020). CLEAR. II. Evidence for Early Formation of the Most Compact Quiescent Galaxies at High Redshift. \apj, 898(2), 171.
• Krantz, H., Pearce, E. C., & Weiner, B. J. (2020). Examining the effects of on-orbit aging of SL-12 rocket bodies using visible band spectra with the MMT telescope. Journal of Space Safety Engineering, 7(3), 376-380. doi:10.1016/j.jsse.2020.07.017
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  Abstract The characterization of deep space debris has posed a significant challenge in the study of space objects. To be most effective, characterization must be performed quickly and under non-ideal operational conditions, generally using non-resolved techniques. Multi-color photometry and the resultant color indices offer the potential to rapidly discriminate between debris and intact space objects such as rocket bodies and satellites. However, these studies are not well informed by high resolution spectra of these same objects, due to the lack of prior measurements with large astronomical telescopes. We present a spectroscopic study of orbital debris aimed at characterizing changes over time in object properties, using ground-based spectroscopy of several similar rocket bodies in geosynchronous orbit, launched at different times. High and moderate resolution spectroscopy is not routinely collected by SSA resources. Nonetheless, several researchers have collected satellite spectra for research purposes. Several researchers have also noted the progressive reddening of spacecraft surfaces. In this study, we have collected high resolution spectra of five Russian SL-12 rocket bodies in geosynchronous orbit. The spectra were collected with the Blue Channel Spectrograph on the 6.5 m MMT telescope at Mt. Hopkins. The measurements were taken using the 300-line grating, which is blazed for the red, and can cover a 520 nm range at dispersion 0.196 nm/pixel. The large collecting aperture of the MMT allowed the rapid collection of multiple high signal-to-noise spectra with only 2 minutes per exposure. This short exposure allowed us to have confidence the solar phase angle was near constant during each collection, but that the spectra were averaged over the rotation of the rocket body. These spectra allow analysis of both the variation in albedo over a large wavelength range, and searches for discrete absorption features. The SL-12 (also called the "Proton K") was a mainstay Russian four-stage to GEO launch vehicle that was used from 1974 to 2012. The SL-12 fourth stage rocket bodies (henceforth referred to as "SL-12 RB") offer a convenient ensemble of objects for which photometric techniques can be developed and tested. For this study, spectra of five SL-12s with a range of years-on-orbit (YOO) ranging from 23-35 years were collected, allowing a comparative study of the evolution of the spectra over a 12-year difference in age. Additionally, all these objects have been previously observed in the near-IR with the UKIRT WFCAM. The spectra are analyzed for evidence of the effects of on-orbit reddening and other changes over time.
• Weiner, B., Pearce, E., Krantz, H., Block, A., Howie, R., Kattner, S., Self, S., & Williams, G. (2020). MMT/Binospec spectroscopy of near earth object 2020 SO distinguishes it from common natural asteroids. The Astronomer's Telegram, 14241, 1.
• Aldcroft, T. L., Allen, A., Bellm, E. C., Berriman, B., Brownstein, J. R., Buzasi, D., Chan, C., Cherinka, B., Connolly, A. J., Cruz, K. L., Desai, V., Dong, C., Economou, F., Faherty, J. K., Foschini, L., Ginsburg, A., Golkhou, V. Z., Gradvohl, A. L., Harrington, J., , Hummels, C., et al. (2019). Elevating the Role of Software as a Product of the Research Enterprise. Bulletin of the American Astronomical Society, 51(7).
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  Software is a critical part of modern research, and those responsible for its development must be retained in the workforce to maximize the scientific return from petabyte-scale datasets. This white paper will present current challenges and suggest practical solutions for elevating the role of software as a product of the research enterprise.
• Bezanson, R., Spilker, J., Williams, C. C., Whitaker, K. E., Narayanan, D., Weiner, B., & Franx, M. (2019). Extremely Low Molecular Gas Content in a Compact, Quiescent Galaxy at z=1.522.
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  One of the greatest challenges to theoretical models of massive galaxyformation is the regulation of star formation at early times. The relativeroles of molecular gas expulsion, depletion, and stabilization are uncertain asdirect observational constraints of the gas reservoirs in quenched or quenchinggalaxies at high redshift are scant. We present ALMA observations of CO(2-1) ina massive ($\log M_{\star}/M_{\odot}=11.2$), recently quenched galaxy at$z=1.522$. The optical spectrum of this object shows strong Balmer absorptionlines, which implies that star formation ceased $\sim$0.8 Gyr ago. We do notdetect CO(2-1) line emission, placing an upper limit on the molecular$\mathrm{H_2}$ gas mass of 1.1$\times10^{10}\,M_{\odot}$. The implied gasfraction is $f_{\rm{H_2}}{\equiv M_{H_2}/M_{\star}}1$ passivegalaxy to date. Our observations show that the depletion of $\mathrm{H_2}$ fromthe interstellar medium of quenched objects can be both efficient and fairlycomplete, in contrast to recent claims of significant cold gas in recentlyquenched galaxies. We explore the variation in observed gas fractions inhigh-$z$ galaxies and show that galaxies with high stellar surface density havelow $f_{\rm{H_2}}$, similar to recent correlations between specific starformation rate and stellar surface density.[Journal_ref: ]
• Bezanson, R., Spilker, J., Williams, C. C., Whitaker, K. E., Narayanan, D., Weiner, B., & Franx, M. (2019). Extremely Low Molecular Gas Content in a Compact, Quiescent Galaxy at z = 1.522. \apjl, 873(2), L19.
• Chan, C., Pickering, T., Juneau, S., Malz, A. I., Pope, B., Aldcroft, T. L., Allen, A., Alpaslan, M., Anderson, L., Barentsen, G., Bektesevic, D., Benavides, J., Berriman, B., Blanton, M. R., Bosch, J., Bouquin, D., Bradley, L., Bryan, G. L., Burke, D., , Burns, K. J., et al. (2019). Sustaining Community-Driven Software for Astronomy in the 2020s. Bulletin of the American Astronomical Society, 51(7).
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  Software is critical to astronomical research. Sharing and sustaining astronomical software has long-term impacts on scientific outcomes. However, support for this has been uneven, creating significant risks. Thus, we highlight changes that will enable a sustainable software sharing system for astronomy and astrophysics in the next decade.
• Estrada-Carpenter, V., Papovich, C., Momcheva, I., Brammer, G., Long, J., Quadri, R. F., Bridge, J., Dickinson, M., Ferguson, H., Finkelstein, S., Giavalisco, M., Gosmeyer, C. M., Lotz, J., Salmon, B., Skelton, R. E., Trump, J. R., & Weiner, B. (2019). CLEAR. I. Ages and Metallicities of Quiescent Galaxies at 1.0 \< z \< 1.8 Derived from Deep Hubble Space Telescope Grism Data. \apj, 870(2), 133.
• Freundlich, J., Combes, F., Tacconi, L., Genzel, R., Garcia-Burillo, S. .., Neri, R., Contini, T., Bolatto, A., Lilly, S., Salom{\'e}, P., Bicalho, I., Boissier, J., Boone, F., Bouch{\'e}, N., Bournaud, F., Burkert, A., Carollo, M., Cooper, M., Cox, P., , Feruglio, C., et al. (2019). PHIBSS2: survey design and z = 0.5 - 0.8 results. Molecular gas reservoirs during the winding-down of star formation. \aap, 622, A105.
• Lundquist, M., Paterson, K., Fong, W., Sand, D., Andrews, J., Shivaei, I., Daly, P., Valenti, S., Yang, S., Christensen, E., Gibbs, A., Shelly, F., Wyatt, S., Eskandari, O., Kuhn, O., Amaro, R., Arcavi, I., Behroozi, P., Butler, N., , Chomiuk, L., et al. (2019). Searches after Gravitational Waves Using ARizona Observatories (SAGUARO): System Overview and First Results from Advanced LIGO/Virgo\textquoterights Third Observing Run. \apjl, 881(2), L26.
• Pickering, T., Chan, C., Bauer, A. E., Bauer, A., Bellm, E. C., Bianco, F. B., Cherinka, B., Cruz, K. L., Desai, V., Dong, C., Economou, F., Harrington, J., Kartaltepe, J. S., Kerzendorf, W., Laginja, I., Li, T., Lundgren, B., Modjaz, M., Narayan, G., , Nord, B., et al. (2019). The Growing Importance of a Tech Savvy Astronomy and Astrophysics Workforce. Bulletin of the American Astronomical Society, 51(7).
• Spilker, J. S., Bezanson, R., Weiner, B. J., Whitaker, K. E., & Williams, C. C. (2019). Evidence for Inside-out Galaxy Growth and Quenching of a z ̃ 2 Compact Galaxy From High-resolution Molecular Gas Imaging. \apj, 883(1), 81.
• Walth, G. L., Egami, E., Cl{\'ement}, B., Rawle, T. D., Rex, M., Richard, J., P{\'erez-Gonz\'alez}, P., Boone, F., Dessauges-Zavadsky, M., Portouw, J., Weiner, B., McGreer, I., & Schneider, E. (2019). Infrared Galaxies in the Field of the Massive Cluster Abell S1063: Discovery of a Luminous Kiloparsec-sized H II Region in a Gravitationally Lensed Infrared-luminous Galaxy at z = 0.6. \apj, 877(1), 7.
• Williams, C. C., Labbe, I., Spilker, J., Stefanon, M., Leja, J., Whitaker, K., Bezanson, R., Narayanan, D., Oesch, P., & Weiner, B. (2019). Discovery of a Dark, Massive, ALMA-only Galaxy at z ̃ 5-6 in a Tiny 3 mm Survey. \apj, 884(2), 154.
• Zahedy}, F. S., Chen, H., Johnson, S. D., Pierce, R. M., Rauch, M., Huang, Y., Weiner, B. J., & Gauthier, J. (2019). Characterizing circumgalactic gas around massive ellipticals at z \ensuremath{\sim} 0.4 - II. Physical properties and elemental abundances. \mnras, 484(2), 2257-2280.
• Zhou, R., Cooper, M. C., Newman, J. A., Ashby, M. L., Aird, J., Conselice, C. J., Davis, M., Dutton, A. A., Faber, S., Fang, J. J., Fazio, G., Guhathakurta, P., Kocevski, D., Koo, D. C., {Nand, r. K., Phillips, A. C., Rosario, D. J., Schlafly, E. F., Trump, J. R., , Weiner, B., et al. (2019). Deep ugrizY imaging and DEEP2/3 spectroscopy: a photometric redshift testbed for LSST and public release of data from the DEEP3 Galaxy Redshift Survey. \mnras, 488(4), 4565-4584.
• Ashcraft, T. A., Windhorst, R. A., Jansen, R. A., Cohen, S. H., Grazian, A., Paris, D., Fontana, A., Giallongo, E., Speziali, R., Testa, V., Boutsia, K., O'Connell, R. W., Rutkowski, M. J., Ryan, R. E., Scarlata, C., & Weiner, B. (2018). Ultra-deep Large Binocular Camera U-band Imaging of the GOODS-North Field: Depth Versus Resolution. Publications of the Astronomical Society of the Pacific, 130(988), 064102.
• Bera, A., Kanekar, N., Weiner, B. J., Sethi, S., & Dwarakanath, K. (2018). Probing Star Formation in Galaxies at z \ensuremath{\approx} 1 via a Giant Metrewave Radio Telescope Stacking Analysis. \apj, 865(1), 39.
• Blanchard, P., Gomez, S., Berger, E., Nicholl, M., Kattner, S., & Weiner, B. (2018). Classification of AT2018bym as a Type I Superluminous Supernova. The Astronomer's Telegram, 11714, 1.
• Chen, H., Zahedy, F. S., Johnson, S. D., Pierce, R. M., Huang, Y., Weiner, B. J., & Gauthier, J. (2018). Characterizing circumgalactic gas around massive ellipticals at z ̃ 0.4 - I. Initial results. \mnras, 479(2), 2547-2563.
• Fang, J. J., Faber, S., Koo, D. C., Rodr{\'\iguez-Puebla}, A., Guo, Y., Barro, G., Behroozi, P., Brammer, G., Chen, Z., Dekel, A., Ferguson, H. C., Gawiser, E., Giavalisco, M., Kartaltepe, J., Kocevski, D. D., Koekemoer, A. M., McGrath, E. J., McIntosh, D., Newman, J. A., , Pacifici, C., et al. (2018). Demographics of Star-forming Galaxies since z ̃ 2.5. I. The UVJ Diagram in CANDELS. \apj, 858(2), 100.
• Kelly, P. L., Diego, J. M., Rodney, S., Kaiser, N., Broadhurst, T., Zitrin, A., Treu, T., P{\'erez-Gonz\'alez}, P. G., Morishita, T., Jauzac, M., Selsing, J., Oguri, M., Pueyo, L., Ross, T. W., Filippenko, A. V., Smith, N., Hjorth, J., Cenko, S. B., Wang, X., , Howell, D. A., et al. (2018). Extreme magnification of an individual star at redshift 1.5 by a galaxy-cluster lens. Nature Astronomy, 2, 334-342.
• Rodney, S., Balestra, I., Bradac, M., Brammer, G., Broadhurst, T., Caminha, G., Chiriv{\i}, G., Diego, J., Filippenko, A., Foley, R., Graur, O., Grillo, C., Hemmati, S., Hjorth, J., Hoag, A., Jauzac, M., Jha, S., Kawamata, R., Kelly, P., , McCully, C., et al. (2018). Two peculiar fast transients in a strongly lensed host galaxy. Nature Astronomy, 2, 324-333.
• Spilker, J., Bezanson, R., Bari{\v{s}i\'c}, I., Bell, E., Lagos, C., Maseda, M., Muzzin, A., Pacifici, C., Sobral, D., Straatman, C., Wel, A., Dokkum, P., Weiner, B., Whitaker, K., Williams, C. C., & Wu, P. (2018). Molecular Gas Contents and Scaling Relations for Massive, Passive Galaxies at Intermediate Redshifts from the LEGA-C Survey. \apj, 860(2), 103.
• Tacconi, L., Genzel, R., Saintonge, A., Combes, F., Garc{\'\ia-Burillo}, S., Neri, R., Bolatto, A., Contini, T., F{\"orster, S. N., Lilly, S., Lutz, D., Wuyts, S., Accurso, G., Boissier, J., Boone, F., Bouch{\'e}, N., Bournaud, F., Burkert, A., Carollo, M., , Cooper, M., et al. (2018). PHIBSS: Unified Scaling Relations of Gas Depletion Time and Molecular Gas Fractions. \apj, 853(2), 179.
• Zahedy, F. S., Chen, H. W., Johnson, S. D., Pierce, R. M., Rauch, M., Huang, Y. H., Weiner, B. J., & Gauthier, J. R. (2018). Characterizing circumgalactic gas around massive ellipticals atz∼ 0.4 – II. Physical properties and elemental abundances. Monthly Notices of the Royal Astronomical Society, 484(2), 2257-2280. doi:10.1093/mnras/sty3482
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  We present a systematic investigation of the circumgalactic medium (CGM) within projected distances d1e11 M_sun. Combining far-ultraviolet Cosmic Origin Spectrograph spectra from the Hubble Space Telescope and optical echelle spectra from the ground enables a detailed ionization analysis based on resolved component structures of a suite of absorption transitions, including the full HI Lyman series and various ionic metal transitions. By comparing the relative abundances of different ions in individually-matched components, we show that cool gas (T~1e4 K) density and metallicity can vary by more than a factor of ten in in an LRG halo. Specifically, metal-poor absorbing components with
• Carleton, T., Cooper, M., Bolatto, A., Bournaud, F., Combes, F., Freundlich, J., Garcia-Burillo, S. .., Genzel, R., Neri, R., Tacconi, L., Sandstrom, K., Weiner, B., & Weiss, A. (2017). PHIBSS: exploring the dependence of the CO-H$_2$ conversion factor on total mass surface density at z$\lt$1.5. \mnras, 467, 4886-4901.
• Geha, M., Wechsler, R., Mao, Y., Tollerud, E., Weiner, B., Bernstein, R., Hoyle, B., Marchi, S., Marshall, P., Mu{\~noz}, R., & Lu, Y. (2017). The SAGA Survey. I. Satellite Galaxy Populations around Eight Milky Way Analogs. \apj, 847, 4.
• Grazian, A., Giallongo, E., Paris, D., Boutsia, K., Dickinson, M., Santini, P., Windhorst, R., Jansen, R., Cohen, S., Ashcraft, T., Scarlata, C., Rutkowski, M., Vanzella, E., Cusano, F., Cristiani, S., Giavalisco, M., Ferguson, H., Koekemoer, A., Grogin, N., , Castellano, M., et al. (2017). Lyman continuum escape fraction of faint galaxies at z 3.3 in the CANDELS/GOODS-North, EGS, and COSMOS fields with LBC. \aap, 602, A18.
• Murphy, E., Momjian, E., Condon, J., Chary, R., Dickinson, M., Inami, H., Taylor, A., & Weiner, B. (2017). The GOODS-N Jansky VLA 10 GHz Pilot Survey: Sizes of Star-forming $\mu$JY Radio Sources. \apj, 839, 35.
• Simons, R., Kassin, S., Weiner, B., Faber, S., Trump, J., Heckman, T., Koo, D., Pacifici, C., Primack, J., Snyder, G., & Vega, A. (2017). z \tilde 2: An Epoch of Disk Assembly. \apj, 843, 46.
• Tinker, J., Brownstein, J., Guo, H., Leauthaud, A., Maraston, C., Masters, K., Montero-Dorta, A., Thomas, D., Tojeiro, R., Weiner, B., Zehavi, I., & Olmstead, M. (2017). The Correlation between Halo Mass and Stellar Mass for the Most Massive Galaxies in the Universe. \apj, 839, 121.
• Bezanson, R., Brammer, G. B., Dokkum, P. G., Franx, M., Labbe, I., Leja, J., Momcheva, I. G., Nelson, E. J., Quadri, R. F., Skelton, R. E., Wake, D. A., Weiner, B. J., & Whitaker, K. E. (2016). Leveraging 3D-HST Grism Redshifts to Quantify Photometric Redshift Performance. The Astrophysical Journal, 822(1), 30. doi:10.3847/0004-637x/822/1/30
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  NASA through Hubble Fellowship - Space Telescope Science Institute [HF-51318, HF2-51368]; NASA [NAS5-26555]; 3D-HST Treasury Program [GO 12177, 12328]
• Bezanson, R., Wake, D. A., Brammer, G. B., van, D., Franx, M., Labbe, I., Leja, J., Momcheva, I. G., Nelson, E. J., Quadri, R. F., Skelton, R. E., Weiner, B. J., & Whitaker, K. E. (2016). LEVERAGING 3D-HST GRISM REDSHIFTS TO QUANTIFY PHOTOMETRIC REDSHIFT PERFORMANCE. ASTROPHYSICAL JOURNAL, 822(1).
• Huang, Y., Chen, H., Johnson, S. D., & Weiner, B. J. (2016). Characterizing the chemically enriched circumgalactic medium of similar to 38 000 luminous red galaxies in SDSS DR12. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 455(2), 1713-1727.
• Kelly, P. L., Brammer, G., Selsing, J., Foley, R. J., Hjorth, J., Rodney, S. A., Christensen, L., Strolger, L. G., Filippenko, A. V., Treu, T., Steidel, C. C., Strom, A., Riess, A. G., Zitrin, A., Schmidt, K. B., Bradač, M., Jha, S. W., Graham, M. L., McCully, C., , Graur, O., et al. (2016). SN REFSDAL: CLASSIFICATION AS A LUMINOUS AND BLUE SN 1987A-LIKE TYPE II SUPERNOVA. The Astrophysical Journal, 831(2), 205-205. doi:10.3847/0004-637x/831/2/205
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  We have acquired Hubble Space Telescope (HST) and Very Large Telescope near-infrared spectra and images of supernova (SN) Refsdal after its discovery as an Einstein cross in fall 2014. The HST light curve of SN Refsdal has a shape consistent with the distinctive, slowly rising light curves of SN 1987A-like SNe, and we find strong evidence for a broad Hα P-Cygni profile and Na I D absorption in the HST grism spectrum at the redshift (z = 1.49) of the spiral host galaxy. SNe IIn, largely powered by circumstellar interaction, could provide a good match to the light curve of SN Refsdal, but the spectrum of a SN IIn would not show broad and strong Hα and Na I D absorption. From the grism spectrum, we measure an Hα expansion velocity consistent with those of SN 1987A-like SNe at a similar phase. The luminosity, evolution, and Gaussian profile of the Hα emission of the WFC3 and X-shooter spectra, separated by ~2.5 months in the rest frame, provide additional evidence that supports the SN 1987A-like classification. In comparison with other examples of SN 1987A-like SNe, photometry of SN Refsdal favors bluer B − V and V − R colors and one of the largest luminosities for the assumed range of potential magnifications. The evolution of the light curve at late times will provide additional evidence about the potential existence of any substantial circumstellar material. Using MOSFIRE and X-shooter spectra, we estimate a subsolar host-galaxy metallicity (8.3 ± 0.1 dex and
• Kelly, P. L., Rodney, S. A., Treu, T., Strolger, L. G., Foley, R. J., Jha, S. W., Selsing, J., Brammer, G., Bradač, M., Cenko, S. B., Graur, O., Filippenko, A. V., Hjorth, J., McCully, C., Molino, A., Nonino, M., Riess, A. G., Schmidt, K. B., Tucker, B., , Von Der Linden, A., et al. (2016). DEJA VU ALL OVER AGAIN: THE REAPPEARANCE OF SUPERNOVA REFSDAL. The Astrophysical Journal, 819(1), L8. doi:10.3847/2041-8205/819/1/l8
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  In Hubble Space Telescope (HST) imaging taken on 2014 November 10, four images of supernova (SN) "Refsdal" (redshift z = 1.49) appeared in an Einstein-cross-like configuration (images S1–S4) around an early-type galaxy in the cluster MACS J1149.5+2223 (z = 0.54). Almost all lens models of the cluster have predicted that the SN should reappear within a year in a second host-galaxy image created by the cluster's potential. In HST observations taken on 2015 December 11, we find a new source at the predicted position of the new image of SN Refsdal approximately $8^{\prime\prime} $ from the previous images S1–S4. This marks the first time the appearance of a SN at a particular time and location in the sky was successfully predicted in advance! We use these data and the light curve from the first four observed images of SN Refsdal to place constraints on the relative time delay and magnification of the new image (SX) compared to images S1–S4. This enables us, for the first time, to test "blind" lens model predictions of both magnifications and time delays for a lensed SN. We find that the timing and brightness of the new image are consistent with the blind predictions of a fraction of the models. The reappearance illustrates the discriminatory power of this blind test and its utility to uncover sources of systematic uncertainty. From planned HST photometry, we expect to reach a precision of 1%–2% on the time delay between S1–S4 and SX.
• Montero-Dorta, A. D., Shu, Y., Bolton, A. S., Brownstein, J. R., & Weiner, B. J. (2016). A steep slope and small scatter for the high-mass end of the L-sigma relation at z similar to 0.55. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 456(3), 3265-3281.
• Pacifici, C., Kassin, S. A., Weiner, B. J., Holden, B., Gardner, J. P., Faber, S. M., Ferguson, H. C., Koo, D. C., Primack, J. R., Bell, E. F., Dekel, A., Gawiser, E., Giavalisco, M., Rafelski, M., Simons, R. C., Barro, G., Croton, D. J., Dave, R., Fontana, A., , Grogin, N. A., et al. (2016). THE EVOLUTION OF STAR FORMATION HISTORIES OF QUIESCENT GALAXIES. ASTROPHYSICAL JOURNAL, 832(1).
• Rodney, S. A., Strolger, L. G., Kelly, P. L., Bradač, M., Brammer, G., Filippenko, A. V., Foley, R. J., Graur, O., Hjorth, J., Jha, S. W., McCully, C., Molino, A., Riess, A. G., Schmidt, K. B., Selsing, J., Sharon, K., Treu, T., Weiner, B. J., & Zitrin, A. (2016). SN REFSDAL: PHOTOMETRY AND TIME DELAY MEASUREMENTS OF THE FIRST EINSTEIN CROSS SUPERNOVA. The Astrophysical Journal, 820(1), 50. doi:10.3847/0004-637x/820/1/50
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  We present the first year of Hubble Space Telescope imaging of the unique supernova (SN) "Refsdal," a gravitationally lensed SN at z = 1.488 ± 0.001 with multiple images behind the galaxy cluster MACS J1149.6+2223. The first four observed images of SN Refsdal (images S1–S4) exhibited a slow rise (over ~150 days) to reach a broad peak brightness around 2015 April 20. Using a set of light curve templates constructed from SN 1987A-like peculiar Type II SNe, we measure time delays for the four images relative to S1 of 4 ± 4 (for S2), 2 ± 5 (S3), and 24 ± 7 days (S4). The measured magnification ratios relative to S1 are 1.15 ± 0.05 (S2), 1.01 ± 0.04 (S3), and 0.34 ± 0.02 (S4). None of the template light curves fully captures the photometric behavior of SN Refsdal, so we also derive complementary measurements for these parameters using polynomials to represent the intrinsic light curve shape. These more flexible fits deliver fully consistent time delays of 7 ± 2 (S2), 0.6 ± 3 (S3), and 27 ± 8 days (S4). The lensing magnification ratios are similarly consistent, measured as 1.17 ± 0.02 (S2), 1.00 ± 0.01 (S3), and 0.38 ± 0.02 (S4). We compare these measurements against published predictions from lens models, and find that the majority of model predictions are in very good agreement with our measurements. Finally, we discuss avenues for future improvement of time delay measurements—both for SN Refsdal and for other strongly lensed SNe yet to come.
• Rujopakarn, W., Dunlop, J. S., Rieke, G. H., Ivison, R. J., Cibinel, A., Nyland, K., Jagannathan, P., Silverman, J. D., Alexander, D. M., Biggs, A. D., Bhatnagar, S., Ballantyne, D. R., Dickinson, M., Elbaz, D., Geach, J. E., Hayward, C. C., Kirkpatrick, A., McLure, R. J., Michałowski, M. J., , Miller, N. A., et al. (2016). VLA AND ALMA IMAGING OF INTENSE GALAXY-WIDE STAR FORMATION IN z ∼ 2 GALAXIES. The Astrophysical Journal, 833(1), 12. doi:10.3847/0004-637x/833/1/12
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  World Premier International Research Center Initiative (WPI), MEXT, Japan; JSPS KAKENHI [JP15K17604]; Chulalongkorn University's Ratchadapiseksompot Endowment Fund; CUniverse (CUAASC); EC FP7 SPACE project ASTRODEEP [312725]; European Research Council [COSMICISM 321302]; ERC; YCAA Prize Postdoctoral Fellowship; NSF [AST-1442650]; NASA [HST AR-13906.001, NAS5-26555]; Cottrell College Science Award; [VLA/14A-360]
• Simons, R. C., Kassin, S. A., Trump, J. R., Weiner, B. J., Heckman, T. M., Barro, G., Koo, D. C., Guo, Y., Pacifici, C., Koekemoer, A., & Stephens, A. W. (2016). KINEMATIC DOWNSIZING at z ∼ 2. Astrophysical Journal, 830(Issue 1). doi:10.3847/0004-637x/830/1/14
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  We present results from a survey of the internal kinematics of 49 star-forming galaxies at z∼2 in the CANDELS fields with the Keck/MOSFIRE spectrograph, Survey in the near-Infrared of Galaxies with Multiple position Angles (SIGMA). Kinematics (rotation velocity Vrot and gas velocity dispersion sg) are measured from nebular emission lines which trace the hot ionized gas surrounding star-forming regions. We find that by z∼2, massive star-forming galaxies (log M∗ Mo ≳ 10.2) have assembled primitive disks: their kinematics are dominated by rotation, they are consistent with a marginally stable disk model, and they form a Tully-Fisher relation. These massive galaxies have values of Vrot δg that are factors of 2-5 lower than local well-ordered galaxies at similar masses. Such results are consistent with findings by other studies. We find that low-mass galaxies (log M∗ Mo ≳10.2) at this epoch are still in the early stages of disk assembly: their kinematics are often dominated by gas velocity dispersion and they fall from the Tully-Fisher relation to significantly low values of Vrot. This kinematic downsizing implies that the process(es) responsible for disrupting disks at z∼2 have a stronger effect and/or are more active in low-mass systems. In conclusion, we find that the period of rapid stellar mass growth at z∼2 is coincident with the nascent assembly of low-mass disks and the assembly and settling of high-mass disks.
• Spilker, J. S., Bezanson, R., Marrone, D. P., Weiner, B. J., Whitaker, K. E., & Williams, C. C. (2016). LOW GAS FRACTIONS CONNECT COMPACT STAR-FORMING GALAXIES TO THEIR z similar to 2 QUIESCENT DESCENDANTS. ASTROPHYSICAL JOURNAL, 832(1).
• {Kelly}, P., {Brammer}, G., {Selsing}, J., {Foley}, R., {Hjorth}, J., {Rodney}, S., {Christensen}, L., {Strolger}, L., {Filippenko}, A., {Treu}, T., {Steidel}, C., {Strom}, A., {Riess}, A., {Zitrin}, A., {Schmidt}, K., {Brada{\v c}}, M., {Jha}, S., {Graham}, M., {McCully}, C., , {Graur}, O., et al. (2016). SN Refsdal: Classification as a Luminous and Blue SN 1987A-like Type II Supernova. \apj, 831, 205.
• {Kelly}, P., {Rodney}, S., {Treu}, T., {Strolger}, L., {Foley}, R., {Jha}, S., {Selsing}, J., {Brammer}, G., {Brada{\v c}}, M., {Cenko}, S., {Graur}, O., {Filippenko}, A., {Hjorth}, J., {McCully}, C., {Molino}, A., {Nonino}, M., {Riess}, A., {Schmidt}, K., {Tucker}, B., , Linden}, A., et al. (2016). Deja Vu All Over Again: The Reappearance of Supernova Refsdal. \apjl, 819, L8.
• {Rawle}, T., {Altieri}, B., {Egami}, E., {P{\'e}rez-Gonz{\'a}lez}, P., {Boone}, F., {Clement}, B., {Ivison}, R., {Richard}, J., {Rujopakarn}, W., {Valtchanov}, I., {Walth}, G., {Weiner}, B., {Blain}, A., {Dessauges-Zavadsky}, M., {Kneib}, J., {Lutz}, D., {Rodighiero}, G., {Schaerer}, D., , I. (2016). A complete census of Herschel-detected infrared sources within the HST Frontier Fields. \mnras, 459, 1626-1645.
• {Rodney}, S., {Strolger}, L., {Kelly}, P., {Brada{\v c}}, M., {Brammer}, G., {Filippenko}, A., {Foley}, R., {Graur}, O., {Hjorth}, J., {Jha}, S., {McCully}, C., {Molino}, A., {Riess}, A., {Schmidt}, K., {Selsing}, J., {Sharon}, K., {Treu}, T., {Weiner}, B., , A. (2016). SN Refsdal: Photometry and Time Delay Measurements of the First Einstein Cross Supernova. \apj, 820, 50.
• {Rujopakarn}, W., {Dunlop}, J., {Rieke}, G., {Ivison}, R., {Cibinel}, A., {Nyland}, K., {Jagannathan}, P., {Silverman}, J., {Alexander}, D., {Biggs}, A., {Bhatnagar}, S., {Ballantyne}, D., {Dickinson}, M., {Elbaz}, D., {Geach}, J., {Hayward}, C., {Kirkpatrick}, A., {McLure}, R., {Micha{\l}owski}, M., , {Miller}, N., et al. (2016). VLA and ALMA Imaging of Intense Galaxy-wide Star Formation in z {\tilde} 2 Galaxies. \apj, 833, 12.
• {Simons}, R., {Kassin}, S., {Trump}, J., {Weiner}, B., {Heckman}, T., {Barro}, G., {Koo}, D., {Guo}, Y., {Pacifici}, C., {Koekemoer}, A., , A. (2016). Kinematic Downsizing at z {\tilde} 2. \apj, 830, 14.
• Alam, S., Albareti, F. D., Allende, P. C., Anders, F., Anderson, S. F., Anderton, T., Andrews, B. H., Armengaud, E., Aubourg, E., Bailey, S., Basu, S., Bautista, J. E., Beaton, R. L., Beers, T. C., Bender, C. F., Berlind, A. A., Beutler, F., Bhardwaj, V., Bird, J. C., , Bizyaev, D., et al. (2015). THE ELEVENTH AND TWELFTH DATA RELEASES OF THE SLOAN DIGITAL SKY SURVEY: FINAL DATA FROM SDSS-III. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 219(1).
• Genzel, R., Tacconi, L. J., Lutz, D., Saintonge, A., Berta, S., Magnelli, B., Combes, F., Garcia-Burillo, S., Neri, R., Bolatto, A., Contini, T., Lilly, S., Boissier, J., Boone, F., Bouche, N., Bournaud, F., Burkert, A., Carollo, M., Colina, L., , Cooper, M. C., et al. (2015). COMBINED CO AND DUST SCALING RELATIONS OF DEPLETION TIME AND MOLECULAR GAS FRACTIONS WITH COSMIC TIME, SPECIFIC STAR-FORMATION RATE, AND STELLAR MASS. ASTROPHYSICAL JOURNAL, 800(1).
• Kartaltepe, J. S., Mozena, M., Kocevski, D., McIntosh, D. H., Lotz, J., Bell, E. F., Faber, S., Ferguson, H., Koo, D., Bassett, R., Bernyk, M., Blancato, K., Bournaud, F., Cassata, P., Castellano, M., Cheung, E., Conselice, C. J., Croton, D., Dahlen, T., , De Mello, D. F., et al. (2015). Candels visual classifications: Scheme, data release, and first results. Astrophysical Journal, Supplement Series, 221(Issue 1). doi:10.1088/0067-0049/221/1/11
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  We have undertaken an ambitious program to visually classify all galaxies in the five CANDELS fields down to H < 24.5 involving the dedicated efforts of over 65 individual classifiers. Once completed, we expect to have detailed morphological classifications for over 50,000 galaxies spanning 0 < z < 4 over all the fields, with classifications from 3 to 5 independent classifiers for each galaxy. Here, we present our detailed visual classification scheme, which was designed to cover a wide range of CANDELS science goals. This scheme includes the basic Hubble sequence types, but also includes a detailed look at mergers and interactions, the clumpiness of galaxies, k-corrections, and a variety of other structural properties. In this paper, we focus on the first field to be completed - GOODS-S, which has been classified at various depths. The wide area coverage spanning the full field (wide+deep+ERS) includes 7634 galaxies that have been classified by at least three different people. In the deep area of the field, 2534 galaxies have been classified by at least five different people at three different depths. With this paper, we release to the public all of the visual classifications in GOODS-S along with the Perl/Tk GUI that we developed to classify galaxies. We present our initial results here, including an analysis of our internal consistency and comparisons among multiple classifiers as well as a comparison to the Sé index.We find that the level of agreement among classifiers is quite good (>70% across the full magnitude range) and depends on both the galaxy magnitude and the galaxy type, with disks showing the highest level of agreement (>50%) and irregulars the lowest (
• Kartaltepe, J. S., Mozena, M., Kocevski, D., McIntosh, D. H., Lotz, J., Bell, E. F., Faber, S., Ferguson, H., Koo, D., Bassett, R., Bernyk, M., Blancato, K., Bournaud, F., Cassata, P., Castellano, M., Cheung, E., Conselice, C. J., Croton, D., Dahlen, T., , De, M., et al. (2015). CANDELS VISUAL CLASSIFICATIONS: SCHEME, DATA RELEASE, AND FIRST RESULTS. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 221(1).
• Kelly, P. L., Rodney, S. A., Treu, T., Foley, R. J., Brammer, G., Schmidt, K. B., Zitrin, A., Sonnenfeld, A., Strolger, L., Graur, O. r., Filippenko, A. V., Jha, S. W., Riess, A. G., Bradac, M., Weiner, B. J., Scolnic, D., Malkan, M. A., von, d., Trenti, M., , Hjorth, J., et al. (2015). Multiple images of a highly magnified supernova formed by an early-type cluster galaxy lens. SCIENCE, 347(6226), 1123-1126.
• Mei, S., Scarlata, C., Pentericci, L., Newman, J. A., Weiner, B. J., Ashby, M., Castellano, M., Conselice, C. J., Finkelstein, S. L., Galametz, A., Grogin, N. A., Koekemoer, A. M., Huertas-Company, M., Lani, C., Lucas, R. A., Papovich, C., Rafelski, M., & Teplitz, H. I. (2015). STAR-FORMING BLUE ETGS IN TWO NEWLY DISCOVERED GALAXY OVERDENSITIES IN THE HUDF AT z=1.84 AND 1.9: UNVEILING THE PROGENITORS OF PASSIVE ETGS IN CLUSTER CORES. ASTROPHYSICAL JOURNAL, 804(2).
• Morris, A. M., Kocevski, D. D., Trump, J. R., Weiner, B. J., Hathi, N. P., Barro, G., Dahlen, T., Faber, S. M., Finkelstein, S. L., Fontana, A., Ferguson, H. C., Grogin, N. A., Gruetzbauch, R., Guo, Y., Hsu, L., Koekemoer, A. M., Koo, D. C., Mobasher, B., Pforr, J., , Salvato, M., et al. (2015). A WFC3 GRISM EMISSION LINE REDSHIFT CATALOG IN THE GOODS-SOUTH FIELD. ASTRONOMICAL JOURNAL, 149(6).
• Morris, A. M., Kocevski, D. D., Trump, J. R., Weiner, B. J., Hathi, N. P., Barro, G., Dahlen, T., Faber, S. M., Finkelstein, S. L., Fontana, A., Ferguson, H. C., Grogin, N. A., Grützbauch, R., Guo, Y., Hsu, L. T., Koekemoer, A. M., Koo, D. C., Mobasher, B., Pforr, J., , Salvato, M., et al. (2015). A WFC3 grism emission line redshift catalog in the goods-south field. Astronomical Journal, 149(Issue 6). doi:10.1088/0004-6256/149/6/178
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  We combine Hubble Space Telescope (HST)/Wide Field Camera3 (WFC3) imaging and G141 grism observations from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) and 3D-HST surveys to produce a catalog of grism spectroscopic redshifts for galaxies in the CANDELS/GOODS-South field. The WFC3/G141 grism spectra cover a wavelength range of 1.1 ≤ λ ≤ 1.7 μm with a resolving power of for point sources, thus providing rest-frame optical spectra for galaxies out to z ∼ 3.5 . The catalog is selected in the H-band (F160W) and includes both galaxies with and without previously published spectroscopic redshifts. Grism spectra are extracted for all H-band detected galaxies with H ≤ 24 and a CANDELS photometric redshift zphot ≥ 0.6. The resulting spectra are visually inspected to identify emission lines, and redshifts are determined using cross-correlation with empirical spectral templates. To establish the accuracy of our redshifts, we compare our results against high-quality spectroscopic redshifts from the literature. Using a sample of 411 control galaxies, this analysis yields a precision of σNMAD = 0.0028 for the grism-derived redshifts, which is consistent with the accuracy reported by the 3D-HST team. Our final catalog covers an area of 153 arcmin2 and contains 1019 redshifts for galaxies in GOODS-S. Roughly 60% (608/1019) of these redshifts are for galaxies with no previously published spectroscopic redshift. These new redshifts span a range of 0.677 ≤ z ≤ 3.456 and have a median redshift of z = 1.282. The catalog contains a total of 234 new redshifts for galaxies at z > 1.5.. In addition, we present 20 galaxy pair candidates identified for the first time using the grism redshifts in our catalog, including four new galaxy pairs at z ∼ 2,, nearly doubling the number of such pairs previously identified.
• Penner, K., Dickinson, M., Weiner, B., Inami, H., Kartaltepe, J., Pforr, J., Nayyeri, H., Kassin, S., Papovich, C., & Pope, A. (2015). Dusty galaxies and the degeneracy between their dust distributions and the attenuation formula.
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  Do spatial distributions of dust grains in galaxies have typical forms, as dospatial distributions of stars? We investigate whether or not the distributionsresemble uniform foreground screens, as commonly assumed by the high-redshiftgalaxy community. We use rest-frame infrared, ultraviolet, and H$\alpha$ lineluminosities of dust-poor and dusty galaxies at z ~ 0 and z ~ 1 to comparemeasured H$\alpha$ escape fractions with those predicted by the Calzettiattenuation formula. The predictions, based on UV escape fractions,overestimate the measured H$\alpha$ escape fractions for all samples. Theinterpretation of this result for dust-poor z ~ 0 galaxies is that regions withionizing stars have more dust than regions with nonionizing UV-emitting stars.Dust distributions for these galaxies are nonuniform. The interpretation of theoverestimates for dusty galaxies at both redshifts is less clear. If theattenuation formula is inapplicable to these galaxies, perhaps thedisagreements are unphysical; perhaps dust distributions in these galaxies areuniform. If the attenuation formula does apply, then dusty galaxies havenonuniform dust distributions; the distributions are more uniform than they arein dust-poor galaxies. A broad range of H$\alpha$ escape fractions at a givenUV escape fraction for z ~ 1 dusty galaxies, if real, indicates diverse dustmorphologies and the implausibility of the screen assumption.[Journal_ref: ]
• Santini, P., Ferguson, H. C., Fontana, A., Mobasher, B., Barro, G., Castellano, M., Finkelstein, S. L., Grazian, A., Hsu, L. T., Lee, B., Lee, S. K., Pforr, J., Salvato, M., Wiklind, T., Wuyts, S., Almaini, O., Cooper, M. C., Galametz, A., Weiner, B., , Amorin, R., et al. (2015). Stellar masses from the candels survey: The goods-south and uds fields. Astrophysical Journal, 801(Issue 2). doi:10.1088/0004-637x/801/2/97
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  We present the public release of the stellar mass catalogs for the GOODS-S and UDS fields obtained using some of the deepest near-IR images available, achieved as part of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey project. We combine the effort from 10 different teams, who computed the stellar masses using the same photometry and the same redshifts. Each team adopted their preferred fitting code, assumptions, priors, and parameter grid. The combination of results using the same underlying stellar isochrones reduces the systematics associated with the fitting code and other choices. Thanks to the availability of different estimates, we can test the effect of some specific parameters and assumptions on the stellar mass estimate. The choice of the stellar isochrone library turns out to have the largest effect on the galaxy stellar mass estimates, resulting in the largest distributions around the median value (with a semi interquartile range larger than 0.1 dex). On the other hand, for most galaxies, the stellar mass estimates are relatively insensitive to the different parameterizations of the star formation history. The inclusion of nebular emission in the model spectra does not have a significant impact for the majority of galaxies (less than a factor of 2 for 80% of the sample). Nevertheless, the stellar mass for the subsample of young galaxies (age
• Simons, R. C., Kassin, S. A., Weiner, B. J., Heckman, T. M., Lee, J. C., Lotz, J. M., Peth, M., & Tchernyshyov, K. (2015). A transition mass in the local Tully-Fisher relation. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 452(1), 986-997.
• Williams, C. C., Giavalisco, M., Lee, B., Tundo, E., Mobasher, B., Nayyeri, H., Ferguson, H. C., Koekemoer, A., Trump, J. R., Cassata, P., Dekel, A., Guo, Y., Lee, K., Pentericci, L., Bell, E. F., Castellano, M., Finkelstein, S. L., Fontana, A., Grazian, A., , Grogin, N., et al. (2015). THE INTERSTELLAR MEDIUM AND FEEDBACK IN THE PROGENITORS OF THE COMPACT PASSIVE GALAXIES AT z similar to 2. ASTROPHYSICAL JOURNAL, 800(1).
• {Alam}, S., {Albareti}, F., {Allende Prieto}, C., {Anders}, F., {Anderson}, S., {Anderton}, T., {Andrews}, B., {Armengaud}, E., {Aubourg}, {., {Bailey}, S., & al., e. (2015). "{The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data from SDSS-III}". apjs, 219, 12.
• {Genzel}, R., {Tacconi}, L., {Lutz}, D., {Saintonge}, A., {Berta}, S., {Magnelli}, B., {Combes}, F., {Garc{'{i}}a-Burillo}, S., {Neri}, R., {Bolatto}, A., {Contini}, T., {Lilly}, S., {Boissier}, J., {Boone}, F., {Bouch{'e}}, N., {Bournaud}, F., {Burkert}, A., {Carollo}, M., {Colina}, L., , {Cooper}, M., et al. (2015). "{Combined CO and Dust Scaling Relations of Depletion Time and Molecular Gas Fractions with Cosmic Time, Specific Star-formation Rate, and Stellar Mass}". apj, 800, 20.
• {Kartaltepe}, J., {Mozena}, M., {Kocevski}, D., {McIntosh}, D., {Lotz}, J., {Bell}, E., {Faber}, S., {Ferguson}, H., {Koo}, D., {Bassett}, R., {Bernyk}, M., {Blancato}, K., {Bournaud}, F., {Cassata}, P., {Castellano}, M., {Cheung}, E., {Conselice}, C., {Croton}, D., {Dahlen}, T., , {de Mello}, D., et al. (2015). "{CANDELS Visual Classifications: Scheme, Data Release, and First Results}". apjs, 221, 11.
• {Kelly}, P., {Rodney}, S., {Brammer}, G., {Strolger}, L., {Foley}, R., {Treu}, T., {Zitrin}, A., {Filippenko}, A., {Jha}, S., {Riess}, A., {Hjorth}, J., {Schmidt}, K., {Graur}, O., {Bradac}, M., {Weiner}, B., {Linden}, A., {McCully}, C., {Molino}, A., {Selsing}, J., , {Nonino}, M., et al. (2015). "{Detection of a SN near the center of the galaxy cluster field MACS1149 consistent with predictions of a new image of Supernova Refsdal}". The Astronomer's Telegram, 8402.
• {Kelly}, P., {Rodney}, S., {Treu}, T., {Foley}, R., {Brammer}, G., {Schmidt}, K., {Zitrin}, A., {Sonnenfeld}, A., {Strolger}, L., {Graur}, O., {Filippenko}, A., {Jha}, S., {Riess}, A., {Bradac}, M., {Weiner}, B., {Scolnic}, D., {Malkan}, M., Linden}, A., {Trenti}, M., , {Hjorth}, J., et al. (2015). "{Multiple images of a highly magnified supernova formed by an early-type cluster galaxy lens}". Science, 347, 1123-1126.
• {Mei}, S., {Scarlata}, C., {Pentericci}, L., {Newman}, J., {Weiner}, B., {Ashby}, M., {Castellano}, M., {Conselice}, C., {Finkelstein}, S., {Galametz}, A., {Grogin}, N., {Koekemoer}, A., {Huertas-Company}, M., {Lani}, C., {Lucas}, R., {Papovich}, C., {Rafelski}, M., , H. (2015). "{Star-forming Blue ETGs in Two Newly Discovered Galaxy Overdensities in the HUDF at z=1.84 and 1.9: Unveiling the Progenitors of Passive ETGs in Cluster Cores}". apj, 804, 117.
• {Morris}, A., {Kocevski}, D., {Trump}, J., {Weiner}, B., {Hathi}, N., {Barro}, G., {Dahlen}, T., {Faber}, S., {Finkelstein}, S., {Fontana}, A., {Ferguson}, H., {Grogin}, N., {Gr{"u}tzbauch}, R., {Guo}, Y., {Hsu}, L., {Koekemoer}, A., {Koo}, D., {Mobasher}, B., {Pforr}, J., , {Salvato}, M., et al. (2015). "{A WFC3 Grism Emission Line Redshift Catalog in the GOODS-South Field}". aj, 149, 178.
• {Papovich}, C., {Labb{'e}}, I., {Quadri}, R., {Tilvi}, V., {Behroozi}, P., {Bell}, E., {Glazebrook}, K., {Spitler}, L., {Straatman}, C., {Tran}, K., {Cowley}, M., {Dav{'e}}, R., {Dekel}, A., {Dickinson}, M., {Ferguson}, H., {Finkelstein}, S., {Gawiser}, E., {Inami}, H., {Faber}, S., , {Kacprzak}, G., et al. (2015). "{ZFOURGE/CANDELS: On the Evolution of M* Galaxy Progenitors from z = 3 to 0.5}". apj, 803, 26.
• {Popping}, G., {Caputi}, K., {Trager}, S., {Somerville}, R., {Dekel}, A., {Kassin}, S., {Kocevski}, D., {Koekemoer}, A., {Faber}, S., {Ferguson}, H., {Galametz}, A., {Grogin}, N., {Guo}, Y., {Lu}, Y., {Wel}, A., , B. (2015). "{The inferred evolution of the cold gas properties of CANDELS galaxies at 0.5 $lt$ z $lt$ 3.0}". mnras, 454, 2258-2276.
• {Santini}, P., {Ferguson}, H., {Fontana}, A., {Mobasher}, B., {Barro}, G., {Castellano}, M., {Finkelstein}, S., {Grazian}, A., {Hsu}, L., {Lee}, B., {Lee}, S., {Pforr}, J., {Salvato}, M., {Wiklind}, T., {Wuyts}, S., {Almaini}, O., {Cooper}, M., {Galametz}, A., {Weiner}, B., , {Amorin}, R., et al. (2015). "{Stellar Masses from the CANDELS Survey: The GOODS-South and UDS Fields}". apj, 801, 97.
• {Simons}, R., {Kassin}, S., {Weiner}, B., {Heckman}, T., {Lee}, J., {Lotz}, J., {Peth}, M., , K. (2015). "{A transition mass in the local Tully-Fisher relation}". mnras, 452, 986-997.
• {Williams}, C., {Giavalisco}, M., {Lee}, B., {Tundo}, E., {Mobasher}, B., {Nayyeri}, H., {Ferguson}, H., {Koekemoer}, A., {Trump}, J., {Cassata}, P., {Dekel}, A., {Guo}, Y., {Lee}, K., {Pentericci}, L., {Bell}, E., {Castellano}, M., {Finkelstein}, S., {Fontana}, A., {Grazian}, A., , {Grogin}, N., et al. (2015). "{The Interstellar Medium and Feedback in the Progenitors of the Compact Passive Galaxies at z ~{} 2}". apj, 800, 21.
• Ahn, C. P., Alexandroff, R., Allende Prieto, C., Anders, F., Anderson, S. F., Anderton, T., Andrews, B. H., Aubourg, '., Bailey, S., Bastien, F. A., & al., e. (2014). The Tenth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-III Apache Point Observatory Galactic Evolution Experiment. apjs, 211, 17.
• Ahn, C. P., Alexandroff, R., Allende, P. C., Anders, F., Anderson, S. F., Anderton, T., Andrews, B. H., Aubourg, E., Bailey, S., Bastien, F. A., Bautista, J. E., Beers, T. C., Beifiori, A., Bender, C. F., Berlind, A. A., Beutler, F., Bhardwaj, V., Bird, J. C., Bizyaev, D., , Blake, C. H., et al. (2014). THE TENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST SPECTROSCOPIC DATA FROM THE SDSS-III APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 211(2).
• Alberts, S., Pope, A., Brodwin, M., Atlee, D. W., Lin, Y., Dey, A., Eisenhardt, P. R., Gettings, D. P., Gonzalez, A. H., Jannuzi, B. T., Mancone, C. L., Moustakas, J., Snyder, G. F., Stanford, S. A., Stern, D., Weiner, B. J., & Zeimann, G. R. (2014). The evolution of dust-obscured star formation activity in galaxy clusters relative to the field over the last 9 billion years. mnras, 437, 437-457.
• Alberts, S., Pope, A., Brodwin, M., Atlee, D. W., Lin, Y., Dey, A., Eisenhardt, P., Gettings, D. P., Gonzalez, A. H., Jannuzi, B. T., Mancone, C. L., Moustakas, J., Snyder, G. F., Stanford, S. A., Stern, D., Weiner, B. J., & Zeimann, G. R. (2014). The evolution of dust-obscured star formation activity in galaxy clusters relative to the field over the last 9 billion years. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 437(1), 437-457.
• Bradac, M., Brammer, G. B., Cenko, S. B., Dressler, A., Filippenko, A. V., Foley, R. J., Fontana, A., Gavazzi, R., Graham, M. L., Graur, O., Hjorth, J., Jha, S., Jones, T., Kelly, P. L., Linden, A. V., Malkan, M. A., Mccully, C., Merten, J., Patel, B., , Postman, M., et al. (2014). Hubble Space Telescope discovery of a multiply imaged, gravitationally lensed supernova. The astronomer's telegram, 6729.
• Brooks, A., Gardner, J. P., Governato, F., Kassin, S. A., & Weiner, B. J. (2014). Kinematic evolution of simulated star-forming galaxies. The Astrophysical Journal, 790(2), 89. doi:10.1088/0004-637x/790/2/89
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  Recent observations have shown that star-forming galaxies like our own Milky Way evolve kinematically into ordered thin disks over the last ∼8 billion years since z = 1.2, undergoing a process of 'disk settling'. For the first time, we study the kinematic evolution of a suite of four state of the art 'zoom in' hydrodynamic simulations of galaxy formation and evolution in a fully cosmological context and compare with these observations. Until now, robust measurements of the internal kinematics of simulated galaxies were lacking because the simulations suffered from low resolution, overproduction of stars, and overly massive bulges. The current generation of simulations has made great progress in overcoming these difficulties and is ready for a kinematic analysis. We show that simulated galaxies follow the same kinematic trends as real galaxies: they progressively decrease in disordered motions (σ{sub g}) and increase in ordered rotation (V{sub rot}) with time. The slopes of the relations between both σ{sub g} and V{sub rot} with redshift are consistent between the simulations and the observations. In addition, the morphologies of the simulated galaxies become less disturbed with time, also consistent with observations. This match between the simulated and observed trends is a significant success formore » the current generation of simulations, and a first step in determining the physical processes behind disk settling'.« less
• Buitrago, F., Conselice, C. J., Epinat, B., Bedregal, A. G., Gr "utzbauch, R., & Weiner, B. J. (2014). SINFONI/VLT 3D spectroscopy of massive galaxies: evidence of rotational support at z tilde 1.4. mnras, 439, 1494-1521.
• Buitrago, F., Conselice, C. J., Epinat, B., Bedregal, A. G., Gruetzbauch, R., & Weiner, B. J. (2014). SINFONI/VLT 3D spectroscopy of massive galaxies: evidence of rotational support at z similar to 1.4. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 439(2), 1494-1521.
• Buitrago, F., Conselice, C. J., Epinat, B., Bedregal, A. G., Grutzbauch, R., & Weiner, B. J. (2014). SINFONI/VLT 3D spectroscopy of massive galaxies: Evidence of rotational support at z~1.4.
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  There is cumulative evidence showing that, for the most massive galaxies, thefraction of disk-like objects compared to those with spheroidal propertiesincreases with redshift. However, this evolution is thus far based on thesurface brightness study of these objects. To explore the consistency of thisscenario, it is necessary to measure the dynamical status of these galaxies.With this aim we have obtained seeing-limited near-infrared integral fieldspectra in the H-band for 10 massive galaxies (M_{stellar} >10^{11} h_{70}^-2M_{Sun}) at z~1.4 with SINFONI at the VLT. Our sample is selected by theirstellar mass and EW[OII] > 15 \AA, to secure their kinematic measurements, butwithout accounting for any morphological or flux criteria a priori. Throughthis 3D kinematic spectroscopy analysis we find that half (i.e. 50+/-7%) of ourgalaxies are compatible with being rotationally supported disks, in agreementwith previous morphological expectations. This is a factor of approximately twohigher than what is observed in the present Universe for objects of the samestellar mass. Strikingly, the majority of our sample of massive galaxies showextended and fairly high rotational velocity maps, implying that massivegalaxies acquire rapidly rotational support and hence gravitationalequilibrium. Our sample also show evidence for ongoing interactions andmergers. Summarizing, massive galaxies at high-z show a significant diversityand must have continued evolution beyond the fading of stellar populations, tobecome their present day counterparts.[Journal_ref: ]
• Decarli, R., Walter, F., Carilli, C., Riechers, D., Cox, P., Neri, R., Aravena, M., Bell, E., Bertoldi, F., Colombo, D., Da Cunha, E., Daddi, E., Dickinson, M., Downes, D., Ellis, R., Lentati, L., Maiolino, R., Menten, K. M., Rix, H. W., , Sargent, M., et al. (2014). A MOLECULAR LINE SCAN IN THE HUBBLE DEEP FIELD NORTH. The Astrophysical Journal, 782(2), 78. doi:10.1088/0004-637x/782/2/78
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  We present a molecular line scan in the Hubble Deep Field North (HDF-N) that covers the entire 3 mm window (79-115 GHz) using the IRAM Plateau de Bure Interferometer. Our CO redshift coverage spans z ≾ 0.45, 1 ≾ z ≾ 1.9 and all z ≳ 2. We reach a CO detection limit that is deep enough to detect essentially all z > 1 CO lines reported in the literature so far. We have developed and applied different line-searching algorithms, resulting in the discovery of 17 line candidates. We estimate that the rate of false positive line detections is ~2/17. We identify optical/NIR counterparts from the deep ancillary database of the HDF-N for seven of these candidates and investigate their available spectral energy distributions. Two secure CO detections in our scan are identified with star-forming galaxies at z = 1.784 and at z = 2.047. These galaxies have colors consistent with the "BzK" color selection and they show relatively bright CO emission compared with galaxies of similar dust continuum luminosity. We also detect two spectral lines in the submillimeter galaxy HDF 850.1 at z = 5.183. We consider an additional nine line candidates as high quality. Our observations also provide a deep 3 mm continuum map (1σ noise level = 8.6 μJy beam^(–1)). Via a stacking approach, we find that optical/MIR bright galaxies contribute only to
• Decarli, R., Walter, F., Carilli, C., Riechers, D., Cox, P., Neri, R., Aravena, M., Bell, E., Bertoldi, F., Colombo, D., Da Cunha, E., Daddi, E., Dickinson, M., Downes, D., Ellis, R., Lentati, L., Maiolino, R., Menten, K. M., Rix, H., , Sargent, M., et al. (2014). A Molecular Line Scan in the Hubble Deep Field North. apj, 782, 78.
• Dolley, T., Brown, M. J., Weiner, B. J., Brodwin, M., Kochanek, C. S., Pimbblet, K. A., Palamara, D. P., Jannuzi, B. T., Dey, A., Atlee, D. W., & Beare, R. (2014). THE CLUSTERING AND HALO MASSES OF STAR-FORMING GALAXIES AT z < 1. ASTROPHYSICAL JOURNAL, 797(2).
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  We present clustering measurements and halo masses of star-forming galaxies at 0.2 < z < 1.0. After excluding active galactic nuclei (AGNs), we construct a sample of 22,553 24 mu m sources selected from 8.42 deg(2) of the Spitzer MIPS AGN and Galaxy Evolution Survey of Bootes. Mid-infrared imaging allows us to observe galaxies with the highest star formation rates (SFRs), less biased by dust obscuration afflicting the optical bands. We find that the galaxies with the highest SFRs have optical colors that are redder than typical blue cloud galaxies, with many residing within the green valley. At z > 0.4 our sample is dominated by luminous infrared galaxies (LIRGs, L-TIR > 10(11) L-circle plus) and is composed entirely of LIRGs and ultraluminous infrared galaxies (ULIRGs, L-TIR > 10(12) L-circle plus) at z > 0.6. We observe weak clustering of r(0) approximate to 3-6 h(-1) Mpc for almost all of our star-forming samples. We find that the clustering and halo mass depend on L-TIR at all redshifts, where galaxies with higher LTIR (hence higher SFRs) have stronger clustering. Galaxies with the highest SFRs at each redshift typically reside within dark matter halos of M-halo approximate to 10(12.9) h(-1) M-circle plus. This is consistent with a transitional halo mass, above which star formation is largely truncated, although we cannot exclude that ULIRGs reside within higher mass halos. By modeling the clustering evolution of halos, we connect our star-forming galaxy samples to their local descendants. Most star-forming galaxies at z < 1.0 are the progenitors of L less than or similar to 2.5L(*) blue galaxies in the local universe, but star-forming galaxies with the highest SFRs (L-TIR greater than or similar to 10(11.7) L-circle plus) at 0.6 < z < 1.0 are the progenitors of early-type galaxies in denser group environments.
• Dolley, T., Brown, M. J., Weiner, B. J., Brodwin, M., Kochanek, C. S., Pimbblet, K. A., Palamara, D. P., Jannuzi, B. T., Dey, A., Atlee, D. W., & Beare, R. (2014). The Clustering and Halo Masses of Star-forming Galaxies at z < 1. The Astrophysical Journal, 797(2), 125. doi:10.1088/0004-637x/797/2/125
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  We present clustering measurements and halo masses of star forming galaxies at 0:2 0:4 our sample is dominated by luminous infrared galaxies (LIRGs, LTIR > 10 11 L ) and is comprised entirely of LIRGs and ultra-luminous infrared galaxies (ULIRGs, LTIR> 10 12 L ) at z> 0:6. We observe weak clustering of r0 3- 6 h -1 Mpc for almost all of our star forming samples. We find that the clustering and halo mass depend on LTIR at all redshifts, where galaxies with higher LTIR (hence higher SFRs) have stronger clustering. Galaxies with the highest SFRs at each redshift typically reside within dark matter halos of Mhalo 10 12:9 h -1 M . This is consistent with a transitional halo mass, above which star formation is largely truncated, although we cannot exclude that ULIRGs reside within higher mass halos. By modeling the clustering evolution of halos, we connect our star forming galaxy samples to their local descendants. Most star forming galaxies at z< 1:0 are the progenitors of L . 2:5L blue galaxies in the local universe, but star forming galaxies with the highest SFRs (LTIR & 10 11:7 L ) at 0:6
• Gott, J. R., Mack, C. E., Ahn, C. P., Alexandroff, R., Allende Prieto, C., Anders, F., Anderson, S. F., Anderton, T., Andrews, B. H., Aubourg, É., Bailey, S., Bastien, F. A., Bautista, J. E., Beers, T. C., Beifiori, A., Bender, C. F., Berlind, A. A., Beutler, F., Bhardwaj, V., , Bird, J. C., et al. (2014). The tenth data release of the Sloan digital sky survey: First spectroscopic data from the SDSS-iii apache point observatory galactic evolution experiment. Astrophysical Journal Supplement Series, 211(2), 17-17. doi:10.1088/0067-0049/211/2/17
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  The Sloan Digital Sky Survey (SDSS) has been in operation since 2000 April. This paper presents the Tenth Public Data Release (DR10) from its current incarnation, SDSS-III. This data release includes the first spectroscopic data from the Apache Point Observatory Galaxy Evolution Experiment (APOGEE), along with spectroscopic data from the Baryon Oscillation Spectroscopic Survey (BOSS) taken through 2012 July. The APOGEE instrument is a near-infrared R ~ 22,500 300 fiber spectrograph covering 1.514-1.696 μm. The APOGEE survey is studying the chemical abundances and radial velocities of roughly 100,000 red giant star candidates in the bulge, bar, disk, and halo of the Milky Way. DR10 includes 178,397 spectra of 57,454 stars, each typically observed three or more times, from APOGEE. Derived quantities from these spectra (radial velocities, effective temperatures, surface gravities, and metallicities) are also included. DR10 also roughly doubles the number of BOSS spectra over those included in the Ninth Data Release. DR10 includes a total of 1,507,954 BOSS spectra comprising 927,844 galaxy spectra, 182,009 quasar spectra, and 159,327 stellar spectra selected over 6373.2 deg2.
• Goulding, A. D., Forman, W. R., Hickox, R. C., Jones, C., Murray, S. S., Paggi, A., Ashby, M. L., Coil, A. L., Cooper, M. C., Huang, J. S., Kraft, R., Newman, J. A., Weiner, B. J., & Willner, S. P. (2014). Tracing the evolution of active galactic nuclei host galaxies over the last 9 Gyr of cosmic time. Astrophysical Journal, 783(Issue 1). doi:10.1088/0004-637x/783/1/40
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  We present the results of a combined galaxy population analysis for the host galaxies of active galactic nuclei (AGN) identified at 0 < z < 1.4 within the Sloan Digital Sky Survey, Boötes, and DEEP2 surveys. We identified AGN in a uniform and unbiased manner at X-ray, infrared, and radio wavelengths. Supermassive black holes undergoing radiatively efficient accretion (detected as X-ray and/or infrared AGN) appear to be hosted in a separate and distinct galaxy population than AGN undergoing powerful mechanically dominated accretion (radio AGN). Consistent with some previous studies, radiatively efficient AGN appear to be preferentially hosted in modest star-forming galaxies, with little dependence on AGN or galaxy luminosity. AGN exhibiting radio-emitting jets due to mechanically dominated accretion are almost exclusively observed in massive, passive galaxies. Crucially, we now provide strong evidence that the observed host-galaxy trends are independent of redshift. In particular, these different accretion-mode AGN have remained as separate galaxy populations throughout the last 9 Gyr. Furthermore, it appears that galaxies hosting AGN have evolved along the same path as galaxies that are not hosting AGN with little evidence for distinctly separate evolution. © 2014. The American Astronomical Society. All rights reserved.
• Goulding, A. D., Forman, W. R., Hickox, R. C., Jones, C., Murray, S. S., Paggi, A., Ashby, M. L., Coil, A. L., Cooper, M. C., Huang, J., Kraft, R., Newman, J. A., Weiner, B. J., & Willner, S. P. (2014). Tracing the Evolution of Active Galactic Nuclei Host Galaxies over the Last 9 Gyr of Cosmic Time. apj, 783, 40.
• Kassin, S. A., Brooks, A., Governato, F., Weiner, B. J., & Gardner, J. P. (2014). KINEMATIC EVOLUTION OF SIMULATED STAR-FORMING GALAXIES. ASTROPHYSICAL JOURNAL, 790(2).
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  Recent observations have shown that star-forming galaxies like our own Milky Way evolve kinematically into ordered thin disks over the last similar to 8 billion years since z = 1.2, undergoing a process of "disk settling." For the first time, we study the kinematic evolution of a suite of four state of the art "zoom in" hydrodynamic simulations of galaxy formation and evolution in a fully cosmological context and compare with these observations. Until now, robust measurements of the internal kinematics of simulated galaxies were lacking because the simulations suffered from low resolution, overproduction of stars, and overly massive bulges. The current generation of simulations has made great progress in overcoming these difficulties and is ready for a kinematic analysis. We show that simulated galaxies follow the same kinematic trends as real galaxies: they progressively decrease in disordered motions (sigma(g)) and increase in ordered rotation (V-rot) with time. The slopes of the relations between both sigma(g) and V-rot with redshift are consistent between the simulations and the observations. In addition, the morphologies of the simulated galaxies become less disturbed with time, also consistent with observations. This match between the simulated and observed trends is a significant success for the current generation of simulations, and a first step in determining the physical processes behind disk settling.
• Kassin, S. A., Brooks, A., Governato, F., Weiner, B. J., & Gardner, J. P. (2014). Kinematic Evolution of Simulated Star-Forming Galaxies.
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  Recent observations have shown that star-forming galaxies like our own MilkyWay evolve kinematically into ordered thin disks over the last ~8 billion yearssince z=1.2, undergoing a process of "disk settling." For the first time, westudy the kinematic evolution of a suite of four state of the art "zoom in"hydrodynamic simulations of galaxy formation and evolution in a fullycosmological context and compare with these observations. Until now, robustmeasurements of the internal kinematics of simulated galaxies were lacking asthe simulations suffered from low resolution, overproduction of stars, andoverly massive bulges. The current generation of simulations has made greatprogress in overcoming these difficulties and is ready for a kinematicanalysis. We show that simulated galaxies follow the same kinematic trends asreal galaxies: they progressively decrease in disordered motions (sigma_g) andincrease in ordered rotation (Vrot) with time. The slopes of the relationsbetween both sigma_g and Vrot with redshift are consistent between thesimulations and the observations. In addition, the morphologies of thesimulated galaxies become less disturbed with time, also consistent withobservations, and they both have similarly large scatter. This match betweenthe simulated and observed trends is a significant success for the currentgeneration of simulations, and a first step in determining the physicalprocesses behind disk settling.[Journal_ref: ]
• Newman, S. F., Buschkamp, P., Genzel, R., Schreiber, N. M., Kurk, J., Sternberg, A., Gnat, O., Rosario, D., Mancini, C., Lilly, S. J., Renzini, A., Burkert, A., Carollo, C. M., Cresci, G., Davies, R., Eisenhauer, F., Genel, S., Shapiro Griffin, K., Hicks, E. K., , Lutz, D., et al. (2014). Nebular Excitation in z ~ 2 Star-forming Galaxies from the SINS and LUCI Surveys: The Influence of Shocks and Active Galactic Nuclei. apj, 781, 21.
• Newman, S. F., Buschkamp, P., Genzel, R., Schreiber, N., Kurk, J., Sternberg, A., Gnat, O., Rosario, D., Mancini, C., Lilly, S. J., Renzini, A., Burkert, A., Carollo, C. M., Cresci, G., Davies, R., Eisenhauer, F., Genel, S., Griffin, K. S., Hicks, E., , Lutz, D., et al. (2014). NEBULAR EXCITATION IN z similar to 2 STAR-FORMING GALAXIES FROM THE SINS AND LUCI SURVEYS: THE INFLUENCE OF SHOCKS AND ACTIVE GALACTIC NUCLEI. ASTROPHYSICAL JOURNAL, 781(1).
• Rodney, S. A., Riess, A. G., Strolger, L. G., Dahlen, T., Graur, O., Casertano, S., Dickinson, M. E., Ferguson, H. C., Garnavich, P., Hayden, B., Jha, S. W., Jones, D. O., Kirshner, R. P., Koekemoer, A. M., McCully, C., Mobasher, B., Patel, B., Weiner, B. J., Cenko, S. B., , Clubb, K. I., et al. (2014). Type Ia supernova rate measurements to redshift 2.5 from candels: Searching for prompt explosions in the early universe. Astronomical Journal, 148(Issue 1). doi:10.1088/0004-6256/148/1/13
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  The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) was a multi-cycle treasury program on the Hubble Space Telescope (HST) that surveyed a total area of ∼0.25 deg2 with ∼900 HST orbits spread across five fields over three years. Within these survey images we discovered 65 supernovae (SNe) of all types, out to z ∼ 2.5. We classify ∼24 of these as Type Ia SNe (SNe Ia) based on host galaxy redshifts and SN photometry (supplemented by grism spectroscopy of six SNe). Here we present a measurement of the volumetric SN Ia rate as a function of redshift, reaching for the first time beyond z = 2 and putting new constraints on SN Ia progenitor models. Our highest redshift bin includes detections of SNe that exploded when the universe was only ∼3 Gyr old and near the peak of the cosmic star formation history. This gives the CANDELS high redshift sample unique leverage for evaluating the fraction of SNe Ia that explode promptly after formation ( 40 Myr. However, mild tension is apparent between ground-based low-z surveys and space-based high-z surveys. In both CANDELS and the sister HST program CLASH (Cluster Lensing And Supernova Survey with Hubble), we find a low rate of SNe Ia at z > 1. This could be a hint that prompt progenitors are in fact relatively rare, accounting for only 20% of all SN Ia explosions - though further analysis and larger samples will be needed to examine that suggestion. © 2014. The American Astronomical Society. All rights reserved.
• Rodney, S. A., Riess, A. G., Strolger, L., Dahlen, T., Graur, O., Casertano, S., Dickinson, M. E., Ferguson, H. C., Garnavich, P., Hayden, B., Jha, S. W., Jones, D. O., Kirshner, R. P., Koekemoer, A. M., McCully, C., Mobasher, B., Patel, B., Weiner, B. J., Cenko, S. B., , Clubb, K. I., et al. (2014). TYPE Ia SUPERNOVA RATE MEASUREMENTS TO REDSHIFT 2.5 FROM CANDELS: SEARCHING FOR PROMPT EXPLOSIONS IN THE EARLY UNIVERSE. ASTRONOMICAL JOURNAL, 148(1).
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  dThe Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) was a multi-cycle treasury program on the Hubble Space Telescope (HST) that surveyed a total area of -0.25 deg2 with -900 HST orbits spread across five fields over three years. Within these survey images we discovered 65 supernovae (SNe) of all types, out to z 2.5. We classify -24 of these as Type Ia SNe (SNe Ia) based on host galaxy redshifts and SN photometry (supplemented by grism spectroscopy of six SNe). Here we present a measurement of the volumetric SN Ia rate as a function of redshift, reaching for the first time beyond z =- 2 and putting new constraints on SN Ia progenitor models. Our highest redshift bin includes detections of SNe that exploded when the universe was only -3 Gyr old and near the peak of the cosmic star formation history. This gives the CANDELS high redshift sample unique leverage for evaluating the fraction of SNe Ia that explode promptly after formation (
• Trump, J. R., Barro, G., Juneau, S., Weiner, B. J., Luo, B., Brammer, G. B., Bell, E. F., Brandt, W. N., Dekel, A., Guo, Y., Hopkins, P. F., Koo, D. C., Kocevski, D. D., McIntosh, D. H., Momcheva, I., Faber, S. M., Ferguson, H. C., Grogin, N. A., Kartaltepe, J., , Koekemoer, A. M., et al. (2014). NO MORE ACTIVE GALACTIC NUCLEI IN CLUMPY DISKS THAN IN SMOOTH GALAXIES AT z similar to 2 IN CANDELS/3D-HST. ASTROPHYSICAL JOURNAL, 793(2).
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  We use CANDELS imaging, 3D-HST spectroscopy, and Chandra X-ray data to investigate if active galactic nuclei (AGNs) are preferentially fueled by violent disk instabilities funneling gas into galaxy centers at 1.3 < z < 2.4. We select galaxies undergoing gravitational instabilities using the number of clumps and degree of patchiness as proxies. The CANDELS visual classification system is used to identify 44 clumpy disk galaxies, along with mass-matched comparison samples of smooth and intermediate morphology galaxies. We note that despite being mass-matched and having similar star formation rates, the smoother galaxies tend to be smaller disks with more prominent bulges compared to the clumpy galaxies. The lack of smooth extended disks is probably a general feature of the z similar to 2 galaxy population, and means we cannot directly compare with the clumpy and smooth extended disks observed at lower redshift. We find that z similar to 2 clumpy galaxies have slightly enhanced AGN fractions selected by integrated line ratios (in the mass-excitation method), but the spatially resolved line ratios indicate this is likely due to extended phenomena rather than nuclear AGNs. Meanwhile, the X-ray data show that clumpy, smooth, and intermediate galaxies have nearly indistinguishable AGN fractions derived from both individual detections and stacked non-detections. The data demonstrate that AGN fueling modes at z similar to 1.85-whether violent disk instabilities or secular processes-are as efficient in smooth galaxies as they are in clumpy galaxies.
• Trump, J. R., Barro, G., Juneau, S., Weiner, B. J., Luo, B., Brammer, G. B., Bell, E. F., Brandt, W. N., Dekel, A., Guo, Y., Hopkins, P. F., Koo, D. C., Kocevski, D. D., McIntosh, D. H., Momcheva, I., Faber, S. M., Ferguson, H. C., Grogin, N. A., Kartaltepe, J., , Koekemoer, A. M., et al. (2014). No more active galactic nuclei in clumpy disks than in smooth galaxies at z ∼ 2 in candels/3D-HST. Astrophysical Journal, 793(Issue 2). doi:10.1088/0004-637x/793/2/101
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  We use CANDELS imaging, 3D-HST spectroscopy, and Chandra X-ray data to investigate if active galactic nuclei (AGNs) are preferentially fueled by violent disk instabilities funneling gas into galaxy centers at 1.3 < z < 2.4. We select galaxies undergoing gravitational instabilities using the number of clumps and degree of patchiness as proxies. The CANDELS visual classification system is used to identify 44 clumpy disk galaxies, along with mass-matched comparison samples of smooth and intermediate morphology galaxies. We note that despite being mass-matched and having similar star formation rates, the smoother galaxies tend to be smaller disks with more prominent bulges compared to the clumpy galaxies. The lack of smooth extended disks is probably a general feature of the z ∼ 2 galaxy population, and means we cannot directly compare with the clumpy and smooth extended disks observed at lower redshift. We find that z ∼ 2 clumpy galaxies have slightly enhanced AGN fractions selected by integrated line ratios (in the mass-excitation method), but the spatially resolved line ratios indicate this is likely due to extended phenomena rather than nuclear AGNs. Meanwhile, the X-ray data show that clumpy, smooth, and intermediate galaxies have nearly indistinguishable AGN fractions derived from both individual detections and stacked non-detections. The data demonstrate that AGN fueling modes at z ∼ 1.85 - whether violent disk instabilities or secular processes - are as efficient in smooth galaxies as they are in clumpy galaxies.
• Walter, F., Decarli, R., Sargent, M., Carilli, C., Dickinson, M., Riechers, D., Ellis, R., Stark, D., Weiner, B., Aravena, M., Bell, E., Bertoldi, F., Cox, P., Da Cunha, E., Daddi, E., Downes, D., Lentati, L., Maiolino, R., Menten, K. M., , Neri, R., et al. (2014). A Molecular Line Scan in the Hubble Deep Field North: Constraints on the CO Luminosity Function and the Cosmic H$_2$ Density. apj, 782, 79.
• Walter, F., Decarli, R., Sargent, M., Carilli, C., Dickinson, M., Riechers, D., Ellis, R., Stark, D., Weiner, B., Aravena, M., Bell, E., Bertoldi, F., Cox, P., Da Cunha, E., Daddi, E., Downes, D., Lentati, L., Maiolino, R., Menten, K. M., , Neri, R., et al. (2014). A molecular line scan in the hubble deep field north: Constraints on the co luminosity function and the cosmic H2 density. Astrophysical Journal, 782(Issue 2). doi:10.1088/0004-637x/782/2/79
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  We present direct constraints on the CO luminosity function at high redshift and the resulting cosmic evolution of the molecular gas density, ρH2 (z), based on a blind molecular line scan in the Hubble Deep Field North (HDF-N) using the IRAM Plateau de Bure Interferometer. Our line scan of the entire 3 mm window (79-115 GHz) covers a cosmic volume of 7000 Mpc3, and redshift rangesz < 0.45, 1.01 < z < 1.89 andz > 2.We use the rich multiwavelength and spectroscopic database of the HDF-N to derive some of the best constraints on CO luminosities in high redshift galaxies to date. We combine the blind CO detections in our molecular line scan (presented in a companion paper) with stacked CO limits from galaxies with available spectroscopic redshifts (slit or mask spectroscopy from Keck and grism spectroscopy from the Hubble Space Telescope) to give first blind constraints on high-z CO luminosity functions and the cosmic evolution of the H2 mass density ρH2 (z) out to redshifts z 3. A comparison to empirical predictions of ρH2 (z) shows that the securely detected sources in our molecular line scan already provide significant contributions to the predicted ρH2 (z) in the redshift bins (z) 1.5 and (z) 2.7. Accounting for galaxies with CO luminosities that are not probed by our observations results in cosmic molecular gas densities ρH2 (z) that are higher than current predictions.We note, however, that the current uncertainties (in particular the luminosity limits, number of detections, as well as cosmic volume probed) are significant, a situation that is about to change with the emerging ALMA observatory. © 2014. The American Astronomical Society. All rights reserved.
• Alberts, S., Pope, A., Brodwin, M., Atlee, D. W., Lin, Y. T., Dey, A., Eisenhardt, P. R., Gettings, D. P., Gonzalez, A. H., Jannuzi, B. T., Mancone, C. L., Moustakas, J., Snyder, G. F., Stanford, S. A., Stern, D., Weiner, B. J., & Zeimann, G. R. (2013). The evolution of dust-obscured star formation activity in galaxy clusters relative to the field over the last 9 billion years. Monthly Notices of the Royal Astronomical Society, 437(Issue 1). doi:10.1093/mnras/stt1897
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  We compare the star formation (SF) activity in cluster galaxies to the field from z = 0.3 to 1.5 using Herschel Spectral and Photometric Imaging REceiver 250 μm imaging and utilizing 274 clusters from the IRAC Shallow Cluster Survey (ISCS). These clusters were selected as rest-frame near-infrared overdensities over the 9 square degree Boötes field. This sample allows us to quantify the evolution of SF in clusters over a long redshift baseline without bias against active cluster systems. Using a stacking analysis, we determine the average star formation rates (SFRs) and specific SFRs (SSFR = SFR/M*) of stellar mass-limited (M ≥ 1.3 × 1010M⊙), statistical samples of cluster and field galaxies, probing both the star-forming and quiescent populations. We find a clear indication that the average SF in cluster galaxies is evolving more rapidly than in the field, with field SF levels at z ≳ 1.2 in the cluster cores (r < 0.5 Mpc), in good agreement with previous ISCS studies. By quantifying the SF in cluster and field galaxies as an exponential function of cosmic time, we determine that cluster galaxies are evolving approximately two times faster than the field. Additionally, we see enhanced SF above the field level at z ~ 1.4 in the cluster outskirts (r > 0.5Mpc). These general trends in the cluster cores and outskirts are driven by the lower mass galaxies in our sample. Blue cluster galaxies have systematically lower SSFRs than blue field galaxies, but otherwise show no strong differential evolution with respect to the field over our redshift range. This suggests that the cluster environment is both suppressing the SF in blue galaxies on long time-scales and rapidly transitioning some fraction of blue galaxies to the quiescent galaxy population on short time-scales. We argue that our results are consistent with both strangulation and ram pressure stripping acting in these clusters, with merger activity occurring in the cluster outskirts. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
• Ashby, M. L., Willner, S. P., Fazio, G. G., Huang, J. S., Arendt, R., Barmby, P., Barro, G., Bell, E. F., Bouwens, R., Cattaneo, A., Croton, D., Davé, R., Dunlop, J. S., Egami, E., Faber, S., Finlator, K., Grogin, N. A., Guhathakurta, P., Hernquist, L., , Hora, J. L., et al. (2013). Seds: The spitzer extended deep survey. Survey design, photometry, and deep irac source counts. Astrophysical Journal, 769(Issue 1). doi:10.1088/0004-637x/769/1/80
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  The Spitzer Extended Deep Survey (SEDS) is a very deep infrared survey within five well-known extragalactic science fields: the UKIDSS Ultra-Deep Survey, the Extended Chandra Deep Field South, COSMOS, the Hubble Deep Field North, and the Extended Groth Strip. SEDS covers a total area of 1.46 deg 2 to a depth of 26 AB mag (3σ) in both of the warm Infrared Array Camera (IRAC) bands at 3.6 and 4.5 μm. Because of its uniform depth of coverage in so many widely-separated fields, SEDS is subject to roughly 25% smaller errors due to cosmic variance than a single-field survey of the same size. SEDS was designed to detect and characterize galaxies from intermediate to high redshifts (z = 2-7) with a built-in means of assessing the impact of cosmic variance on the individual fields. Because the full SEDS depth was accumulated in at least three separate visits to each field, typically with six-month intervals between visits, SEDS also furnishes an opportunity to assess the infrared variability of faint objects. This paper describes the SEDS survey design, processing, and publicly-available data products. Deep IRAC counts for the more than 300,000 galaxies detected by SEDS are consistent with models based on known galaxy populations. Discrete IRAC sources contribute 5.6 ± 1.0 and 4.4 ± 0.8 nW m-2 sr-1 at 3.6 and 4.5 μm to the diffuse cosmic infrared background (CIB). IRAC sources cannot contribute more than half of the total CIB flux estimated from DIRBE data. Barring an unexpected error in the DIRBE flux estimates, half the CIB flux must therefore come from a diffuse component. © 2013. The American Astronomical Society. All rights reserved.
• Ashby, M. L., Willner, S. P., Fazio, G. G., Huang, J., Arendt, R., Barmby, P., Barro, G., Bell, E. F., Bouwens, R., Cattaneo, A., Croton, D., Dav 'e, R., Dunlop, J. S., Egami, E., Faber, S., Finlator, K., Grogin, N. A., Guhathakurta, P., Hernquist, L., , Hora, J. L., et al. (2013). SEDS: The Spitzer Extended Deep Survey. Survey Design, Photometry, and Deep IRAC Source Counts. apj, 769, 80.
• Ashby, M., Willner, S. P., Fazio, G. G., Huang, J. -., Arendt, R., Barmby, P., Barro, G., Bell, E. F., Bouwens, R., Cattaneo, A., Croton, D., Dave, R., Dunlop, J. S., Egami, E., Faber, S., Finlator, K., Grogin, N. A., Guhathakurta, P., Hernquist, L., , Hora, J. L., et al. (2013). SEDS: THE SPITZER EXTENDED DEEP SURVEY. SURVEY DESIGN, PHOTOMETRY, AND DEEP IRAC SOURCE COUNTS. ASTROPHYSICAL JOURNAL, 769(1).
• Burkert, A., Buschkamp, P., Carollo, C. M., Cresci, G., Davies, R., Eisenhauer, F., Genel, S., Genzel, R., Gnat, O., Griffin, K. S., Hicks, E. K., Kurk, J., Lilly, S. J., Lutz, D., Mancini, C., Naab, T., Newman, S. F., Peng, Y., Renzini, A., , Rosario, D. J., et al. (2013). Nebular excitation in z ~ 2 star-forming galaxies from the SINS and LUCI surveys: the influence of shocks and active galactic nuclei. The Astrophysical Journal, 781(1), 21. doi:10.1088/0004-637x/781/1/21
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  Based on high-resolution, spatially resolved data of 10 z ~ 2 star-forming galaxies from the SINS/zC-SINF survey and LUCI data for 12 additional galaxies, we probe the excitation properties of high-z galaxies and the impact of active galactic nuclei (AGNs), shocks, and photoionization. We explore how these spatially resolved line ratios can inform our interpretation of integrated emission line ratios obtained at high redshift. Many of our galaxies fall in the composite region of the z ~ 0 [N II]/Hα versus [O III]/Hβ diagnostic (BPT) diagram, between star-forming galaxies and those with AGNs. Based on our resolved measurements, we find that some of these galaxies likely host an AGN, while others appear to be affected by the presence of shocks possibly caused by an outflow or from an enhanced ionization parameter as compared with H II regions in normal, local star-forming galaxies. We find that the Mass-Excitation (MEx) diagnostic, which separates purely star-forming and AGN hosting local galaxies in the [O III]/Hβ versus stellar mass plane, does not properly separate z ~ 2 galaxies classified according to the BPT diagram. However, if we shift the galaxies based on the offset between the local and z ~ 2 mass-metallicity relation (i.e., to the mass they would have at z ~ 0 with the same metallicity), we find better agreement between the MEx and BPT diagnostics. Finally, we find that metallicity calibrations based on [N II]/Hα are more biased by shocks and AGNs at high-z than the [O III]/Hβ/[N II]/Hα calibration.
• Cooper, M. C., Yan, R., Dickinson, M., Juneau, S., Lotz, J. M., Newman, J. A., Papovich, C., Salim, S., Walth, G., Weiner, B. J., & Willmer, C. N. (2013). Arizona CDFS Environment Survey, ACES (Cooper+, 2012). VizieR Online Data Catalog, 742, 52116.
• Dahlen, T., Mobasher, B., Faber, S. M., Ferguson, H. C., Barro, G., Finkelstein, S. L., Finlator, K., Fontana, A., Gruetzbauch, R., Johnson, S., Pforr, J., Salvato, M., Wiklind, T., Wuyts, S., Acquaviva, V., Dickinson, M. E., Guo, Y., Huang, J., Huang, K. H., , Newman, J. A., et al. (2013). A critical assessment of photometric redshift methods: A candels investigation. Astrophysical Journal, 775(Issue 2). doi:10.1088/0004-637x/775/2/93
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  We present results from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) photometric redshift methods investigation. In this investigation, the results from 11 participants, each using a different combination of photometric redshift code, template spectral energy distributions (SEDs), and priors, are used to examine the properties of photometric redshifts applied to deep fields with broadband multi-wavelength coverage. The photometry used includes U-band through mid-infrared filters and was derived using the TFIT method. Comparing the results, we find that there is no particular code or set of template SEDs that results in significantly better photometric redshifts compared to others. However, we find that codes producing the lowest scatter and outlier fraction utilize a training sample to optimize photometric redshifts by adding zero-point offsets, template adjusting, or adding extra smoothing errors. These results therefore stress the importance of the training procedure. We find a strong dependence of the photometric redshift accuracy on the signal-to-noise ratio of the photometry. On the other hand, we find a weak dependence of the photometric redshift scatter with redshift and galaxy color. We find that most photometric redshift codes quote redshift errors (e.g., 68% confidence intervals) that are too small compared to that expected from the spectroscopic control sample. We find that all codes show a statistically significant bias in the photometric redshifts. However, the bias is in all cases smaller than the scatter; the latter therefore dominates the errors. Finally, we find that combining results from multiple codes significantly decreases the photometric redshift scatter and outlier fraction. We discuss different ways of combining data to produce accurate photometric redshifts and error estimates. © 2013. The American Astronomical Society. All rights reserved..
• Dahlen, T., Mobasher, B., Faber, S. M., Ferguson, H. C., Barro, G., Finkelstein, S. L., Finlator, K., Fontana, A., Gruetzbauch, R., Johnson, S., Pforr, J., Salvato, M., Wiklind, T., Wuyts, S., Acquaviva, V., Dickinson, M. E., Guo, Y., Huang, J., Huang, K., , Newman, J. A., et al. (2013). A CRITICAL ASSESSMENT OF PHOTOMETRIC REDSHIFT METHODS: A CANDELS INVESTIGATION. ASTROPHYSICAL JOURNAL, 775(2).
• Dahlen, T., Mobasher, B., Faber, S. M., Ferguson, H. C., Barro, G., Finkelstein, S. L., Finlator, K., Fontana, A., Gruetzbauch, R., Johnson, S., Pforr, J., Salvato, M., Wiklind, T., Wuyts, S., Acquaviva, V., Dickinson, M. E., Guo, Y., Huang, J., Huang, K., , Newman, J. A., et al. (2013). A Critical Assessment of Photometric Redshift Methods: A CANDELS Investigation. apj, 775, 93.
• Dawson, K. S., Schlegel, D. J., Ahn, C. P., Anderson, S. F., Aubourg, '., Bailey, S., Barkhouser, R. H., Bautista, J. E., Beifiori, A., Berlind, A. A., Bhardwaj, V., Bizyaev, D., Blake, C. H., Blanton, M. R., Blomqvist, M., Bolton, A. S., Borde, A., Bovy, J., Brandt, W. N., , Brewington, H., et al. (2013). The Baryon Oscillation Spectroscopic Survey of SDSS-III. aj, 145, 10.
• Dawson, K. S., Schlegel, D. J., Ahn, C. P., Anderson, S. F., Aubourg, E., Bailey, S., Barkhouser, R. H., Bautista, J. E., Beifiori, A., Berlind, A. A., Bhardwaj, V., Bizyaev, D., Blake, C. H., Blanton, M. R., Blomqvist, M., Bolton, A. S., Borde, A., Bovy, J. o., Brandt, W. N., , Brewington, H., et al. (2013). THE BARYON OSCILLATION SPECTROSCOPIC SURVEY OF SDSS-III. ASTRONOMICAL JOURNAL, 145(1).
• Finkelstein, S. L., Papovich, C., Dickinson, M., Song, M., Tilvi, V., Koekemoer, A. M., Finkelstein, K. D., Mobasher, B., Ferguson, H. C., Giavalisco, M., Reddy, N., Ashby, M. L., Dekel, A., Fazio, G. G., Fontana, A., Grogin, N. A., Huang, J., Kocevski, D., Rafelski, M., , Weiner, B. J., et al. (2013). A galaxy rapidly forming stars 700 million years after the Big Bang at redshift 7.51. nat, 502, 524-527.
• Finkelstein, S. L., Papovich, C., Dickinson, M., Song, M., Tilvi, V., Koekemoer, A. M., Finkelstein, K. D., Mobasher, B., Ferguson, H. C., Giavalisco, M., Reddy, N., Ashby, M., Dekel, A., Fazio, G. G., Fontana, A., Grogin, N. A., Huang, J. -., Kocevski, D., Rafelski, M., , Weiner, B. J., et al. (2013). A galaxy rapidly forming stars 700 million years after the Big Bang at redshift 7.51. NATURE, 502(7472), 524-527.
• Freundlich, J., Combes, F., Tacconi, L. J., Cooper, M. C., Genzel, R., Neri, R., Bolatto, A., Bournaud, F., Burkert, A., Cox, P., Davis, M., Schreiber, N. M., Garcia-Burillo, S., Gracia-Carpio, J., Lutz, D., Naab, T., Newman, S., Sternberg, A., & Weiner, B. (2013). Towards a resolved Kennicutt-Schmidt law at high redshift. aap, 553, A130.
• Galametz, A., Grazian, A., Fontana, A., Ferguson, H. C., Ashby, M. L., Barro, G., Castellano, M., Dahlen, T., Donley, J. L., Faber, S. M., Grogin, N., Guo, Y., Huang, K., Kocevski, D. D., Koekemoer, A. M., Lee, K., McGrath, E. J., Peth, M., Willner, S. P., , Almaini, O., et al. (2013). CANDELS Multiwavelength Catalogs: Source Identification and Photometry in the CANDELS UKIDSS Ultra-deep Survey Field. apjs, 206, 10.
• Galametz, A., Grazian, A., Fontana, A., Ferguson, H. C., Ashby, M., Barro, G., Castellano, M., Dahlen, T., Donley, J. L., Faber, S. M., Grogin, N., Guo, Y., Huang, K., Kocevski, D. D., Koekemoer, A. M., Lee, K., McGrath, E. J., Peth, M., Willner, S. P., , Almaini, O., et al. (2013). CANDELS MULTIWAVELENGTH CATALOGS: SOURCE IDENTIFICATION AND PHOTOMETRY IN THE CANDELS UKIDSS ULTRA-DEEP SURVEY FIELD. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 206(2).
• Genzel, R., Tacconi, L. J., Kurk, J., Wuyts, S., Combes, F., Freundlich, J., Bolatto, A., Cooper, M. C., Neri, R., Nordon, R., Bournaud, F., Burkert, A., Comerford, J., Cox, P., Davis, M., Förster Schreiber, N. M., García-Burillo, S., Gracia-Carpio, J., Lutz, D., , Naab, T., et al. (2013). PHIBSS: MOLECULAR GAS, EXTINCTION, STAR FORMATION, AND KINEMATICS IN THE z = 1.5 STAR-FORMING GALAXY EGS13011166*. The Astrophysical Journal, 773(1), 68-68. doi:10.1088/0004-637x/773/1/68
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  We report matched resolution imaging spectroscopy of the CO 3-2 line (with the IRAM Plateau de Bure millimeter interferometer) and of the Hα line (with LUCI at the Large Binocular Telescope) in the massive z = 1.53 main-sequence galaxy EGS 13011166, as part of the Plateau de Bure high-z, blue-sequence survey (PHIBSS: Tacconi et al.). We combine these data with Hubble Space Telescope V-I-J-H-band maps to derive spatially resolved distributions of stellar surface density, star formation rate, molecular gas surface density, optical extinction, and gas kinematics. The spatial distribution and kinematics of the ionized and molecular gas are remarkably similar and are well modeled by a turbulent, globally Toomre unstable, rotating disk. The stellar surface density distribution is smoother than the clumpy rest-frame UV/optical light distribution and peaks in an obscured, star-forming massive bulge near the dynamical center. The molecular gas surface density and the effective optical screen extinction track each other and are well modeled by a mixed extinction model. The inferred slope of the spatially resolved molecular gas to star formation rate relation, N = dlogΣstar form/dlogΣmol gas, depends strongly on the adopted extinction model, and can vary from 0.8 to 1.7. For the preferred mixed dust-gas model, we find N = 1.14 ± 0.1.
• Genzel, R., Tacconi, L. J., Kurk, J., Wuyts, S., Combes, F., Freundlich, J., Bolatto, A., Cooper, M. C., Neri, R., Nordon, R., Bournaud, F., Burkert, A., Comerford, J., Cox, P., Davis, M., Schreiber, N. M., Garc ' ia-Burillo, S., Gracia-Carpio, J., Lutz, D., , Naab, T., et al. (2013). Phibss: Molecular Gas, Extinction, Star Formation, and Kinematics in the z = 1.5 Star- forming Galaxy EGS13011166. apj, 773, 68.
• Huang, J., Faber, S. M., Willmer, C. N., Rigopoulou, D., Koo, D., Newman, J., Shu, C., Ashby, M. L., Barmby, P., Coil, A., Luo, Z., Magdis, G., Wang, T., Weiner, B., Willner, S. P., Zheng, X. Z., & Fazio, G. G. (2013). Multi-Wavelength Study of a Complete IRAC 3.6 $ mu$m Selected Galaxy Sample: A Fair Census of Red and Blue Populations at Redshifts 0.4-1.2. apj, 766, 21.
• Jones, D. O., Rodney, S. A., Riess, A. G., Mobasher, B., Dahlen, T., McCully, C., Frederiksen, T. F., Casertano, S., Hjorth, J., Keeton, C. R., Koekemoer, A., Strolger, L., Wiklind, T. G., Challis, P., Graur, O. r., Hayden, B., Patel, B., Weiner, B. J., Filippenko, A. V., , Garnavich, P., et al. (2013). THE DISCOVERY OF THE MOST DISTANT KNOWN TYPE Ia SUPERNOVA AT REDSHIFT 1.914. ASTROPHYSICAL JOURNAL, 768(2).
• Jones, D. O., Rodney, S. A., Riess, A. G., Mobasher, B., Dahlen, T., McCully, C., Frederiksen, T. F., Casertano, S., Hjorth, J., Keeton, C. R., Koekemoer, A., Strolger, L., Wiklind, T. G., Challis, P., Graur, O., Hayden, B., Patel, B., Weiner, B. J., Filippenko, A. V., , Garnavich, P., et al. (2013). The Discovery of the Most Distant Known Type Ia Supernova at Redshift 1.914. apj, 768, 166.
• Juneau, S., Dickinson, M., Bournaud, F., Alexander, D. M., Daddi, E., Mullaney, J. R., Magnelli, B., Kartaltepe, J. S., Hwang, H. S., Willner, S. P., Coil, A. L., Rosario, D. J., Trump, J. R., Weiner, B. J., Willmer, C. N., Cooper, M. C., Elbaz, D., Faber, S. M., Frayer, D. T., , Kocevski, D. D., et al. (2013). Widespread and Hidden Active Galactic Nuclei in Star-forming Galaxies at Redshift gt 0.3. apj, 764, 176.
• Juneau, S., Dickinson, M., Bournaud, F., Alexander, D. M., Daddi, E., Mullaney, J. R., Magnelli, B., Kartaltepe, J. S., Hwang, H. S., Willner, S. P., Coil, A. L., Rosario, D. J., Trump, J. R., Weiner, B. J., Willmer, C., Cooper, M. C., Elbaz, D., Faber, S. M., Frayer, D. T., , Kocevski, D. D., et al. (2013). WIDESPREAD AND HIDDEN ACTIVE GALACTIC NUCLEI IN STAR-FORMING GALAXIES AT REDSHIFT > 0.3. ASTROPHYSICAL JOURNAL, 764(2).
• Kornei, K. A., Shapley, A. E., Martin, C. L., Coil, A. L., Lotz, J. M., & Weiner, B. J. (2013). FINE-STRUCTURE Fe II* EMISSION AND RESONANT Mg II EMISSION IN z similar to 1 STAR-FORMING GALAXIES. ASTROPHYSICAL JOURNAL, 774(1).
• Kornei, K. A., Shapley, A. E., Martin, C. L., Coil, A. L., Lotz, J. M., & Weiner, B. J. (2013). Fine-structure Fe II* Emission and Resonant Mg II Emission in z ~ 1 Star-forming Galaxies. apj, 774, 50.
• Kornei, K. A., Shapley, A. E., Martin, C. L., Coil, A. L., Lotz, J. M., & Weiner, B. J. (2013). Phibss: Molecular gas content and scaling relations in z ∼ 1-3 massive, main-sequence star-forming galaxies. Astrophysical Journal, 768(Issue 1). doi:10.1088/0004-637x/768/1/74
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  We present PHIBSS, the IRAM Plateau de Bure high-z blue sequence CO 3-2 survey of the molecular gas properties in massive, main-sequence star-forming galaxies (SFGs) near the cosmic star formation peak. PHIBSS provides 52 CO detections in two redshift slices at z ∼ 1.2 and 2.2, with log(M * (M⊙)) ≥ 10.4 and log(SFR(M ⊙/yr)) ≥ 1.5. Including a correction for the incomplete coverage of the M* -SFR plane, and adopting a "Galactic" value for the CO-H2 conversion factor, we infer average gas fractions of ∼0.33 at z ∼ 1.2 and ∼0.47 at z ∼ 2.2. Gas fractions drop with stellar mass, in agreement with cosmological simulations including strong star formation feedback. Most of the z ∼ 1-3 SFGs are rotationally supported turbulent disks. The sizes of CO and UV/optical emission are comparable. The molecular-gas-star-formation relation for the z = 1-3 SFGs is near-linear, with a ∼0.7 Gyr gas depletion timescale; changes in depletion time are only a secondary effect. Since this timescale is much less than the Hubble time in all SFGs between z ∼ 0 and 2, fresh gas must be supplied with a fairly high duty cycle over several billion years. At given z and M *, gas fractions correlate strongly with the specific star formation rate (sSFR). The variation of sSFR between z ∼ 0 and 3 is mainly controlled by the fraction of baryonic mass that resides in cold gas. © 2013. The American Astronomical Society. All rights reserved.
• Maseda, M. V., Wel, A., Cunha, E., Rix, H., Pacifici, C., Momcheva, I., Brammer, G. B., Franx, M., Dokkum, P., Bell, E. F., Fumagalli, M., Grogin, N. A., Kocevski, D. D., Koekemoer, A. M., Lundgren, B. F., Marchesini, D., Nelson, E. J., Patel, S. G., Skelton, R. E., , Straughn, A. N., et al. (2013). Confirmation of Small Dynamical and Stellar Masses for Extreme Emission Line Galaxies at z ~ 2. apjl, 778, L22.
• Maseda, M. V., van, d., da, C. E., Rix, H., Pacifici, C., Momcheva, I., Brammer, G. B., Franx, M., van, D. P., Bell, E. F., Fumagalli, M., Grogin, N. A., Kocevski, D. D., Koekemoer, A. M., Lundgren, B. F., Marchesini, D., Nelson, E. J., Patel, S. G., Skelton, R. E., , Straughn, A. N., et al. (2013). CONFIRMATION OF SMALL DYNAMICAL AND STELLAR MASSES FOR EXTREME EMISSION LINE GALAXIES AT z similar to 2. ASTROPHYSICAL JOURNAL LETTERS, 778(1).
• Mostek, N., Coil, A. L., Cooper, M., Davis, M., Newman, J. A., & Weiner, B. J. (2013). Mid-infrared determination of total infrared luminosity and star formation rates of local and high-redshift galaxies. Astrophysical Journal, 767(Issue 1). doi:10.1088/0004-637x/767/1/73
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  We demonstrate estimating the total infrared luminosity, L(TIR), and star formation rates (SFRs) of star-forming galaxies at redshift 0 < z < 2.8 from single-band 24 μm observations, using local spectral energy distribution (SED) templates without introducing additional free parameters. Our method is based on characterizing the SEDs of galaxies as a function of their L(TIR) surface density, which is motivated by the indications that the majority of IR luminous star-forming galaxies at 1 < z < 3 have extended star-forming regions, in contrast to the strongly nuclear concentrated, merger-induced starbursts in local luminous and ultraluminous IR galaxies. We validate our procedure for estimating L(TIR) by comparing the resulting L(TIR) with those measured from far-IR observations, such as those from Herschel in the Extended Chandra Deep Field South (ECDFS) and Hubble Deep Field North (HDFN), as well as L(TIR) measured from stacked far-IR observations at redshift 0 < z < 2.8. Active galactic nuclei were excluded using X-ray and 3.6-8.0 μm observations, which are generally available in deep cosmological survey fields. The Gaussian fits to the distribution of the discrepancies between the L(TIR) measurements from single-band 24 μm and Herschel observations in the ECDFS and HDFN samples have σ < 0.1 dex, with ∼10% of objects disagreeing by more than 0.2 dex. Since the 24 μm estimates are based on SEDs for extended galaxies, this agreement suggests that ∼90% of IR galaxies at high z are indeed much more physically extended than local counterparts of similar L(TIR), consistent with recent independent studies of the fractions of galaxies forming stars in the main-sequence and starburst modes, respectively. Because we have not introduced empirical corrections to enhance these estimates, in principle, our method should be applicable to lower luminosity galaxies. This will enable use of the 21 μm band of the Mid-Infrared Instrument on board the James Webb Space Telescope to provide an extremely sensitive tracer of obscured SFR in individual star-forming galaxies across the peak of the cosmic star formation history. © 2013. The American Astronomical Society. All rights reserved..
• Mostek, N., Coil, A. L., Cooper, M., Davis, M., Newman, J. A., & Weiner, B. J. (2013). THE DEEP2 GALAXY REDSHIFT SURVEY: CLUSTERING DEPENDENCE ON GALAXY STELLAR MASS AND STAR FORMATION RATE AT z similar to 1. ASTROPHYSICAL JOURNAL, 767(1).
• Mostek, N., Coil, A. L., Cooper, M., Davis, M., Newman, J. A., & Weiner, B. J. (2013). The DEEP2 Galaxy Redshift Survey: Clustering Dependence on Galaxy Stellar Mass and Star Formation Rate at z ~ 1. apj, 767, 89.
• Newman, J. A., Cooper, M. C., Davis, M., Faber, S. M., Coil, A. L., Guhathakurta, P., Koo, D. C., Phillips, A. C., Conroy, C., Dutton, A. A., Finkbeiner, D. P., Gerke, B. F., Rosario, D. J., Weiner, B. J., Willmer, C. N., Yan, R., Harker, J. J., Kassin, S. A., Konidaris, N. P., , Lai, K., et al. (2013). The DEEP2 Galaxy Redshift Survey: Design, Observations, Data Reduction, and Redshifts. apjs, 208, 5.
• Newman, J. A., Cooper, M. C., Davis, M., Faber, S. M., Coil, A. L., Guhathakurta, P., Koo, D. C., Phillips, A. C., Conroy, C., Dutton, A. A., Finkbeiner, D. P., Gerke, B. F., Rosario, D. J., Weiner, B. J., Willmer, C. N., Yan, R., Harker, J. J., Kassin, S. A., Konidaris, N. P., , Lai, K., et al. (2013). The deep2 galaxy redshift survey: Design, observations, data reduction, and redshifts. Astrophysical Journal, Supplement Series, 208(Issue 1). doi:10.1088/0067-0049/208/1/5
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  We describe the design and data analysis of the DEEP2 Galaxy Redshift Survey, the densest and largest high-precision redshift survey of galaxies at z ∼ 1 completed to date. The survey was designed to conduct a comprehensive census of massive galaxies, their properties, environments, and large-scale structure down to absolute magnitude MB = -20 at z ∼ 1 via ∼90 nights of observation on the Keck telescope. The survey covers an area of 2.8 deg2 divided into four separate fields observed to a limiting apparent magnitude of RAB = 24.1. Objects with z ≲ 0.7 are readily identifiable using BRI photometry and rejected in three of the four DEEP2 fields, allowing galaxies with z > 0.7 to be targeted ∼2.5 times more efficiently than in a purely magnitude-limited sample. Approximately 60% of eligible targets are chosen for spectroscopy, yielding nearly 53,000 spectra and more than 38,000 reliable redshift measurements. Most of the targets that fail to yield secure redshifts are blue objects that lie beyond z ∼ 1.45, where the [O II] 3727 Å doublet lies in the infrared. The DEIMOS 1200 line mm-1 grating used for the survey delivers high spectral resolution (R ∼ 6000), accurate and secure redshifts, and unique internal kinematic information. Extensive ancillary data are available in the DEEP2 fields, particularly in the Extended Groth Strip, which has evolved into one of the richest multiwavelength regions on the sky. This paper is intended as a handbook for users of the DEEP2 Data Release 4, which includes all DEEP2 spectra and redshifts, as well as for the DEEP2 DEIMOS data reduction pipelines. Extensive details are provided on object selection, mask design, biases in target selection and redshift measurements, the spec2d two-dimensional data-reduction pipeline, the spec1d automated redshift pipeline, and the zspec visual redshift verification process, along with examples of instrumental signatures or other artifacts that in some cases remain after data reduction. Redshift errors and catastrophic failure rates are assessed through more than 2000 objects with duplicate observations. Sky subtraction is essentially photon-limited even under bright OH sky lines; we describe the strategies that permitted this, based on high image stability, accurate wavelength solutions, and powerful B-spline modeling methods. We also investigate the impact of targets that appear to be single objects in ground-based targeting imaging but prove to be composite in Hubble Space Telescope data; they constitute several percent of targets at z ∼ 1, approaching ∼5%-10% at z > 1.5. Summary data are given that demonstrate the superiority of DEEP2 over other deep high-precision redshift surveys at z ∼ 1 in terms of redshift accuracy, sample number density, and amount of spectral information. We also provide an overview of the scientific highlights of the DEEP2 survey thus far. © 2013. The American Astronomical Society. All rights reserved.
• Newman, J. A., Cooper, M. C., Davis, M., Faber, S. M., Coil, A. L., Guhathakurta, P., Koo, D. C., Phillips, A. C., Conroy, C., Dutton, A. A., Finkbeiner, D. P., Gerke, B. F., Rosario, D. J., Weiner, B. J., Willmer, C., Yan, R., Harker, J. J., Kassin, S. A., Konidaris, N. P., , Lai, K., et al. (2013). THE DEEP2 GALAXY REDSHIFT SURVEY: DESIGN, OBSERVATIONS, DATA REDUCTION, AND REDSHIFTS. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 208(1).
• Pacifici, C., Kassin, S. A., Weiner, B., Charlot, S., & Gardner, J. P. (2013). THE RISE AND FALL OF THE STAR FORMATION HISTORIES OF BLUE GALAXIES AT REDSHIFTS 0.2 < z < 1.4. ASTROPHYSICAL JOURNAL LETTERS, 762(1).
• Pacifici, C., Kassin, S. A., Weiner, B., Charlot, S., & Gardner, J. P. (2013). The Rise and Fall of the Star Formation Histories of Blue Galaxies at Redshifts 0.2 lt z lt 1.4. apjl, 762, L15.
• Pacifici, C., Kassin, S. A., Weiner, B., Charlot, S., & Gardner, J. P. (2013). The rise and fall of the star formation histories of blue galaxies at redshifts 0.2
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  Popular cosmological scenarios predict that galaxies form hierarchically fromthe merger of many progenitors, each with their own unique star formationhistory (SFH). We use a sophisticated approach to constrain the SFHs of 4517blue (presumably star-forming) galaxies with spectroscopic redshifts in therange 0.2 < z < 1.4 from the All-Wavelength Extended Groth Strip InternationalSurvey (AEGIS). This consists in the Bayesian analysis of the observed galaxyspectral energy distributions with a comprehensive library of synthetic spectraassembled using realistic, hierarchical star formation and chemical enrichmenthistories from cosmological simulations. We constrain the SFH of each galaxy inour sample by comparing the observed fluxes in the B, R, I and Ks bands andrest-frame optical emission-line luminosities with those of one million modelspectral energy distributions. We explore the dependence of the resulting SFHson galaxy stellar mass and redshift. We find that the average SFHs of high-massgalaxies rise and fall in a roughly symmetric bell-shaped manner, while thoseof low-mass galaxies rise progressively in time, consistent with the typicallystronger activity of star formation in low-mass compared to high-mass galaxies.For galaxies of all masses, the star formation activity rises more rapidly athigh than at low redshift. These findings imply that the standard approximationof exponentially declining SFHs widely used to interpret observed galaxyspectral energy distributions may not be appropriate to constrain the physicalparameters of star-forming galaxies at intermediate redshifts.[Journal_ref: ]
• Palamara, D. P., Brown, M. J., Jannuzi, B. T., Dey, A., Stern, D., Pimbblet, K. A., Weiner, B. J., Ashby, M. L., Kochanek, C. S., Gonzalez, A., Brodwin, M., Le Floc'h, E., & Rieke, M. (2013). The Clustering of Extremely Red Objects. apj, 764, 31.
• Palamara, D. P., Brown, M., Jannuzi, B. T., Dey, A., Stern, D., Pimbblet, K. A., Weiner, B. J., Ashby, M., Kochanek, C. S., Gonzalez, A., Brodwin, M., Le, F. E., & Rieke, M. (2013). THE CLUSTERING OF EXTREMELY RED OBJECTS. ASTROPHYSICAL JOURNAL, 764(1).
• Rujopakarn, W., Rieke, G. H., Weiner, B. J., 'alez, P., Rex, M., Walth, G. L., & Kartaltepe, J. S. (2013). Mid-infrared Determination of Total Infrared Luminosity and Star Formation Rates of Local and High-redshift Galaxies. apj, 767, 73.
• Shim, H., Im, M., Ko, J., Jeon, Y., Karouzos, M., Kim, S. J., Lee, H. M., Papovich, C., Willmer, C., & Weiner, B. J. (2013). HECTOSPEC AND HYDRA SPECTRA OF INFRARED LUMINOUS SOURCES IN THE AKARI NORTH ECLIPTIC POLE SURVEY FIELD. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 207(2).
• Shim, H., Im, M., Ko, J., Jeon, Y., Karouzos, M., Kim, S. J., Lee, H. M., Papovich, C., Willmer, C., & Weiner, B. J. (2013). Hectospec and Hydra Spectra of Infrared Luminous Sources in the AKARI North Ecliptic Pole Survey Field. apjs, 207, 37.
• Shim, H., Im, M., Ko, J., Jeon, Y., Karouzos, M., Kim, S. J., Lee, H. M., Papovich, C., Willmer, C., & Weiner, B. J. (2013). Hectospec and hydra spectra of infrared luminous sources in the akari north ecliptic pole survey field. Astrophysical Journal, Supplement Series, 207(Issue 2). doi:10.1088/0067-0049/207/2/37
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  We present spectra of 1796 sources selected in the AKARI North Ecliptic Pole Wide Survey field, obtained with MMT/Hectospec and WIYN/Hydra, for which we measure 1645 redshifts. We complemented the generic flux-limited spectroscopic surveys at 11 μm and 15 μm, with additional sources selected based on the MIR and optical colors. In MMT/Hectospec observations, the redshift identification rates are ∼80% for objects with R < 21.5 mag. On the other hand, in WIYN/Hydra observations, the redshift identification rates are ∼80% at R magnitudes brighter than 19 mag. The observed spectra were classified through the visual inspection or from the line diagnostics. We identified 1128 star-forming or absorption-line-dominated galaxies, 198 Type-1 active galactic nuclei (AGNs), 8 Type-2 AGNs, 121 Galactic stars, and 190 spectra in unknown category due to low signal-to-noise ratio. The spectra were flux-calibrated but to an accuracy of 0.1-0.18 dex for most of the targets and worse for the remainder. We derive star formation rates (SFRs) from the mid-infrared fluxes or from the optical emission lines, showing that our sample spans an SFR range of 0.1 to a few hundred M yr-1. We find that the extinction inferred from the difference between the IR and optical SFR increases as the IR luminosity increases but with a large scatter. © 2013. The American Astronomical Society. All rights reserved.
• Shipley, H. V., Papovich, C., Rieke, G. H., Dey, A., Jannuzi, B. T., Moustakas, J., & Weiner, B. (2013). SPITZER SPECTROSCOPY OF INFRARED-LUMINOUS GALAXIES: DIAGNOSTICS OF ACTIVE GALACTIC NUCLEI AND STAR FORMATION AND CONTRIBUTION TO TOTAL INFRARED LUMINOSITY. ASTROPHYSICAL JOURNAL, 769(1).
• Shipley, H. V., Papovich, C., Rieke, G. H., Dey, A., Jannuzi, B. T., Moustakas, J., & Weiner, B. (2013). Spitzer Spectroscopy of Infrared-luminous Galaxies: Diagnostics of Active Galactic Nuclei and Star Formation and Contribution to Total Infrared Luminosity. apj, 769, 75.
• Tacconi, L. J., Neri, R., Genzel, R., Combes, F., Bolatto, A., Cooper, M. C., Wuyts, S., Bournaud, F., Burkert, A., Comerford, J., Cox, P., Davis, M., Schreiber, N. M., Garc ' ia-Burillo, S., Gracia-Carpio, J., Lutz, D., Naab, T., Newman, S., Omont, A., , Saintonge, A., et al. (2013). Phibss: Molecular Gas Content and Scaling Relations in z ~ 1-3 Massive, Main-sequence Star-forming Galaxies. apj, 768, 74.
• Tacconi, L. J., Neri, R., Genzel, R., Combes, F., Bolatto, A., Cooper, M. C., Wuyts, S., Bournaud, F., Burkert, A., Comerford, J., Cox, P., Davis, M., Schreiber, N., Garcia-Burillo, S., Gracia-Carpio, J., Lutz, D., Naab, T., Newman, S., Omont, A., , Saintonge, A., et al. (2013). PHIBSS: MOLECULAR GAS CONTENT AND SCALING RELATIONS IN z similar to 1-3 MASSIVE, MAIN-SEQUENCE STAR-FORMING GALAXIES. ASTROPHYSICAL JOURNAL, 768(1).
• Trump, J. R., Konidaris, N. P., Barro, G., Koo, D. C., Kocevski, D. D., Juneau, S., Weiner, B. J., Faber, S. M., McLean, I. S., Yan, R., 'alez, P. G., & Villar, V. (2013). Testing Diagnostics of Nuclear Activity and Star Formation in Galaxies at z gt 1. apjl, 763, L6.
• Trump, J. R., Konidaris, N. P., Barro, G., Koo, D. C., Kocevski, D. D., Juneau, S., Weiner, B. J., Faber, S. M., McLean, I. S., Yan, R., Perez-Gonzalez, P. G., & Villar, V. (2013). TESTING DIAGNOSTICS OF NUCLEAR ACTIVITY AND STAR FORMATION IN GALAXIES AT z > 1. ASTROPHYSICAL JOURNAL LETTERS, 763(1).
• Woo, J., Dekel, A., Faber, S. M., Noeske, K., Koo, D. C., Gerke, B. F., Cooper, M. C., Salim, S., Dutton, A. A., Newman, J., Weiner, B. J., Bundy, K., Willmer, C. N., Davis, M., & Yan, R. (2013). Dependence of galaxy quenching on halo mass and distance from its centre. mnras, 428, 3306-3326.
• Woo, J., Dekel, A., Faber, S. M., Noeske, K., Koo, D. C., Gerke, B. F., Cooper, M. C., Salim, S., Dutton, A. A., Newman, J., Weiner, B. J., Bundy, K., Willmer, C., Davis, M., & Yan, R. (2013). Dependence of galaxy quenching on halo mass and distance from its centre. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 428(4), 3306-3326.
• Ahn, C. P., Alexandroff, R., Allende Prieto, C., Anderson, S. F., Anderton, T., Andrews, B. H., Aubourg, '., Bailey, S., Balbinot, E., Barnes, R., & al., e. (2012). The Ninth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-III Baryon Oscillation Spectroscopic Survey. apjs, 203, 21.
• Ahn, C. P., Alexandroff, R., Allende Prieto, C., Anderson, S. F., Anderton, T., Andrews, B. H., Aubourg, É., Bailey, S., Balbinot, E., Barnes, R., Bautista, J., Beers, T. C., Beifiori, A., Berlind, A. A., Bhardwaj, V., Bizyaev, D., Blake, C. H., Blanton, M. R., Blomqvist, M., , Bochanski, J. J., et al. (2012). The ninth data release of the sloan digital sky survey: First spectroscopic data from the sdss-iii baryon oscillation spectroscopic survey. Astrophysical Journal, Supplement Series, 203(Issue 2). doi:10.1088/0067-0049/203/2/21
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  The Sloan Digital Sky Survey III (SDSS-III) presents the first spectroscopic data from the Baryon Oscillation Spectroscopic Survey (BOSS). This ninth data release (DR9) of the SDSS project includes 535,995 new galaxy spectra (median z 0.52), 102,100 new quasar spectra (median z 2.32), and 90,897 new stellar spectra, along with the data presented in previous data releases. These spectra were obtained with the new BOSS spectrograph and were taken between 2009 December and 2011 July. In addition, the stellar parameters pipeline, which determines radial velocities, surface temperatures, surface gravities, and metallicities of stars, has been updated and refined with improvements in temperature estimates for stars with T eff < 5000 K and in metallicity estimates for stars with [Fe/H] > -0.5. DR9 includes new stellar parameters for all stars presented in DR8, including stars from SDSS-I and II, as well as those observed as part of the SEGUE-2. The astrometry error introduced in the DR8 imaging catalogs has been corrected in the DR9 data products. The next data release for SDSS-III will be in Summer 2013, which will present the first data from the APOGEE along with another year of data from BOSS, followed by the final SDSS-III data release in 2014 December. © 2012. The American Astronomical Society. All rights reserved..
• Ahn, C. P., Alexandroff, R., Prieto, C. A., Anderson, S. F., Anderton, T., Andrews, B. H., Aubourg, E., Bailey, S., Balbinot, E., Barnes, R., Bautista, J., Beers, T. C., Beifiori, A., Berlind, A. A., Bhardwaj, V., Bizyaev, D., Blake, C. H., Blanton, M. R., Blomqvist, M., , Bochanski, J. J., et al. (2012). THE NINTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST SPECTROSCOPIC DATA FROM THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 203(2).
• Cheung, E., Faber, S. M., Koo, D. C., Dutton, A. A., Simard, L., McGrath, E. J., Huang, J. -., Bell, E. F., Dekel, A., Fang, J. J., Salim, S., Barro, G., Bundy, K., Coil, A. L., Cooper, M. C., Conselice, C. J., Davis, M., Dominguez, A., Kassin, S. A., , Kocevski, D. D., et al. (2012). THE DEPENDENCE OF QUENCHING UPON THE INNER STRUCTURE OF GALAXIES AT 0.5 <= z < 0.8 IN THE DEEP2/AEGIS SURVEY. ASTROPHYSICAL JOURNAL, 760(2).
• Cheung, E., Faber, S. M., Koo, D. C., Dutton, A. A., Simard, L., McGrath, E. J., Huang, J., Bell, E. F., Dekel, A., Fang, J. J., Salim, S., Barro, G., Bundy, K., Coil, A. L., Cooper, M. C., Conselice, C. J., Davis, M., Dom ' inguez, A., Kassin, S. A., , Kocevski, D. D., et al. (2012). The Dependence of Quenching upon the Inner Structure of Galaxies at 0.5 lt= z lt 0.8 in the DEEP2/AEGIS Survey. apj, 760, 131.
• Comerford, J. M., Gerke, B. F., Stern, D., Cooper, M. C., Weiner, B. J., Newman, J. A., Madsen, K., & Barrows, R. S. (2012). KILOPARSEC-SCALE SPATIAL OFFSETS IN DOUBLE-PEAKED NARROW-LINE ACTIVE GALACTIC NUCLEI. I. MARKERS FOR SELECTION OF COMPELLING DUAL ACTIVE GALACTIC NUCLEUS CANDIDATES. ASTROPHYSICAL JOURNAL, 753(1).
• Comerford, J. M., Gerke, B. F., Stern, D., Cooper, M. C., Weiner, B. J., Newman, J. A., Madsen, K., & Barrows, R. S. (2012). Kiloparsec-scale Spatial Offsets in Double-peaked Narrow-line Active Galactic Nuclei. I. Markers for Selection of Compelling Dual Active Galactic Nucleus Candidates. apj, 753, 42.
• Comerford, J. M., Gerke, B. F., Stern, D., Cooper, M. C., Weiner, B. J., Newman, J. A., Madsen, K., & Barrows, R. S. (2012). Kiloparsec-scale spatial offsets in double-peaked narrow-line active galactic nuclei. I. Markers for selection of compelling dual active galactic nucleus candidates. Astrophysical Journal, 753(Issue 1). doi:10.1088/0004-637x/753/1/42
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  Merger-remnant galaxies with kiloparsec (kpc) scale separation dual active galactic nuclei (AGNs) should be widespread as a consequence of galaxy mergers and triggered gas accretion onto supermassive black holes, yet very few dual AGNs have been observed. Galaxies with double-peaked narrow AGN emission lines in the Sloan Digital Sky Survey (SDSS) are plausible dual AGN candidates, but their double-peaked profiles could also be the result of gas kinematics or AGN-driven outflows and jets on small or large scales. To help distinguish between these scenarios, we have obtained spatial profiles of the AGN emission via follow-up long-slit spectroscopy of 81 double-peaked narrow-line AGNs in SDSS at 0.03 ≤ z ≤ 0.36 using Lick, Palomar, and MMT Observatories. We find that all 81 systems exhibit double AGN emission components with kpc projected spatial separations on the sky (0.2 h -1 70kpc
• Cooper, M. C., Griffith, R. L., Newman, J. A., Coil, A. L., Davis, M., Dutton, A. A., Faber, S. M., Guhathakurta, P., Koo, D. C., Lotz, J. M., Weiner, B. J., Willmer, C. N., & Yan, R. (2012). The DEEP3 Galaxy Redshift Survey: the impact of environment on the size evolution of massive early-type galaxies at intermediate redshift. mnras, 419, 3018-3027.
• Cooper, M. C., Griffith, R. L., Newman, J. A., Coil, A. L., Davis, M., Dutton, A. A., Faber, S. M., Guhathakurta, P., Koo, D. C., Lotz, J. M., Weiner, B. J., Willmer, C., & Yan, R. (2012). The DEEP3 Galaxy Redshift Survey: the impact of environment on the size evolution of massive early-type galaxies at intermediate redshift. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 419(4), 3018-3027.
• Cooper, M. C., Yan, R., Dickinson, M., Juneau, S., Lotz, J. M., Newman, J. A., Papovich, C., Salim, S., Walth, G., Weiner, B. J., & Willmer, C. (2012). The Arizona CDFS Environment Survey (ACES): A Magellan/IMACS Spectroscopic Survey of the Chandra Deep Field-South. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 425(3), 2116-2127.
• Cooper, M. C., Yan, R., Dickinson, M., Juneau, S., Lotz, J. M., Newman, J. A., Papovich, C., Salim, S., Walth, G., Weiner, B. J., & Willmer, C. N. (2012). The Arizona CDFS Environment Survey (ACES): A Magellan/IMACS Spectroscopic Survey of the Chandra Deep Field-South. mnras, 425, 2116-2127.
• Cooper, M. C., Yan, R., Dickinson, M., Juneau, S., Lotz, J. M., Newman, J. A., Papovich, C., Salim, S., Walth, G., Weiner, B. J., & Willmer, C. N. (2012). The Arizona CDFS Environment Survey (ACES): A Magellan/IMACS Spectroscopic Survey of the Chandra Deep Field-South: Arizona CDFS Environment Survey (ACES). Monthly Notices of the Royal Astronomical Society, 425(3), 2116-2127. doi:10.1111/j.1365-2966.2012.21524.x
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  We present the Arizona CDFS Environment Survey (ACES), a recently completed spectroscopic redshift survey of the Chandra Deep Field-South (CDFS) conducted using the Inamori-Magellan Areal Camera and Spectrograph on the Magellan-Baade telescope. In total, the survey targeted 7277 unique sources down to a limiting magnitude of RAB = 24.1, yielding 5080 secure redshifts across the ∼30arcmin × 30arcmin extended CDFS region. The ACES data set delivers a significant increase to both the spatial coverage and the sampling density of the spectroscopic observations in the field. Combined with previously published spectroscopic redshifts, ACES now creates a highly complete survey of the galaxy population at R < 23, enabling the local galaxy density (or environment) on relatively small scales (∼1Mpc) to be measured at z < 1 in one of the most heavily studied and data-rich fields in the sky. Here, we describe the motivation, design and implementation of the survey and present a preliminary redshift and environment catalogue. In addition, we utilize the ACES spectroscopic redshift catalogue to assess the quality of photometric redshifts from both the COMBO-17 and Multiwavelength Survey by Yale-Chile imaging surveys of the CDFS. © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS.
• Dickinson, M., Kartaltepe, J. S., Kashikawa, N., Mobasher, B., Nakajima, K., Nayyeri, H., Ono, Y., Ouchi, M., Penner, K., Shimasaku, K., Spinrad, H., Stern, D., & Weiner, B. J. (2012). Spectroscopic Confirmation of Three z-dropout Galaxies at z = 6.844-7.213: Demographics of Lyα Emission in z ~ 7 Galaxies. The Astrophysical Journal, 744(2), 83. doi:10.1088/0004-637x/744/2/83
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  We present the results of our ultra-deep Keck/DEIMOS spectroscopy of z-dropout galaxies in the Subaru Deep Field and Great Observatories Origins Deep Survey's northern field. For 3 out of 11 objects, we detect an emission line at ~1 ?m with a signal-to-noise ratio of ~10. The lines show asymmetric profiles with high weighted skewness values, consistent with being Ly?, yielding redshifts of z = 7.213, 6.965, and 6.844. Specifically, we confirm the z = 7.213 object in two independent DEIMOS runs with different spectroscopic configurations. The z = 6.965 object is a known Ly? emitter, IOK-1, for which our improved spectrum at a higher resolution yields a robust skewness measurement. The three z-dropouts have Ly? fluxes of 3 ? 10?17?erg?s?1?cm?2 and rest-frame equivalent widths EWLy? 0 = 33-43 ?. Based on the largest spectroscopic sample of 43 z-dropouts, which is the combination of our and previous data, we find that the fraction of Ly?-emitting galaxies (EWLy? 0 > 25 ?) is low at z ~ 7; 17% ? 10% and 24% ? 12% for bright (M UV ?21) and faint (M UV ?19.5) galaxies, respectively. The fractions of Ly?-emitting galaxies drop from z ~ 6 to 7 and the amplitude of the drop is larger for faint galaxies than for bright galaxies. These two pieces of evidence would indicate that the neutral hydrogen fraction of the intergalactic medium increases from z ~ 6 to 7 and that the reionization proceeds from high- to low-density environments, as suggested by an inside-out reionization model.
• Genzel, R., Tacconi, L. J., Combes, F., Bolatto, A., Neri, R., Sternberg, A., Cooper, M. C., Bouch 'e, N., Bournaud, F., Burkert, A., Comerford, J., Cox, P., Davis, M., Schreiber, N. M., Garcia-Burillo, S., Gracia-Carpio, J., Lutz, D., Naab, T., Newman, S., , Saintonge, A., et al. (2012). The Metallicity Dependence of the CO rarr H$_2$ Conversion Factor in z gt= 1 Star-forming Galaxies. apj, 746, 69.
• Genzel, R., Tacconi, L. J., Combes, F., Bolatto, A., Neri, R., Sternberg, A., Cooper, M. C., Bouche, N., Bournaud, F., Burkert, A., Comerford, J., Cox, P., Davis, M., Schreiber, N., Garcia-Burillo, S., Gracia-Carpio, J., Lutz, D., Naab, T., Newman, S., , Saintonge, A., et al. (2012). THE METALLICITY DEPENDENCE OF THE CO -> H-2 CONVERSION FACTOR IN z >= 1 STAR-FORMING GALAXIES. ASTROPHYSICAL JOURNAL, 746(1).
• Genzel, R., Tacconi, L. J., Combes, F., Bolatto, A., Neri, R., Sternberg, A., Cooper, M. C., Bouché, N., Bournaud, F., Burkert, A., Comerford, J., Cox, P., Davis, M., Schreiber, N. M., Garcia-Burillo, S., Gracia-Carpio, J., Lutz, D., Naab, T., Newman, S., , Saintonge, A., et al. (2012). The metallicity dependence of the CO → H2 conversion factor in z ≥ 1 star-forming galaxies. Astrophysical Journal, 746(Issue 1). doi:10.1088/0004-637x/746/1/69
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  We use the first systematic samples of CO millimeter emission in z ≥ 1 ''main-sequence'' star-forming galaxies to study the metallicity dependence of the conversion factor αCO, from CO line luminosity to molecular gas mass. The molecular gas depletion rate inferred from the ratio of the star formation rate (SFR) to CO luminosity, is 1Gyr-1 for near-solar metallicity galaxies with stellar masses above M S 1011 M. In this regime, the depletion rate does not vary more than a factor of two to three as a function of molecular gas surface density or redshift between z 0 and 2. Below M S the depletion rate increases rapidly with decreasing metallicity. We argue that this trend is not caused by starburst events, by changes in the physical parameters of the molecular clouds, or by the impact of the fundamental-metallicity-SFR-stellar mass relation. A more probable explanation is that the conversion factor is metallicity dependent and that star formation can occur in "CO-dark" gas. The trend is also expected theoretically from the effect of enhanced photodissociation of CO by ultraviolet radiation at low metallicity. From the available z 0 and z 1-3 samples we constrain the slope of the log(αCO)-log (metallicity) relation to range between -1 and -2, fairly insensitive to the assumed slope of the gas-SFR relation. Because of the lower metallicities near the peak of the galaxy formation activity at z 1-2 compared to z 0, we suggest that molecular gas masses estimated from CO luminosities have to be substantially corrected upward for galaxies below M S. © 2012. The American Astronomical Society. All rights reserved.
• Gerke, B. F., Newman, J. A., Davis, M., Coil, A. L., Cooper, M. C., Dutton, A. A., Faber, S. M., Guhathakurta, P., Konidaris, N., Koo, D. C., Lin, L., Noeske, K., Phillips, A. C., Rosario, D. J., Weiner, B. J., Willmer, C. N., & Yan, R. (2012). The DEEP2 Galaxy Redshift Survey: The Voronoi-Delaunay Method Catalog of Galaxy Groups. apj, 751, 50.
• Gerke, B. F., Newman, J. A., Davis, M., Coil, A. L., Cooper, M. C., Dutton, A. A., Faber, S. M., Guhathakurta, P., Konidaris, N., Koo, D. C., Lin, L., Noeske, K., Phillips, A. C., Rosario, D. J., Weiner, B. J., Willmer, C. N., & Yan, R. (2012). The deep2 galaxy redshift survey: The Voronoi-Delaunay method catalog of galaxy groups. Astrophysical Journal, 751(Issue 1). doi:10.1088/0004-637x/751/1/50
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  We present a public catalog of galaxy groups constructed from the spectroscopic sample of galaxies in the fourth data release from the Deep Extragalactic Evolutionary Probe 2 (DEEP2) Galaxy Redshift Survey, including the Extended Groth Strip (EGS). The catalog contains 1165 groups with two or more members in the EGS over the redshift range 0 < z < 1.5 and 1295 groups at z > 0.6 in the rest of DEEP2. Twenty-five percent of EGS galaxies and fourteen percent of high-z DEEP2 galaxies are assigned to galaxy groups. The groups were detected using the Voronoi-Delaunay method (VDM) after it has been optimized on mock DEEP2 catalogs following similar methods to those employed in Gerke et al. In the optimization effort, we have taken particular care to ensure that the mock catalogs resemble the data as closely as possible, and we have fine-tuned our methods separately on mocks constructed for the EGS and the rest of DEEP2. We have also probed the effect of the assumed cosmology on our inferred group-finding efficiency by performing our optimization on three different mock catalogs with different background cosmologies, finding large differences in the group-finding success we can achieve for these different mocks. Using the mock catalog whose background cosmology is most consistent with current data, we estimate that the DEEP2 group catalog is 72% complete and 61% pure (74% and 67% for the EGS) and that the group finder correctly classifies 70% of galaxies that truly belong to groups, with an additional 46% of interloper galaxies contaminating the catalog (66% and 43% for the EGS). We also confirm that the VDM catalog reconstructs the abundance of galaxy groups with velocity dispersions above 300kms-1 to an accuracy better than the sample variance, and this successful reconstruction is not strongly dependent on cosmology. This makes the DEEP2 group catalog a promising probe of the growth of cosmic structure that can potentially be used for cosmological tests. © 2012. The American Astronomical Society. All rights reserved.
• Gerke, B. F., Newman, J. A., Davis, M., Coil, A. L., Cooper, M. C., Dutton, A. A., Faber, S. M., Guhathakurta, P., Konidaris, N., Koo, D. C., Lin, L., Noeske, K., Phillips, A. C., Rosario, D. J., Weiner, B. J., Willmer, C., & Yan, R. (2012). THE DEEP2 GALAXY REDSHIFT SURVEY: THE VORONOI-DELAUNAY METHOD CATALOG OF GALAXY GROUPS. ASTROPHYSICAL JOURNAL, 751(1).
• Griffith, R. L., Cooper, M. C., Newman, J. A., Moustakas, L. A., Stern, D., Comerford, J. M., Davis, M., Lotz, J. M., Barden, M., Conselice, C. J., Capak, P. L., Faber, S. M., Kirkpatrick, J. D., Koekemoer, A. M., Koo, D. C., Noeske, K. G., Scoville, N., Sheth, K., Shopbell, P., , Willmer, C. N., et al. (2012). The Advanced Camera for Surveys General Catalog: Structural Parameters for Approximately Half a Million Galaxies. apjs, 200, 9.
• Griffith, R. L., Cooper, M. C., Newman, J. A., Moustakas, L. A., Stern, D., Comerford, J. M., Davis, M., Lotz, J. M., Barden, M., Conselice, C. J., Capak, P. L., Faber, S. M., Kirkpatrick, J. D., Koekemoer, A. M., Koo, D. C., Noeske, K. G., Scoville, N., Sheth, K., Shopbell, P., , Willmer, C. N., et al. (2012). The advanced camera for surveys general catalog: Structural parameters for approximately half a million galaxies. Astrophysical Journal, Supplement Series, 200(Issue 1). doi:10.1088/0067-0049/200/1/9
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  We present the Advanced Camera for Surveys General Catalog (ACS-GC), a photometric and morphological database using publicly available data obtained with the Advanced Camera for Surveys (ACS) instrument on the Hubble Space Telescope. The goal of the ACS-GC database is to provide a large statistical sample of galaxies with reliable structural and distance measurements to probe the evolution of galaxies over a wide range of look-back times. The ACS-GC includes approximately 470,000 astronomical sources (stars + galaxies) derived from the AEGIS, COSMOS, GEMS, and GOODS surveys. GALAPAGOS was used to construct photometric (SEXTRACTOR) and morphological (GALFIT) catalogs. The analysis assumes a single Sérsic model for each object to derive quantitative structural parameters. We include publicly available redshifts from the DEEP2, COMBO-17, TKRS, PEARS, ACES, CFHTLS, and zCOSMOS surveys to supply redshifts (spectroscopic and photometric) for a considerable fraction (74%) of the imaging sample. The ACS-GC includes color postage stamps, GALFIT residual images, and photometry, structural parameters, and redshifts combined into a single catalog. © 2012. The American Astronomical Society. All rights reserved..
• Griffith, R. L., Cooper, M. C., Newman, J. A., Moustakas, L. A., Stern, D., Comerford, J. M., Davis, M., Lotz, J. M., Barden, M., Conselice, C. J., Capak, P. L., Faber, S. M., Kirkpatrick, J. D., Koekemoer, A. M., Koo, D. C., Noeske, K. G., Scoville, N., Sheth, K., Shopbell, P., , Willmer, C., et al. (2012). THE ADVANCED CAMERA FOR SURVEYS GENERAL CATALOG: STRUCTURAL PARAMETERS FOR APPROXIMATELY HALF A MILLION GALAXIES. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 200(1).
• Kartaltepe, J. S., Dickinson, M., Alexander, D. M., Bell, E. F., Dahlen, T., Elbaz, D., Faber, S. M., Lotz, J., McIntosh, D. H., Wiklind, T., Altieri, B., Aussel, H., Bethermin, M., Bournaud, F., Charmandaris, V., Conselice, C. J., Cooray, A., Dannerbauer, H., Dav 'e, R., , Dunlop, J., et al. (2012). GOODS-Herschel and CANDELS: The Morphologies of Ultraluminous Infrared Galaxies at z ~ 2. apj, 757, 23.
• Kartaltepe, J. S., Dickinson, M., Alexander, D. M., Bell, E. F., Dahlen, T., Elbaz, D., Faber, S. M., Lotz, J., McIntosh, D. H., Wiklind, T., Altieri, B., Aussel, H., Bethermin, M., Bournaud, F., Charmandaris, V., Conselice, C. J., Cooray, A., Dannerbauer, H., Dave, R., , Dunlop, J., et al. (2012). GOODS-HERSCHEL AND CANDELS: THE MORPHOLOGIES OF ULTRALUMINOUS INFRARED GALAXIES AT z similar to 2. ASTROPHYSICAL JOURNAL, 757(1).
• Kartaltepe, J. S., Dickinson, M., Alexander, D. M., Bell, E. F., Dahlen, T., Elbaz, D., Faber, S. M., Lotz, J., McIntosh, D. H., Wiklind, T., Altieri, B., Aussel, H., Bethermin, M., Bournaud, F., Charmandaris, V., Conselice, C. J., Cooray, A., Dannerbauer, H., Davé, R., , Dunlop, J., et al. (2012). GOODS-Herschel and candels: The morphologies of ultraluminous infrared galaxies at z ∼ 2. Astrophysical Journal, 757(Issue 1). doi:10.1088/0004-637x/757/1/23
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  Using deep 100 and 160 μm observations in GOODS-South from GOODS-Herschel, combined with high-resolution HST/WFC3 near-infrared imaging from CANDELS, we present the first detailed morphological analysis of a complete, far-infrared (FIR) selected sample of 52 ultraluminous infrared galaxies (ULIRGs; LIR > 1012 L⊙) at z ∼ 2. We also make use of a comparison sample of galaxies with lower IR luminosities but with the same redshift and H-band magnitude distribution. Our visual classifications of these two samples indicate that the fractions of objects with disk and spheroid morphologies are roughly the same but that there are significantly more mergers, interactions, and irregular galaxies among the ULIRGs (72+5-7% versus 32 ± 3%). The combination of disk and irregular/interacting morphologies suggests that early-stage interactions, minor mergers, and disk instabilities could play an important role in ULIRGs at z ∼ 2. We compare these fractions with those of a z ∼ 1 sample selected from GOODS-H and COSMOS across a wide luminosity range and find that the fraction of disks decreases systematically with LIR while the fraction of mergers and interactions increases, as has been observed locally. At comparable luminosities, the fraction of ULIRGs with various morphological classifications is similar at z ∼ 2 and z ∼ 1, though there are slightly fewer mergers and slightly more disks at higher redshift. We investigate the position of the z ∼ 2 ULIRGs, along with 70 z ∼ 2 LIRGs, on the specific star formation rate versus redshift plane, and find 52 systems to be starbursts (i.e., they lie more than a factor of three above the main-sequence relation). We find that many of these systems are clear interactions and mergers (∼50%) compared to only 24% of systems on the main sequence relation. If irregular disks are included as potential minor mergers, then we find that up to ∼73% of starbursts are involved in a merger or interaction at some level. Although the final coalescence of a major merger may not be required for the high luminosities of ULIRGs at z ∼ 2 as is the case locally, the large fraction (50%-73%) of interactions at all stages and potential minor mergers suggests that these processes contribute significantly to the high star formation rates of ULIRGs at z ∼ 2. © 2012. The American Astronomical Society. All rights reserved.
• Kassin, S. A., Weiner, B. J., Faber, S. M., Gardner, J. P., Willmer, C. N., Coil, A. L., Cooper, M. C., Devriendt, J., Dutton, A. A., Guhathakurta, P., Koo, D. C., Metevier, A. J., Noeske, K. G., & Primack, J. R. (2012). The Epoch of Disk Settling: z ~ 1 to Now. apj, 758, 106.
• Kassin, S. A., Weiner, B. J., Faber, S. M., Gardner, J. P., Willmer, C., Coil, A. L., Cooper, M. C., Devriendt, J., Dutton, A. A., Guhathakurta, P., Koo, D. C., Metevier, A. J., Noeske, K. G., & Primack, J. R. (2012). THE EPOCH OF DISK SETTLING: z similar to 1 TO NOW. ASTROPHYSICAL JOURNAL, 758(2).
• Ko, J., Im, M., Lee, H. M., Lee, M. G., Kim, S. J., Shim, H., Jeon, Y., Hwang, H. S., Willmer, C. N., Malkan, M. A., Papovich, C., Weiner, B. J., Matsuhara, H., Oyabu, S., & Takagi, T. (2012). AKARI Observation of the North Ecliptic Pole (NEP) Supercluster at z = 0.087: Mid- infrared View of Transition Galaxies. apj, 745, 181.
• Ko, J., Im, M., Lee, H. M., Lee, M. G., Kim, S. J., Shim, H., Jeon, Y., Hwang, H. S., Willmer, C., Malkan, M. A., Papovich, C., Weiner, B. J., Matsuhara, H., Oyabu, S., & Takagi, T. (2012). AKARI OBSERVATION OF THE NORTH ECLIPTIC POLE (NEP) SUPERCLUSTER AT z=0.087: MID-INFRARED VIEW OF TRANSITION GALAXIES. ASTROPHYSICAL JOURNAL, 745(2).
• Martin, C. L., Shapley, A. E., Coil, A. L., Kornei, K. A., Bundy, K., Weiner, B. J., Noeske, K. G., & Schiminovich, D. (2012). DEMOGRAPHICS AND PHYSICAL PROPERTIES OF GAS OUTFLOWS/INFLOWS AT 0.4 < z < 1.4. ASTROPHYSICAL JOURNAL, 760(2).
• Martin, C. L., Shapley, A. E., Coil, A. L., Kornei, K. A., Bundy, K., Weiner, B. J., Noeske, K. G., & Schiminovich, D. (2012). Demographics and Physical Properties of Gas Outflows/Inflows at 0.4 lt z lt 1.4. apj, 760, 127.
• Mostek, N., Coil, A. L., Moustakas, J., Salim, S., & Weiner, B. J. (2012). CALIBRATING THE STAR FORMATION RATE AT z similar to 1 FROM OPTICAL DATA. ASTROPHYSICAL JOURNAL, 746(2).
• Mostek, N., Coil, A. L., Moustakas, J., Salim, S., & Weiner, B. J. (2012). Calibrating the Star Formation Rate at z ~ 1 from Optical Data. apj, 746, 124.
• Mostek, N., Coil, A. L., Moustakas, J., Salim, S., & Weiner, B. J. (2012). Calibrating the Star Formation Rate at z=1 from Optical Data. ApJ,.
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  We present a star-formation rate calibration based on optical data that isconsistent with average observed rates in both the red and blue galaxypopulations at z~1. The motivation for this study is to calculate SFRs forDEEP2 Redshift Survey galaxies in the 0.7
• Nidever, D. L., Zasowski, G., Majewski, S. R., Bird, J., Robin, A. C., Martinez-Valpuesta, I., Beaton, R. L., Sch "onrich, R., Schultheis, M., Wilson, J. C., Skrutskie, M. F., O'Connell, R. W., Shetrone, M., Schiavon, R. P., Johnson, J. A., Weiner, B., Gerhard, O., Schneider, D. P., Allende Prieto, C., , Sellgren, K., et al. (2012). The Apache Point Observatory Galactic Evolution Experiment: First Detection of High- velocity Milky Way Bar Stars. apjl, 755, L25.
• Nidever, D. L., Zasowski, G., Majewski, S. R., Bird, J., Robin, A. C., Martinez-Valpuesta, I., Beaton, R. L., Schoenrich, R., Schultheis, M., Wilson, J. C., Skrutskie, M. F., O'Connell, R. W., Shetrone, M., Schiavon, R. P., Johnson, J. A., Weiner, B., Gerhard, O., Schneider, D. P., Prieto, C. A., , Sellgren, K., et al. (2012). THE APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT: FIRST DETECTION OF HIGH-VELOCITY MILKY WAY BAR STARS. ASTROPHYSICAL JOURNAL LETTERS, 755(2).
• Nidever, D. L., Zasowski, G., Majewski, S. R., Bird, J., Robin, A. C., Martinez-Valpuesta, I., Beaton, R. L., Schönrich, R., Schultheis, M., Wilson, J. C., Skrutskie, M. F., O'Connell, R. W., Shetrone, M., Schiavon, R. P., Johnson, J. A., Weiner, B., Gerhard, O., Schneider, D. P., Allende Prieto, C., , Sellgren, K., et al. (2012). The apache point observatory galactic evolution experiment: First detection of high-velocity milky way bar stars. Astrophysical Journal Letters, 755(Issue 2). doi:10.1088/2041-8205/755/2/l25
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  Commissioning observations with the Apache Point Observatory Galactic Evolution Experiment (APOGEE), part of the Sloan Digital Sky Survey III, have produced radial velocities (RVs) for 4700K/M-giant stars in the Milky Way (MW) bulge. These high-resolution (R 22, 500), high-S/N (>100 per resolution element), near-infrared (NIR; 1.51-1.70 μm) spectra provide accurate RVs (εV 0.2kms-1) for the sample of stars in 18 Galactic bulge fields spanning -1° -32°. This represents the largest NIR high-resolution spectroscopic sample of giant stars ever assembled in this region of the Galaxy. A cold (σV 30kms-1), high-velocity peak (V GSR ≈ +200kms-1) is found to comprise a significant fraction (10%) of stars in many of these fields. These high RVs have not been detected in previous MW surveys and are not expected for a simple, circularly rotating disk. Preliminary distance estimates rule out an origin from the background Sagittarius tidal stream or a new stream in the MW disk. Comparison to various Galactic models suggests that these high RVs are best explained by stars in orbits of the Galactic bar potential, although some observational features remain unexplained. © © 2012. The American Astronomical Society. All rights reserved.
• Ono, Y., Ouchi, M., Mobasher, B., Dickinson, M., Penner, K., Shimasaku, K., Weiner, B. J., Kartaltepe, J. S., Nakajima, K., Nayyeri, H., Stern, D., Kashikawa, N., & Spinrad, H. (2012). SPECTROSCOPIC CONFIRMATION OF THREE z-DROPOUT GALAXIES AT z=6.844-7.213: DEMOGRAPHICS OF Ly alpha EMISSION IN z similar to 7 GALAXIES. ASTROPHYSICAL JOURNAL, 744(2).
• Papovich, C., Bassett, R., Lotz, J. M., Van Der Wel, A., Tran, K. V., Finkelstein, S. L., Bell, E. F., Conselice, C. J., Dekel, A., Dunlop, J. S., Guo, Y., Faber, S. M., Farrah, D., Ferguson, H. C., Finkelstein, K. D., Häussler, B., Kocevski, D. D., Koekemoer, A. M., Koo, D. C., , McGrath, E. J., et al. (2012). Candels observations of the structural properties of cluster galaxies at z = 1.62. Astrophysical Journal, 750(Issue 2). doi:10.1088/0004-637x/750/2/93
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  We discuss the structural and morphological properties of galaxies in a z = 1.62 proto-cluster using near-IR imaging data from Hubble Space Telescope Wide Field Camera 3 data of the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS). The cluster galaxies exhibit a clear color-morphology relation: galaxies with colors of quiescent stellar populations generally have morphologies consistent with spheroids, and galaxies with colors consistent with ongoing star formation have disk-like and irregular morphologies. The size distribution of the quiescent cluster galaxies shows a deficit of compact (≲ 1 kpc), massive galaxies compared to CANDELS field galaxies at z = 1.6. As a result, the cluster quiescent galaxies have larger average effective sizes compared to field galaxies at fixed mass at greater than 90% significance. Combined with data from the literature, the size evolution of quiescent cluster galaxies is relatively slow from z ≃ 1.6 to the present, growing as (1 + z)-0.6 ± 0.1. If this result is generalizable, then it implies that physical processes associated with the denser cluster region seem to have caused accelerated size growth in quiescent galaxies prior to z = 1.6 and slower subsequent growth at z < 1.6 compared to galaxies in the lower density field. The quiescent cluster galaxies at z = 1.6 have higher ellipticities compared to lower redshift samples at fixed mass, and their surface-brightness profiles suggest that they contain extended stellar disks. We argue that the cluster galaxies require dissipationless (i.e., gas-poor or "dry") mergers to reorganize the disk material and to match the relations for ellipticity, stellar mass, size, and color of early-type galaxies in z < 1 clusters. © © 2012. The American Astronomical Society. All rights reserved..
• Papovich, C., Bassett, R., Lotz, J. M., Wel, A., Tran, K., Finkelstein, S. L., Bell, E. F., Conselice, C. J., Dekel, A., Dunlop, J. S., Guo, Y., Faber, S. M., Farrah, D., Ferguson, H. C., Finkelstein, K. D., H "aussler, B., Kocevski, D. D., Koekemoer, A. M., Koo, D. C., , McGrath, E. J., et al. (2012). CANDELS Observations of the Structural Properties of Cluster Galaxies at z = 1.62. apj, 750, 93.
• Papovich, C., Bassett, R., Lotz, J. M., van, d., Tran, K. -., Finkelstein, S. L., Bell, E. F., Conselice, C. J., Dekel, A., Dunlop, J. S., Guo, Y., Faber, S. M., Farrah, D., Ferguson, H. C., Finkelstein, K. D., Haeussler, B., Kocevski, D. D., Koekemoer, A. M., Koo, D. C., , McGrath, E. J., et al. (2012). CANDELS OBSERVATIONS OF THE STRUCTURAL PROPERTIES OF CLUSTER GALAXIES AT z=1.62. ASTROPHYSICAL JOURNAL, 750(2).
• Rhoads, J. E., Hibon, P., Malhotra, S., Cooper, M., & Weiner, B. (2012). A Ly alpha GALAXY AT REDSHIFT z=6.944 IN THE COSMOS FIELD. ASTROPHYSICAL JOURNAL LETTERS, 752(2).
• Rhoads, J. E., Hibon, P., Malhotra, S., Cooper, M., & Weiner, B. (2012). A Ly$ alpha$ Galaxy at Redshift z = 6.944 in the COSMOS Field. apjl, 752, L28.
• Rhoads, J. E., Hibon, P., Malhotra, S., Cooper, M., & Weiner, B. (2012). A Lyman Alpha Galaxy at Redshift z=6.944 in the COSMOS Field.
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  Lyman-alpha emitting galaxies can be used to study cosmological reionization,because a neutral intergalactic medium scatters Lyman-alpha photons intodiffuse halos whose surface brightness falls below typical survey detectionlimits. Here we present the Lyman-alpha emitting galaxy LAEJ095950.99+021219.1, identified at redshift z=6.944 in the COSMOS field usingnarrowband imaging and followup spectroscopy with the IMACS instrument on theMagellan I Baade telescope. With a single object spectroscopically confirmed sofar, our survey remains consistent with a wide range of IGM neutral fraction atredshift seven, but further observations are planned and will help clarify thesituation. Meantime, the object we present here is only the third Lyman-alphaselected galaxy to be spectroscopically confirmed at redshift seven, and is2--3 times fainter than the previously confirmed redshift seven Lyman alphagalaxies.[Journal_ref: ]
• Rodney, S. A., Riess, A. G., Dahlen, T., Strolger, L., Ferguson, H. C., Hjorth, J., Frederiksen, T. F., Weiner, B. J., Mobasher, B., Casertano, S., Jones, D. O., Challis, P., Faber, S. M., Filippenko, A. V., Garnavich, P., Graur, O. r., Grogin, N. A., Hayden, B., Jha, S. W., , Kirshner, R. P., et al. (2012). A TYPE Ia SUPERNOVA AT REDSHIFT 1.55 IN HUBBLE SPACE TELESCOPE INFRARED OBSERVATIONS FROM CANDELS. ASTROPHYSICAL JOURNAL, 746(1).
• Rodney, S. A., Riess, A. G., Dahlen, T., Strolger, L., Ferguson, H. C., Hjorth, J., Frederiksen, T. F., Weiner, B. J., Mobasher, B., Casertano, S., Jones, D. O., Challis, P., Faber, S. M., Filippenko, A. V., Garnavich, P., Graur, O., Grogin, N. A., Hayden, B., Jha, S. W., , Kirshner, R. P., et al. (2012). A Type Ia Supernova at Redshift 1.55 in Hubble Space Telescope Infrared Observations from CANDELS. apj, 746, 5.
• Rujopakarn, W., Rieke, G. H., Papovich, C. J., Weiner, B. J., Rigby, J. R., Rex, M., Bian, F., Kuhn, O. P., & Thompson, D. (2012). Large Binocular Telescope and Spitzer Spectroscopy of Star-forming Galaxies at 1 ltz lt 3: Extinction and Star Formation Rate Indicators. apj, 755, 168.
• Sheth, K., Melbourne, J., Elmegreen, D. M., Elmegreen, B. G., Athanassoula, E., Abraham, R. G., & Weiner, B. J. (2012). HOT DISKS AND DELAYED BAR FORMATION. ASTROPHYSICAL JOURNAL, 758(2).
• Sheth, K., Melbourne, J., Elmegreen, D. M., Elmegreen, B. G., Athanassoula, E., Abraham, R. G., & Weiner, B. J. (2012). Hot Disks and Delayed Bar Formation. apj, 758, 136.
• Smith, N., Silverman, J. M., Filippenko, A. V., Cooper, M. C., Matheson, T., Bian, F., Weiner, B. J., & Comerford, J. M. (2012). SYSTEMATIC BLUESHIFT OF LINE PROFILES IN THE TYPE IIn SUPERNOVA 2010jl: EVIDENCE FOR POST-SHOCK DUST FORMATION?. ASTRONOMICAL JOURNAL, 143(1).
• Smith, N., Silverman, J. M., Filippenko, A. V., Cooper, M. C., Matheson, T., Bian, F., Weiner, B. J., & Comerford, J. M. (2012). Systematic Blueshift Of Line Profiles In The Type IIn Supernova 2010jl: Evidence For Post-Shock Dust Formation?. The Astronomical Journal, 143(1), 17. doi:10.1088/0004-6256/143/1/17
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  Type IIn supernovae (SNe) show spectral evidence for strong interaction between their blast wave and dense circumstellar material (CSM) around the progenitor star. SN 2010jl was the brightest core-collapse supernova in 2010, and it was a Type IIn explosion with strong CSM interaction. Andrews et al. recently reported evidence for an infrared (IR) excess in SN 2010jl, indicating either new dust formation or the heating of CSM dust in an IR echo. Here we report multi-epoch spectra of SN 2010jl that reveal the tell-tale signature of new dust formation: emission-line profiles becoming systematically more blueshifted as the red side of the line is blocked by increasing extinction. The effect is seen clearly in the intermediate-width (400-4000 km s–1) component of Hα beginning roughly 30 days after explosion. Moreover, we present near-IR spectra demonstrating that the asymmetry in the hydrogen-line profiles is wavelength dependent, appearing more pronounced at shorter wavelengths. This evidence suggests that new dust grains had formed quickly in the post-shock shell of SN 2010jl arising from CSM interaction. Since the observed dust temperature has been attributed to an IR echo and not to new dust, either (1) IR excess emission at λ < 5 μm is not a particularly sensitive tracer of new dust formation in SNe, or (2) some assumptions about expected dust temperatures might require further study. Lastly, we discuss one possible mechanism other than dust that might lead to increasingly blueshifted line profiles in SNe IIn, although the wavelength dependence of the asymmetry argues against this hypothesis in the case of SN 2010jl.
• Smith, N., Silverman, J. M., Filippenko, A. V., Cooper, M. C., Matheson, T., Bian, F., Weiner, B. J., & Comerford, J. M. (2012). Systematic Blueshift of Line Profiles in the Type IIn Supernova 2010jl: Evidence for Post-shock Dust Formation?. aj, 143, 17.
• Twite, J. W., Conselice, C. J., Buitrago, F., Noeske, K., Weiner, B. J., Acosta-Pulido, J. A., & Bauer, A. E. (2012). H$ alpha$ star formation rates in massive galaxies at z tilde 1. mnras, 420, 1061-1078.
• Twite, J. W., Conselice, C. J., Buitrago, F., Noeske, K., Weiner, B. J., Acosta-Pulido, J. A., & Bauer, A. E. (2012). Ha star formation rates in massive galaxies at z similar to 1. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 420(2), 1061-1078.
• Twite, J. W., Conselice, C. J., Buitrago, F., Noeske, K., Weiner, B. J., Acosta-Pulido, J. A., & Bauer, A. E. (2012). Hα star formation rates in massive galaxies at z~ 1. Monthly Notices of the Royal Astronomical Society, 420(Issue 2). doi:10.1111/j.1365-2966.2011.20057.x
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  We present a near-infrared spectroscopic study of a stellar mass selected sample of galaxies at z~ 1 utilizing the Long-slit Intermediate Resolution Infrared Spectrograph multi-object spectrograph on the William Herschel Telescope. We detect continuum, and the Hα line for our sample, which is one of the better direct tracers of star formation in external galaxies. We spectroscopically measure the Hα emission from 41 massive (M * > 10 10.5M ⊙) galaxies taken from the POWIR Survey with spectroscopic redshifts 0.4 < z spec < 1.4. We correct our Hα fluxes for dust extinction by using multiwavelength data, and investigate star formation rate (SFR) trends with mass and colour. We find a drop in the fraction of massive galaxies with M * > 10 11M ⊙ which are detected in Hα emission at z < 0.9. We furthermore find that the fraction of galaxies with Hα emission drops steadily and significantly with redder (U-B) colours at z~ 1, and that the specific SFR (SSFR) drops with increasing (U-B) colour for galaxies at all masses. By investigating the SFR-mass relation, we find that the SFR is roughly constant with mass, in possible contrast to previous work, and that the SSFR is lower in the most massive galaxies. The scatter in the SFR versus mass relationship is very small for those systems with ongoing star formation, which suggests that star formation in the most massive galaxies at z~ 1 shuts off rather abruptly over
• Wang, T., Huang, J., Faber, S. M., Fang, G., Wuyts, S., Fazio, G. G., Yan, H., Dekel, A., Guo, Y., Ferguson, H. C., Grogin, N., Lotz, J. M., Weiner, B., McGrath, E. J., Kocevski, D., Hathi, N. P., Lucas, R. A., Koekemoer, A. M., Kong, X. u., & Gu, Q. (2012). CANDELS: CORRELATIONS OF SPECTRAL ENERGY DISTRIBUTIONS AND MORPHOLOGIES WITH STAR FORMATION STATUS FOR MASSIVE GALAXIES AT z similar to 2. ASTROPHYSICAL JOURNAL, 752(2).
• Wang, T., Huang, J., Faber, S. M., Fang, G., Wuyts, S., Fazio, G. G., Yan, H., Dekel, A., Guo, Y., Ferguson, H. C., Grogin, N., Lotz, J. M., Weiner, B., McGrath, E. J., Kocevski, D., Hathi, N. P., Lucas, R. A., Koekemoer, A. M., Kong, X., & Gu, Q. (2012). CANDELS: Correlations of Spectral Energy Distributions and Morphologies with Star formation Status for Massive Galaxies at z ~ 2. apj, 752, 134.
• Wu, J., Tsai, C. W., Sayers, J., Benford, D., Bridge, C., Blain, A., Eisenhardt, P. M., Stern, D., Petty, S., Assef, R., Bussmann, S., Comerford, J. M., Cutri, R., Evans, N. J., Griffith, R., Jarrett, T., Lake, S., Lonsdale, C., Rho, J., , Stanford, A., et al. (2012). Submillimeter follow-up of wise-selected hyperluminous galaxies. Astrophysical Journal, 756(Issue 1). doi:10.1088/0004-637x/756/1/96
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  We have used the Caltech Submillimeter Observatory (CSO) to follow-up a sample of Wide-field Infrared Survey Explorer (WISE) selected, hyperluminous galaxies, the so-called W1W2-dropout galaxies. This is a rare ( ∼1000 all-sky) population of galaxies at high redshift (peaks at z= 2-3), which are faint or undetected by WISE at 3.4 and 4.6 μm, yet are clearly detected at 12 and 22 μm. The optical spectra of most of these galaxies show significant active galactic nucleus activity. We observed 14 high-redshift (z > 1.7) W1W2-dropout galaxies with SHARC-II at 350-850 μm, with nine detections, and observed 18 with Bolocam at 1.1mm, with five detections. Warm Spitzer follow-up of 25 targets at 3.6 and 4.5 μm, as well as optical spectra of 12 targets, are also presented in the paper. Combining WISE data with observations from warm Spitzer and CSO, we constructed their mid-IR to millimeter spectral energy distributions (SEDs). These SEDs have a consistent shape, showing significantly higher mid-IR to submillimeter ratios than other galaxy templates, suggesting a hotter dust temperature. We estimate their dust temperatures to be 60-120K using a single-temperature model. Their infrared luminosities are well over 10 13 L⊙. These SEDs are not well fitted with existing galaxy templates, suggesting they are a new population with very high luminosity and hot dust. They are likely among the most luminous galaxies in the universe. We argue that they are extreme cases of luminous, hot dust-obscured galaxies (DOGs), possibly representing a short evolutionary phase during galaxy merging and evolution. A better understanding of their long-wavelength properties needs ALMA as well as Herschel data. © 2012. The American Astronomical Society. All rights reserved.
• Wu, J., Tsai, C., Sayers, J., Benford, D., Bridge, C., Blain, A., Eisenhardt, P. R., Stern, D., Petty, S., Assef, R., Bussmann, S., Comerford, J. M., Cutri, R., Evans, N. J., Griffith, R., Jarrett, T., Lake, S., Lonsdale, C., Rho, J., , Stanford, S. A., et al. (2012). Submillimeter Follow-up of WISE-selected Hyperluminous Galaxies. apj, 756, 96.
• Wu, J., Tsai, C., Sayers, J., Benford, D., Bridge, C., Blain, A., Eisenhardt, P., Stern, D., Petty, S., Assef, R., Bussmann, S., Comerford, J. M., Cutri, R., Evans, N., Griffith, R., Jarrett, T., Lake, S., Lonsdale, C., Rho, J., , Stanford, S. A., et al. (2012). SUBMILLIMETER FOLLOW-UP OF WISE-SELECTED HYPERLUMINOUS GALAXIES. ASTROPHYSICAL JOURNAL, 756(1).
• Wuyts, S., Schreiber, N. M., Genzel, R., Guo, Y., Barro, G., Bell, E. F., Dekel, A., Faber, S. M., Ferguson, H. C., Giavalisco, M., Grogin, N. A., Hathi, N. P., Huang, K., Kocevski, D. D., Koekemoer, A. M., Koo, D. C., Lotz, J., Lutz, D., McGrath, E., , Newman, J. A., et al. (2012). Smooth(er) Stellar Mass Maps in CANDELS: Constraints on the Longevity of Clumps in High-redshift Star-forming Galaxies. apj, 753, 114.
• Wuyts, S., Schreiber, N., Genzel, R., Guo, Y., Barro, G., Bell, E. F., Dekel, A., Faber, S. M., Ferguson, H. C., Giavalisco, M., Grogin, N. A., Hathi, N. P., Huang, K., Kocevski, D. D., Koekemoer, A. M., Koo, D. C., Lotz, J., Lutz, D., McGrath, E., , Newman, J. A., et al. (2012). SMOOTH(ER) STELLAR MASS MAPS IN CANDELS: CONSTRAINTS ON THE LONGEVITY OF CLUMPS IN HIGH-REDSHIFT STAR-FORMING GALAXIES. ASTROPHYSICAL JOURNAL, 753(2).
• Yan, H., Finkelstein, S. L., Huang, K., Ryan, R. E., Ferguson, H. C., Koekemoer, A. M., Grogin, N. A., Dickinson, M., Newman, J. A., Somerville, R. S., Dav 'e, R., Faber, S. M., Papovich, C., Guo, Y., Giavalisco, M., Lee, K., Reddy, N., Cooray, A. R., Siana, B. D., , Hathi, N. P., et al. (2012). Luminous and High Stellar Mass Candidate Galaxies at z ap 8 Discovered in the Cosmic Assembly Near-Infrared Deep Extragalactic Legacy Survey. apj, 761, 177.
• Yan, H., Finkelstein, S. L., Huang, K., Ryan, R. E., Ferguson, H. C., Koekemoer, A. M., Grogin, N. A., Dickinson, M., Newman, J. A., Somerville, R. S., Dave, R., Faber, S. M., Papovich, C., Guo, Y., Giavalisco, M., Lee, K., Reddy, N., Cooray, A. R., Siana, B. D., , Hathi, N. P., et al. (2012). LUMINOUS AND HIGH STELLAR MASS CANDIDATE GALAXIES AT z approximate to 8 DISCOVERED IN THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY. ASTROPHYSICAL JOURNAL, 761(2).
• Atek, H., Bell, E. F., Dickinson, M., Donley, J. L., Dunlop, J. S., Faber, S. M., Ferguson, H. C., Finkelstein, S. L., Grogin, N. A., Hathi, N. P., Juneau, S., Kartaltepe, J. S., Kocevski, D. D., Koekemoer, A. M., Koo, D. C., Laird, E. S., Mcgrath, E. J., Mozena, M., Nandra, K., , Newman, J. A., et al. (2011). A CANDELS WFC3 grism study of emission-line galaxies at z ~ 2: a mix of nuclear activity and low-metallicity star formation. The Astrophysical Journal, 743(2), 144. doi:10.1088/0004-637x/743/2/144
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  We present Hubble Space Telescope Wide Field Camera 3 (WFC3) slitless grism spectroscopy of 28 emission-line galaxies at z ~ 2, in the GOODS-S region of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. The high sensitivity of these grism observations, with >1σ detections of emission lines to f > 2.5 × 10^(–18) erg s^(–1) cm^(–2), means that the galaxies in the sample are typically ~7 times less massive (median M_* = 10^(9.5) M_☉) than previously studied z ~ 2 emission-line galaxies. Despite their lower mass, the galaxies have [O III]/Hβ ratios which are very similar to previously studied z ~ 2 galaxies and much higher than the typical emission-line ratios of local galaxies. The WFC3 grism allows for unique studies of spatial gradients in emission lines, and we stack the two-dimensional spectra of the galaxies for this purpose. In the stacked data the [O III] emission line is more spatially concentrated than the Hβ emission line with 98.1% confidence. We additionally stack the X-ray data (all sources are individually undetected), and find that the average L_([O III])/L_(0.5-10keV) ratio is intermediate between typical z ~ 0 obscured active galaxies and star-forming galaxies. Together the compactness of the stacked [O III] spatial profile and the stacked X-ray data suggest that at least some of these low-mass, low-metallicity galaxies harbor weak active galactic nuclei.
• Chen, H. W., Cooksey, K. L., Mulchaey, J. S., Prochaska, J. X., & Weiner, B. J. (2011). PROBING THE IGM/GALAXY CONNECTION. IV. THE LCO/WFCCD GALAXY SURVEY OF 20 FIELDS SURROUNDING UV-BRIGHT QUASARS. Astrophysical Journal Supplement Series, 193(2), 28. doi:10.1088/0067-0049/193/2/28
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  We publish the survey for galaxies in 20 fields containing ultraviolet bright quasars (with z em 0.1-0.5) that can be used to study the association between galaxies and absorption systems from the low-z intergalactic medium (IGM). The survey is magnitude limited (R 19.5 mag) and highly complete out to 10' from the quasar in each field. It was designed to detect dwarf galaxies (L 0.1L*) at an impact parameter ρ 1 Mpc (z = 0.1) from a quasar. The complete sample (all 20 fields) includes R-band photometry for 84,718 sources and confirmed redshifts for 2800 sources. This includes 1198 galaxies with 0.005 < z < (z em – 0.01) at a median redshift of 0.18, which may associated with IGM absorption lines. All of the imaging was acquired with cameras on the Swope 40'' telescope and the spectra were obtained via slit mask observations using the WFCCD spectrograph on the Dupont 100'' telescope at Las Campanas Observatory. This paper describes the data reduction, imaging analysis, photometry, and spectral analysis of the survey. We tabulate the principal measurements for all sources in each field and provide the spectroscopic data set online.
• Coil, A. L., Weiner, B. J., Holz, D. E., Cooper, M. C., Yan, R., & Aird, J. (2011). OUTFLOWING GALACTIC WINDS IN POST-STARBURST AND ACTIVE GALACTIC NUCLEUS HOST GALAXIES AT 0.2 < z < 0.8. ASTROPHYSICAL JOURNAL, 743(1).
• Coil, A. L., Weiner, B. J., Holz, D. E., Cooper, M. C., Yan, R., & Aird, J. (2011). Outflowing Galactic Winds in Post-starburst and Active Galactic Nucleus Host Galaxies at 0.2 < z < 0.8. The Astrophysical Journal, 743(1), 46. doi:10.1088/0004-637x/743/1/46
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  We present Keck/LRIS-B spectra for a sample of 10 AEGIS X-ray active galactic nucleus (AGN) host galaxies and 13 post-starburst galaxies from SDSS and DEEP2 at 0.2 < z < 0.8 in order to investigate the presence, properties, and influence of outflowing galactic winds at intermediate redshifts. We focus on galaxies that either host a low-luminosity AGN or have recently had their star formation quenched to test whether these galaxies have winds of sufficient velocity to potentially clear gas from the galaxy. We find, using absorption features of Fe II, Mg II, and Mg I, that six of the ten (60%) X-ray AGN host galaxies and four of the thirteen (31%) post-starburst galaxies have outflowing galactic winds, with typical velocities of {approx}200 km s{sup -1}. We additionally find that most of the galaxies in our sample show line emission, possibly from the wind, in either Fe II* or Mg II. A total of 100% of our X-ray AGN host sample (including four red sequence galaxies) and 77% of our post-starburst sample has either blueshifted absorption or line emission. Several K+A galaxies have small amounts of cool gas absorption at the systemic velocity, indicating that not all of the cool gasmore » has been expelled. We conclude that while outflowing galactic winds are common in both X-ray low-luminosity AGN host galaxies and post-starburst galaxies at intermediate redshifts, the winds are likely driven by supernovae (as opposed to AGNs) and do not appear to have sufficiently high velocities to quench star formation in these galaxies.« less
• Dutton, A. A., van, d., Faber, S. M., Simard, L., Kassin, S. A., Koo, D. C., Bundy, K., Huang, J., Weiner, B. J., Cooper, M. C., Newman, J. A., Mozena, M., & Koekemoer, A. M. (2011). On the evolution of the velocity-mass-size relations of disc-dominated galaxies over the past 10 billion years. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 410(3), 1660-1676.
• Grogin, N. A., Kocevski, D. D., Faber, S. M., Ferguson, H. C., Koekemoer, A. M., Riess, A. G., Acquaviva, V., Alexander, D. M., Almaini, O., Ashby, M. L., Barden, M., Bell, E. F., Bournaud, F., Brown, T. M., Caputi, K. I., Casertano, S., Cassata, P., Castellano, M., Challis, P., , Chary, R. R., et al. (2011). CANDELS: The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. Astrophysical Journal Supplement Series, 197(2), 35. doi:10.1088/0067-0049/197/2/35
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  The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) is designed to document the first third of galactic evolution, over the approximate redshift (z) range 8-1.5. It will image >250,000 distant galaxies using three separate cameras on the Hubble Space Telescope, from the mid-ultraviolet to the near-infrared, and will find and measure Type Ia supernovae at z > 1.5 to test their accuracy as standardizable candles for cosmology. Five premier multi-wavelength sky regions are selected, each with extensive ancillary data. The use of five widely separated fields mitigates cosmic variance and yields statistically robust and complete samples of galaxies down to a stellar mass of 10(9)M(circle dot) to z approximate to 2, reaching the knee of the ultraviolet luminosity function of galaxies to z approximate to 8. The survey covers approximately 800 arcmin(2) and is divided into two parts. The CANDELS/Deep survey (5 sigma point-source limit H = 27.7 mag) covers similar to 125 arcmin(2) within Great Observatories Origins Deep Survey (GOODS)-N and GOODS-S. The CANDELS/Wide survey includes GOODS and three additional fields (Extended Groth Strip, COSMOS, and Ultra-deep Survey) and covers the full area to a 5 sigma point-source limit of H greater than or similar to 27.0 mag. Together with the Hubble Ultra Deep Fields, the strategy creates a three-tiered "wedding-cake" approach that has proven efficient for extragalactic surveys. Data from the survey are nonproprietary and are useful for a wide variety of science investigations. In this paper, we describe the basic motivations for the survey, the CANDELS team science goals and the resulting observational requirements, the field selection and geometry, and the observing design. The Hubble data processing and products are described in a companion paper.
• Grogin, N. A., Kocevski, D. D., Faber, S. M., Ferguson, H. C., Koekemoer, A. M., Riess, A. G., Acquaviva, V., Alexander, D. M., Almaini, O., Ashby, M., Barden, M., Bell, E. F., Bournaud, F., Brown, T. M., Caputi, K. I., Casertano, S., Cassata, P., Castellano, M., Challis, P., , Chary, R., et al. (2011). CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 197(2).
• Kassin, S. A., Fogarty, L., Goodsall, T., Clarke, F. J., Houghton, R., Salter, G., Thatte, N., Tecza, M., Davies, R. L., Weiner, B. J., Willmer, C., Salim, S., Cooper, M. C., Newman, J. A., Bundy, K., Conselice, C. J., Koekemoer, A. M., Lin, L., Moustakas, L. A., & Wang, T. (2011). Oxford SWIFT integral field spectrograph and multiwavelength observations of the Eagle galaxy at z=0.77. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 417(4), 2882-2890.
• Koekemoer, A. M., Faber, S. M., Ferguson, H. C., Grogin, N. A., Kocevski, D. D., Koo, D. C., Lai, K., Lotz, J. M., Lucas, R. A., McGrath, E. J., Ogaz, S., Rajan, A., Riess, A. G., Rodney, S. A., Strolger, L., Casertano, S., Castellano, M., Dahlen, T., Dickinson, M., , Dolch, T., et al. (2011). CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY-THE HUBBLE SPACE TELESCOPE OBSERVATIONS, IMAGING DATA PRODUCTS, AND MOSAICS. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 197(2).
• Koekemoer, A. M., Faber, S. M., Ferguson, H. C., Grogin, N. A., Kocevski, D. D., Koo, D. C., Lai, K., Lotz, J. M., Lucas, R. A., McGrath, E. J., Ogaz, S., Rajan, A., Riess, A. G., Rodney, S. A., Strolger, L., Casertano, S., Castellano, M., Dahlen, T., Dickinson, M., , Dolch, T., et al. (2011). Candels: The cosmic assembly near-infrared deep extragalactic legacy survey - The hubble space telescope observations, imaging data products, and mosaics. Astrophysical Journal Supplement Series, 197(2), 36. doi:10.1088/0067-0049/197/2/36
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  This paper describes the Hubble Space Telescope imaging data products and data reduction procedures for the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS). This survey is designed to document the evolution of galaxies and black holes at z 1.5-8, and to study Type Ia supernovae at z > 1.5. Five premier multi-wavelength sky regions are selected, each with extensive multi-wavelength observations. The primary CANDELS data consist of imaging obtained in the Wide Field Camera 3 infrared channel (WFC3/IR) and the WFC3 ultraviolet/optical channel, along with the Advanced Camera for Surveys (ACS). The CANDELS/Deep survey covers ~125 arcmin2 within GOODS-N and GOODS-S, while the remainder consists of the CANDELS/Wide survey, achieving a total of ~800 arcmin2 across GOODS and three additional fields (Extended Groth Strip, COSMOS, and Ultra-Deep Survey). We summarize the observational aspects of the survey as motivated by the scientific goals and present a detailed description of the data reduction procedures and products from the survey. Our data reduction methods utilize the most up-to-date calibration files and image combination procedures. We have paid special attention to correcting a range of instrumental effects, including charge transfer efficiency degradation for ACS, removal of electronic bias-striping present in ACS data after Servicing Mission 4, and persistence effects and other artifacts in WFC3/IR. For each field, we release mosaics for individual epochs and eventual mosaics containing data from all epochs combined, to facilitate photometric variability studies and the deepest possible photometry. A more detailed overview of the science goals and observational design of the survey are presented in a companion paper.
• Prochaska, J. X., Weiner, B., Chen, H. -., Mulchaey, J., & Cooksey, K. (2011). PROBING THE INTERGALACTIC MEDIUM/GALAXY CONNECTION. V. ON THE ORIGIN OF Ly alpha AND O VI ABSORPTION AT z < 0.2. ASTROPHYSICAL JOURNAL, 740(2).
• Prochaska, J. X., Weiner, B., Chen, H. W., Mulchaey, J., & Cooksey, K. (2011). Probing the intergalactic medium/galaxy connection. V. on the origin of Lyα and O VI absorption at z < 0.2. Astrophysical Journal, 740(Issue 2). doi:10.1088/0004-637x/740/2/91
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  We analyze the association of galaxies with Lyα and O VI absorption, the most commonly detected transitions of the low-z intergalactic medium (IGM), in the fields of 14 quasars with z em = 0.06-0.57. Confirming previous studies, we observe a high covering fraction for Lyα absorption to impact parameter ρ = 300h -1 72kpc: 33/37 of our L > 0.01 L* galaxies show Lyα equivalent width W Lyα ≥ 50m. Galaxies of all luminosity L > 0.01 L* and spectral type are surrounded by a diffuse and ionized circumgalactic medium (CGM), whose baryonic mass is estimated at ∼1010.5±0.3 M ⊙ for a constant N H = 1019 cm -2. The virialized halos and extended CGM of present-day galaxies are responsible for most strong Lyα absorbers (W Lyα > 300m) but cannot reproduce the majority of observed lines in the Lyα forest. We conclude that the majority of Lyα absorption with W Lyα = 30-300m occurs in the cosmic web predicted by cosmological simulations and estimate a characteristic width for these filaments of 400h -1 72kpc. Regarding O VI, we observe a near unity covering fraction to ρ = 200h -1 72kpc for L > 0.1 L* galaxies and to ρ = 300h -1 72kpc for sub-L* (0.1 L* < L < L*) galaxies. Similar to our Lyα results, stronger O VI systems (W 1031 > 70m) arise in the virialized halos of L > 0.1 L* galaxies. Unlike Lyα, the weaker O VI systems (W 1031 30m) arise in the extended CGM of sub-L* galaxies. The majority of O VI gas observed in the low-z IGM is associated with a diffuse medium surrounding individual galaxies with L 0.3 L* and rarely originates in the so-called warm-hot IGM (predicted by cosmological simulations. © 2011. The American Astronomical Society. All rights reserved.
• Trump, J. R., Weiner, B. J., Scarlata, C., Kocevski, D. D., Bell, E. F., McGrath, E. J., Koo, D. C., Faber, S. M., Laird, E. S., Mozena, M., Rangel, C., Yan, R., Yesuf, H., Atek, H., Dickinson, M., Donley, J. L., Dunlop, J. S., Ferguson, H. C., Finkelstein, S. L., , Grogin, N. A., et al. (2011). A CANDELS WFC3 GRISM STUDY OF EMISSION-LINE GALAXIES AT z similar to 2: A MIX OF NUCLEAR ACTIVITY AND LOW-METALLICITY STAR FORMATION. ASTROPHYSICAL JOURNAL, 743(2).
• Van Der Wel, A., Straughn, A. N., Rix, H. W., Finkelstein, S. L., Koekemoer, A. M., Weiner, B. J., Wuyts, S., Bell, E. F., Faber, S. M., Trump, J. R., Koo, D. C., Ferguson, H. C., Scarlata, C., Hathi, N. P., Dunlop, J. S., Newman, J. A., Dickinson, M., Jahnke, K., Salmon, B. W., , De Mello, D. F., et al. (2011). Extreme emission-line galaxies in CANDELS: Broadband-selected, starbursting dwarf galaxies at z > 1. Astrophysical Journal, 742(Issue 2). doi:10.1088/0004-637x/742/2/111
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  We identify an abundant population of extreme emission-line galaxies (EELGs) at redshift z ∼ 1.7 in the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey imaging from Hubble Space Telescope/Wide Field Camera 3 (HST/WFC3). Sixty-nine EELG candidates are selected by the large contribution of exceptionally bright emission lines to their near-infrared broadband magnitudes. Supported by spectroscopic confirmation of strong [O III] emission lines - with rest-frame equivalent widths ∼1000 Å- in the four candidates that have HST/WFC3 grism observations, we conclude that these objects are galaxies with ∼108 M⊙ in stellar mass, undergoing an enormous starburst phase with M*/M *;̇of only ∼15Myr. These bursts may cause outflows that are strong enough to produce cored dark matter profiles in low-mass galaxies. The individual star formation rates and the comoving number density (3.7 × 10-4 Mpc-3) can produce in ∼4Gyr much of the stellar mass density that is presently contained in 10 8-109 M⊙ dwarf galaxies. Therefore, our observations provide a strong indication that many or even most of the stars in present-day dwarf galaxies formed in strong, short-lived bursts, mostly at z > 1. © 2011. The American Astronomical Society. All rights reserved.
• Yan, R., Ho, L. C., Newman, J. A., Coil, A. L., Willmer, C. N., Laird, E. S., Georgakakis, A., Aird, J., Barmby, P., Bundy, K., Cooper, M. C., Davis, M., Faber, S. M., Fang, T., Griffith, R. L., Koekemoer, A. M., Koo, D. C., Nandra, K., Park, S. Q., , Sarajedini, V. L., et al. (2011). Aegis: Demographics of X-ray and optically selected active galactic nuclei. Astrophysical Journal, 728(Issue 1). doi:10.1088/0004-637x/728/1/38
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  We develop a new diagnostic method to classify galaxies into active galactic nucleus (AGN) hosts, star-forming galaxies, and absorption-dominated galaxies by combining the [O III]/Hβ ratio with rest-frame U.B color. This can be used to robustly select AGNs in galaxy samples at intermediate redshifts (z < 1). We compare the result of this optical AGN selection with X-ray selection using a sample of 3150 galaxies with 0.3 < z < 0.8 and IAB < 22, selected from the DEEP2 Galaxy Redshift Survey and the All-wavelength Extended Groth Strip International Survey. Among the 146 X-ray sources in this sample, 58% are classified optically as emission-line AGNs, the rest as star-forming galaxies or absorption-dominated galaxies. The latter are also known as "X-ray bright, optically normal galaxies" (XBONGs). Analysis of the relationship between optical emission lines and X-ray properties shows that the completeness of optical AGN selection suffers from dependence on the star formation rate and the quality of observed spectra. It also shows that XBONGs do not appear to be a physically distinct population from other X-ray detected, emission-line AGNs. On the other hand, X-ray AGN selection also has strong bias. About 2/3 of all emission-line AGNs at Lbol > 1044 erg s-1 in our sample are not detected in our 200 ks Chandra images, most likely due to moderate or heavy absorption by gas near the AGN. The 2-7 keV detection rate of Seyfert 2s at z ∼ 0.6 suggests that their column density distribution and Compton-thick fraction are similar to that of local Seyferts. Multiple sample selection techniques are needed to obtain as complete a sample as possible. © 2011. The American Astronomical Society.
• Yan, R., Ho, L. C., Newman, J. A., Coil, A. L., Willmer, C., Laird, E. S., Georgakakis, A., Aird, J., Barmby, P., Bundy, K., Cooper, M. C., Davis, M., Faber, S. M., Fang, T., Griffith, R. L., Koekemoer, A. M., Koo, D. C., Nandra, K., Park, S. Q., , Sarajedini, V. L., et al. (2011). AEGIS: DEMOGRAPHICS OF X-RAY AND OPTICALLY SELECTED ACTIVE GALACTIC NUCLEI. ASTROPHYSICAL JOURNAL, 728(1).
• van, d., Straughn, A. N., Rix, H. -., Finkelstein, S. L., Koekemoer, A. M., Weiner, B. J., Wuyts, S., Bell, E. F., Faber, S. M., Trump, J. R., Koo, D. C., Ferguson, H. C., Scarlata, C., Hathi, N. P., Dunlop, J. S., Newman, J. A., Dickinson, M., Jahnke, K., Salmon, B. W., , de, M., et al. (2011). EXTREME EMISSION-LINE GALAXIES IN CANDELS: BROADBAND-SELECTED, STARBURSTING DWARF GALAXIES AT z > 1. ASTROPHYSICAL JOURNAL, 742(2).
• Chen, Y., Tremonti, C. A., Heckman, T. M., Kauffmann, G., Weiner, B. J., Brinchmann, J., & Wang, J. (2010). ABSORPTION-LINE PROBES OF THE PREVALENCE AND PROPERTIES OF OUTFLOWS IN PRESENT-DAY STAR-FORMING GALAXIES. ASTRONOMICAL JOURNAL, 140(2), 445-461.
• Chen, Y., Tremonti, C. A., Heckman, T. M., Kauffmann, G., Weiner, B. J., Brinchmann, J., & Wang, J. (2010). Absorption-line probes of the prevalence and properties of outflows in present-day star-forming galaxies. The Astronomical Journal, 445-461.
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  We analyze star forming galaxies drawn from SDSS DR7 to show how theinterstellar medium (ISM) Na I 5890, 5896 (Na D) absorption lines depend ongalaxy physical properties, and to look for evidence of galactic winds. Wecombine the spectra of galaxies with similar geometry/physical parameters tocreate composite spectra with signal-to-noise ~300. The stellar continuum ismodeled using stellar population synthesis models, and the continuum-normalizedspectrum is fit with two Na I absorption components. We find that: (1) ISM Na Dabsorption lines with equivalent widths EW > 0.8A are only prevalent in diskgalaxies with specific properties -- large extinction (Av), high star formationrates (SFR), high star formation rate per unit area ($\Sigma_{\rm SFR}$), orhigh stellar mass (M*). (2) the ISM Na D absorption lines can be separated intotwo components: a quiescent disk-like component at the galaxy systemic velocityand an outflow component; (3) the disk-like component is much stronger in theedge-on systems, and the outflow component covers a wide angle but is strongerwithin 60deg of the disk rotation axis; (4) the EW and covering factor of thedisk component correlate strongly with dust attenuation, highlighting theimportance that dust shielding may play the survival of Na I. (5) The EW of theoutflow component depends primarily on $\Sigma_{\rm SFR}$ and secondarily onAv; (6) the outflow velocity varies from ~120 to 160km/s but shows little hintof a correlation with galaxy physical properties over the modest dynamic rangethat our sample probes (1.2 dex in log$\Sigma_{\rm SFR}$ and 1 dex in log M*).[Journal_ref: The Astronomical Journal 140 (2010) 445-461]
• Cooper, M. C., Coil, A. L., Gerke, B. F., Newman, J. A., Bundy, K., Conselice, C. J., Croton, D. J., Davis, M., Faber, S. M., Guhathakurta, P., Koo, D. C., Lin, L., Weiner, B. J., Willmer, C., & Yan, R. (2010). Absence of evidence is not evidence of absence: the colour-density relation at fixed stellar mass persists to z similar to 1. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 409(1), 337-345.
• Covington, M. D., Kassin, S. A., Dutton, A. A., Weiner, B. J., Cox, T. J., Jonsson, P., Primack, J. R., Faber, S. M., & Koo, D. C. (2010). EVOLUTION OF THE STELLAR MASS TULLY-FISHER RELATION IN DISK GALAXY MERGER SIMULATIONS. ASTROPHYSICAL JOURNAL, 710(1), 279-288.
• Covington, M. D., Kassin, S. A., Dutton, A. A., Weiner, B. J., Cox, T. J., Jonsson, P., Primack, J. R., Faber, S. M., & Koo, D. C. (2010). Evolution of the stellar mass Tully-fisher relation in disk galaxy merger simulations. Astrophysical Journal, 710(Issue 1). doi:10.1088/0004-637x/710/1/279
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  There is a large observational scatter toward low velocities in the stellar mass Tully-Fisher (TF) relation if disturbed and compact objects are included. However, this scatter can be eliminated if one replaces rotation velocity with S 0.5, a quantity that includes a velocity dispersion term added in quadrature with the rotation velocity. In this work, we use a large suite of hydrodynamic N-body galaxy merger simulations to explore a possible mechanism for creating the observed relations. Using mock observations of the simulations, we test for the presence of observational effects and explore the relationship between S 0.5 and intrinsic properties of the galaxies. We find that galaxy mergers can explain the scatter in the TF as well as the tight S 0.5-stellar mass relation. Furthermore, S 0.5 is correlated with the total central mass of a galaxy, including contributions due to dark matter. © 2010 The American Astronomical Society.
• Genzel, R., Tacconi, L. J., Gracia-Carpio, J., Sternberg, A., Cooper, M. C., Shapiro, K., Bolatto, A., Bouche, N., Bournaud, F., Burkert, A., Combes, F., Comerford, J., Cox, P., Davis, M., Schreiber, N., Garcia-Burillo, S., Lutz, D., Naab, T., Neri, R., , Omont, A., et al. (2010). A study of the gas-star formation relation over cosmic time. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 407(4), 2091-2108.
• Rubin, K. H., Prochaska, J. X., Koo, D. C., Phillips, A. C., & Weiner, B. J. (2010). Galaxies probing galaxies: Cool halo gas from A z = 0.47 post-starburst galaxy. Astrophysical Journal, 712(Issue 1). doi:10.1088/0004-637x/712/1/574
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  We study the cool gas around a galaxy at z = 0.4729 using Keck/LRIS spectroscopy of a bright (B = 21.7) background galaxy at z = 0.6942 at a transverse distance of 16.5h -1 70 kpc. The background galaxy spectrum reveals strong Fe II, Mg II, Mg I, and Ca II absorption at the redshift of the foreground galaxy, with an Mg II λ2796 rest equivalent width of 3.93 0.08, indicative of a velocity width exceeding 400 km s -1. Because the background galaxy is large (>4h -1 70 kpc), the high covering fraction of the absorbing gas suggests that it arises in a spatially extended complex of cool clouds with large velocity dispersion. Spectroscopy of the massive (log M */M ⊙ = 11.15 0.08) host galaxy reveals that it experienced a burst of star formation about 1 Gyr ago and that it harbors a weak active galactic nucleus. We discuss the possible origins of the cool gas in its halo, including multiphase cooling of hot halo gas, cold inflow, tidal interactions, and galactic winds. We conclude that the absorbing gas was most likely ejected or tidally stripped from the interstellar medium of the host galaxy or its progenitors during the past starburst event. Adopting the latter interpretation, these results place one of only a few constraints on the radial extent of cool gas driven or stripped from a galaxy in the distant universe. Future studies with integral field unit spectroscopy of spatially extended background galaxies will provide multiple sight lines through foreground absorbers and permit analysis of the morphology and kinematics of the gas surrounding galaxies with a diverse set of properties and environments. © 2010. The American Astronomical Society. All rights reserved..
• Rubin, K. H., Weiner, B. J., Koo, D. C., Martin, C. L., Prochaska, J. X., Coil, A. L., & Newman, J. A. (2010). The persistence of cool galactic winds in high stellar mass galaxies between z ∼ 1.4 and ∼1. Astrophysical Journal, 719(Issue 2). doi:10.1088/0004-637x/719/2/1503
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  We present an analysis of the Mgii λλ2796, 2803 and Feii λλ 2586, 2600 absorption line profiles in co-added spectra of 468 galaxies at 0.7 < z < 1.5. The galaxy sample, drawn from the Team Keck Treasury Redshift Survey of the GOODS-N field, has a range in stellar mass (M*) comparable to that of the sample at z ∼ 1.4 analyzed in a similar manner by Weiner et al. (W09), but extends to lower redshifts and has specific star formation rates which are lower by ∼0.6 dex. We identify outflows of cool gas from the Doppler shift of the Mg ii absorption lines and find that the equivalent width (EW) of absorption due to outflowing gas increases on average with M* and star formation rate (SFR). We attribute the large EWs measured in spectra of the more massive, higher-SFR galaxies to optically thick absorbing clouds having large velocity widths. The outflows have hydrogen column densities N(H) ≳ 1019.4 cm -2 and extend to velocities of ∼500 km s-1. While galaxies with SFR > 10 M⊙ yr-1 host strong outflows in both this and the W09 sample, we do not detect outflows in lower-SFR (i.e., log M*/M⊙ ≲ 10.5) galaxies at lower redshifts. Using a simple galaxy evolution model that assumes exponentially declining SFRs, we infer that strong outflows persist in galaxies with log M*/M⊙ > 10.5 as they age between z = 1.4 and z ∼ 1, presumably because of their high absolute SFRs. Finally, our spectral analysis, combined with high-resolution Hubble Space Telescope/Advanced Camera for Surveys imaging, weakly suggests that outflow absorption strength increases with galaxy SFR surface density. © 2010. The American Astronomical Society.
• Rubin, K., Prochaska, J. X., Koo, D. C., Phillips, A. C., & Weiner, B. J. (2010). GALAXIES PROBING GALAXIES: COOL HALO GAS FROM A z=0.47 POST-STARBURST GALAXY. ASTROPHYSICAL JOURNAL, 712(1), 574-584.
• Rubin, K., Weiner, B. J., Koo, D. C., Martin, C. L., Prochaska, J. X., Coil, A. L., & Newman, J. A. (2010). THE PERSISTENCE OF COOL GALACTIC WINDS IN HIGH STELLAR MASS GALAXIES BETWEEN z similar to 1.4 AND similar to 1*. ASTROPHYSICAL JOURNAL, 719(2), 1503-1525.
• Tacconi, L. J., Genzel, R., Neri, R., Cox, P., Cooper, M. C., Shapiro, K., Bolatto, A., Bouche, N., Bournaud, F., Burkert, A., Combes, F., Comerford, J., Davis, M., Schreiber, N., Garcia-Burillo, S., Gracia-Carpio, J., Lutz, D., Naab, T., Omont, A., , Shapley, A., et al. (2010). High molecular gas fractions in normal massive star-forming galaxies in the young Universe. NATURE, 463(7282), 781-784.
• Veilleux, S., Weiner, B. J., Rupke, D. S., McDonald, M., Birk, C., Bland-Hawthorn, J., Dressler, A., Hare, T., Osip, D., Pietraszewski, C., & Vogel, S. N. (2010). MMTF: THE MARYLAND-MAGELLAN TUNABLE FILTER. The Astronomical Journal, 139(1), 145-157. doi:10.1088/0004-6256/139/1/145
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  This paper describes the Maryland-Magellan Tunable Filter (MMTF) on the Magellan-Baade 6.5 m telescope. MMTF is based on a 150 mm clear aperture Fabry-Perot (FP) etalon that operates in low orders and provides transmission bandpass and central wavelength adjustable from ~5 A to ~15 A and from ~5000 A to over ~9200 A, respectively. It is installed in the Inamori Magellan Areal Camera and Spectrograph and delivers an image quality of ~05 over a field of view of 27' in diameter (monochromatic over ~10'). This versatile and easy-to-operate instrument has been used over the past three years for a wide variety of projects. This paper first reviews the basic principles of FP tunable filters, and then provides a detailed description of the hardware and software associated with MMTF and the techniques developed to observe with this instrument and reduce the data. The main lessons learned in the course of the commissioning and implementation of MMTF are highlighted next, before concluding with a brief outlook on the future of MMTF and of similar facilities which are soon coming on line.
• van den Bosch, A. A., Faber, S. M., Simard, L., Kassin, S. A., Koo, D. C., Bundy, K., Huang, J., Weiner, B. J., Cooper, M. C., Newman, J. A., Mozena, M., & Koekemoer, A. M. (2010). On the evolution of the velocity–mass–size relations of disc-dominated galaxies over the past 10 billion years. Monthly Notices of the Royal Astronomical Society, 410(3), 1660-1676. doi:10.1111/j.1365-2966.2010.17555.x
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  We study the evolution of the scaling relations between maximum circular velocity, stellar mass and optical half-light radius of star-forming disk-dominated galaxies in the context ofCDM-based galaxy formation models. Using data from the literature combined with new data from the DEEP2 and AEGIS surveys we show that there is a consistent picture for the evolution of these scaling relations from z � 2 to z = 0, both observationally and theoretically. The evolution of the observed stellar scaling rela- tions is weaker than that of the virial scaling relations of dark matter haloes, which can be reproduced, both qualitatively and quantitatively, with a simple, cosmologically- motivated model for disk evolution inside growing Navarro-Frenk-White dark matter haloes. In this model optical half-light radii are smaller, both at fixed stellar mass and maximum circular velocity, at higher redshifts. This model also predicts that the scaling relations between baryonic quantities (baryonic mass, baryonic half-mass radii, and maximum circular velocity) evolve even more weakly than the corresponding stel- lar relations. We emphasize, though, that this weak evolution does not imply that individual galaxies evolve weakly. On the contrary, individual galaxies grow strongly in mass, size and velocity, but in such a way that they move largely along the scaling relations. Finally, recent observations have claimed surprisingly large sizes for a num- ber of star-forming disk galaxies at z ' 2, which has caused some authors to suggest that high redshift disk galaxies have abnormally high spin parameters. However, we argue that the disk scale lengths in question have been systematically overestimated by a factor � 2, and that there is an offset of a factor � 1:4 between Hsizes and optical sizes. Taking these effects into account, there is no indication that star forming galaxies at high redshifts (z ' 2) have abnormally high spin parameters.
• Blanton, M. R., Coil, A. L., Cooper, M. C., Dave, R., Hogg, D. W., Holden, B. P., Jonsson, P., Kassin, S. A., Lotz, J. M., Moustakas, J., Newman, J. A., Prochaska, J. X., Teuben, P., Tremonti, C., Weiner, B. J., & Willmer, C. N. (2009). Astronomical Software Wants To Be Free: A Manifesto. Astrophysics, 2010.
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  Author(s): Weiner, Benjamin J; Blanton, Michael R; Coil, Alison L; Cooper, Michael C; Dave, Romeel; Hogg, David W; Holden, Bradford P; Jonsson, Patrik; Kassin, Susan A; Lotz, Jennifer M; Moustakas, John; Newman, Jeffrey A; Prochaska, JX; Teuben, Peter J; Tremonti, Christy A; Willmer, Christopher NA | Abstract: Astronomical software is now a fact of daily life for all hands-on members of our community. Purpose-built software for data reduction and modeling tasks becomes ever more critical as we handle larger amounts of data and simulations. However, the writing of astronomical software is unglamorous, the rewards are not always clear, and there are structural disincentives to releasing software publicly and to embedding it in the scientific literature, which can lead to significant duplication of effort and an incomplete scientific record. We identify some of these structural disincentives and suggest a variety of approaches to address them, with the goals of raising the quality of astronomical software, improving the lot of scientist-authors, and providing benefits to the entire community, analogous to the benefits provided by open access to large survey and simulation datasets. Our aim is to open a conversation on how to move forward. We advocate that: (1) the astronomical community consider software as an integral and fundable part of facility construction and science programs; (2) that software release be considered as integral to the open and reproducible scientific process as are publication and data release; (3) that we adopt technologies and repositories for releasing and collaboration on software that have worked for open-source software; (4) that we seek structural incentives to make the release of software and related publications easier for scientist-authors; (5) that we consider new ways of funding the development of grass-roots software; (6) and that we rethink our values to acknowledge that astronomical software development is not just a technical endeavor, but a fundamental part of our scientific practice.
• Coil, A. L., Georgakakis, A., Newman, J. A., Cooper, M. C., Croton, D., Davis, M., Koo, D. C., Laird, E. S., Nandra, K., Weiner, B. J., Willmer, C. N., & Yan, R. (2009). Aegis: The clustering of x-ray active galactic nucleus relative to galaxies at z 1. Astrophysical Journal, 701(Issue 2). doi:10.1088/0004-637x/701/2/1484
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  We measure the clustering of nonquasar X-ray active galactic nucleus (AGN) at z = 0.7-1.4 in the AEGIS field. Using the cross-correlation of 113 Chandra-selected AGN, with a median log L X = 42.8 erg s -1, with 5000 DEEP2 galaxies, we find that the X-ray AGNs are fitted by a power law with a clustering scale length of r 0 = 5.95 0.90 h -1 Mpc and slope γ = 1.66 0.22. X-ray AGNs have a similar clustering amplitude as red, quiescent and "green" transition galaxies at z 1 and are significantly more clustered than blue, star-forming galaxies. The X-ray AGN clustering strength is primarily determined by the host galaxy color; AGNs in red host galaxies are significantly more clustered than AGNs in blue host galaxies, with a relative bias that is similar to that of red to blue DEEP2 galaxies. We detect no dependence of clustering on optical brightness, X-ray luminosity, or hardness ratio within the ranges probed here. We find evidence for galaxies hosting X-ray AGN to be more clustered than a sample of galaxies with matching joint optical color and magnitude distributions. This implies that galaxies hosting X-ray AGN are more likely to reside in groups and more massive dark matter halos than galaxies of the same color and luminosity without an X-ray AGN. In comparison to optically selected quasars in the DEEP2 fields, we find that X-ray AGNs at z 1 are more clustered than optically selected quasars (with a 2.6σ significance) and therefore may reside in more massive dark matter halos. Our results are consistent with galaxies undergoing a quasar phase while in the blue cloud before settling on the red sequence with a lower-luminosity X-ray AGN, if they are similar objects at different evolutionary stages. © 2009 The American Astronomical Society. All rights reserved.
• Coil, A. L., Georgakakis, A., Newman, J. A., Cooper, M. C., Croton, D., Davis, M., Koo, D. C., Laird, E. S., Nandra, K., Weiner, B. J., Willmer, C., & Yan, R. (2009). AEGIS: THE CLUSTERING OF X-RAY ACTIVE GALACTIC NUCLEUS RELATIVE TO GALAXIES AT z similar to 1. ASTROPHYSICAL JOURNAL, 701(2), 1484-1499.
• Rieke, G. H., Alonso-Herrero, A., Weiner, B. J., Perez-Gonzalez, P. G., Blaylock, M., Donley, J. L., & Marcillac, D. (2009). DETERMINING STAR FORMATION RATES FOR INFRARED GALAXIES. ASTROPHYSICAL JOURNAL, 692(1), 556-573.
• Rieke, G. H., Alonso-Herrero, A., Weiner, B. J., Pérez-González, P. G., Blaylock, M., Donley, J. L., & Marcillac, D. (2009). Determining Star Formation Rates for Infrared Galaxies. The Astrophysical Journal, 692(1), 556-573. doi:10.1088/0004-637x/692/1/556
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  We show that measures of star formation rates (SFRs) for infrared galaxies using either single-band 24 μm or extinction-corrected Paα luminosities are consistent in the total infrared luminosity = L(TIR) ~ 1010 L ☉ range. MIPS 24 μm photometry can yield SFRs accurately from this luminosity upward: SFR(M ☉ yr–1) = 7.8 × 10–10 L(24 μm, L ☉) from L(TIR) = 5× 109 L ☉ to 1011 L ☉ and SFR = 7.8 × 10–10 L(24 μm, L ☉)(7.76 × 10–11 L(24))0.048 for higher L(TIR). For galaxies with L(TIR) ≥ 1010 L ☉, these new expressions should provide SFRs to within 0.2 dex. For L(TIR) ≥ 1011 L ☉, we find that the SFR of infrared galaxies is significantly underestimated using extinction-corrected Paα (and presumably using any other optical or near-infrared recombination lines). As a part of this work, we constructed spectral energy distribution templates for eleven luminous and ultraluminous purely star forming infrared galaxies and over the spectral range 0.4 μm to 30 cm. We use these templates and the SINGS data to construct average templates from 5 μm to 30 cm for infrared galaxies with L(TIR) = 5× 109 to 1013 L ☉. All of these templates are made available online.
• Salim, S., Dickinson, M., Rich, R. M., Charlot, S., Lee, J. C., Schiminovich, D., Perez-Gonzalez, P. G., Ashby, M., Papovich, C., Faber, S. M., Ivison, R. J., Frayer, D. T., Walton, J. M., Weiner, B. J., Chary, R., Bundy, K., Noeske, K., & Koekemoer, A. M. (2009). MID-IR LUMINOSITIES AND UV/OPTICAL STAR FORMATION RATES AT z < 1.4. ASTROPHYSICAL JOURNAL, 700(1), 161-182.
• Salim, S., Dickinson, M., Rich, R. M., Charlot, S., Lee, J. C., Schiminovich, D., Pérez-González, P. G., Ashby, M. L., Papovich, C., Faber, S. M., Ivison, R. J., Frayer, D. T., Walton, J. M., Weiner, B. J., Chary, R. R., Bundy, K., Noeske, K., & Koekemoer, A. M. (2009). MID-IR luminosities and UV/OPTICAL star formation rates at z < 1.4. Astrophysical Journal, 700(Issue 1). doi:10.1088/0004-637x/700/1/161
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  Ultraviolet (UV) nonionizing continuum and mid-infrared (IR) emission constitute the basis of two widely used star formation (SF) indicators at intermediate and high redshifts. We study 2430 galaxies with z < 1.4 in the Extended Groth Strip with deep MIPS 24 μm observations from FIDEL, spectroscopy from DEEP2, and UV, optical, and near-IR photometry from the AEGIS. The data are coupled with dust-reddened stellar population models and Bayesian spectral energy distribution (SED) fitting to estimate dust-corrected star formation rates (SFRs). In order to probe the dust heating from stellar populations of various ages, the derived SFRs were averaged over various timescales-from 100 Myr for "current" SFR (corresponding to young stars) to 1-3 Gyr for long-timescale SFRs (corresponding to the light-weighted age of the dominant stellar populations). These SED-based UV/optical SFRs are compared to total IR luminosities extrapolated from 24 μm observations, corresponding to 10-18 μm rest frame. The total IR luminosities are in the range of normal star-forming galaxies and luminous IR galaxies (1010-1012LΘ). We show that the IR luminosity can be estimated from the UV and optical photometry to within a factor of 2, implying that most z < 1.4 galaxies are not optically thick. We find that for the blue, actively star-forming galaxies the correlation between the IR luminosity and the UV/optical SFR shows a decrease in scatter when going from shorter to longer SFR-averaging timescales. We interpret this as the greater role of intermediate age stellar populations in heating the dust than what is typically assumed. Equivalently, we observe that the IR luminosity is better correlated with dust-corrected optical luminosity than with dust-corrected UV light. We find that this holds over the entire redshift range. Many so-called green valley galaxies are simply dust-obscured actively star-forming galaxies. However, there exist 24 μm detected galaxies, some with LIR > 1011LΘ, yet with little current SF. For them a reasonable amount of dust absorption of stellar light (but presumably higher than in nearby early-type galaxies) is sufficient to produce the observed levels of IR, which includes a large contribution from intermediate and old stellar populations. In our sample, which contains very few ultraluminous IR galaxies, optical and X-ray active galactic nuclei do not contribute on average more than ∼ 50% to the mid-IR luminosity, and we see no evidence for a large population of "IR excess" galaxies.
• Weiner, B. J. (2009). Star Formation Driven Galactic Winds at z similar to 1.4. MONSTER'S FIERY BREATH: FEEDBACK IN GALAXIES, GROUPS, AND CLUSTERS, 1201, 142-145.
• Weiner, B. J., Coil, A. L., Prochaska, J. X., Newman, J. A., Cooper, M. C., Bundy, K., Conselice, C. J., Dutton, A. A., Faber, S. M., Koo, D. C., Lotz, J. M., Rieke, G. H., & Rubin, K. (2009). UBIQUITOUS OUTFLOWS IN DEEP2 SPECTRA OF STAR-FORMING GALAXIES AT z=1.4. ASTROPHYSICAL JOURNAL, 692(1), 187-211.
• Weiner, B. J., Coil, A. L., Prochaska, J. X., Newman, J. A., Cooper, M. C., Bundy, K., Conselice, C. J., Dutton, A. A., Faber, S. M., Koo, D. C., Lotz, J. M., Rieke, G. H., & Rubin, K. H. (2009). Ubiquitous outflows in DEEP2 spectra of star-forming galaxies at z = 1.4. Astrophysical Journal, 692(Issue 1). doi:10.1088/0004-637x/692/1/187
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  Galactic winds are a prime suspect for the metal enrichment of the intergalactic medium (IGM) and may have a strong influence on the chemical evolution of galaxies and the nature of QSO absorption-line systems. We use a sample of 1406 galaxy spectra at z ∼ 1.4 from the DEEP2 redshift survey to show that blueshifted Mg IYI λλ 2796, 2803 absorption is ubiquitous in star-forming galaxies at this epoch. This is the first detection of frequent outflowing galactic winds at z ∼ 1. The presence and depth of absorption are independent of active galactic nuclei spectral signatures or galaxy morphology; major mergers are not a prerequisite for driving a galactic wind from massive galaxies. Outflows are found in co-added spectra of galaxies spanning a range of 30 times in stellar mass and 10 times in star formation rate (SFR), calibrated from K-band and from the Multiband Imaging Photometer for Spitzer IR fluxes. The outflows have column densities of order NH ∼ 1020 cm-2 and characteristic velocities of ∼ 300-500 km s-1, with absorption seen out to 1000 km s-1 in the most massive, highest SFR galaxies. The velocities suggest that the outflowing gas can escape into the IGM and that massive galaxies can produce cosmologically and chemically significant outflows. Both the Mg II equivalent width and the outflow velocity are larger for galaxies of higher stellar mass and SFR, with Vwind ∼ SFR0.3, similar to the scaling in low redshift IR-luminous galaxies. The high frequency of outflows in the star-forming galaxy population at z ∼ 1 indicates that galactic winds occur in the progenitors of massive spirals as well as those of ellipticals. The increase of outflow velocity with mass and SFR constrains theoretical models of galaxy evolution that include feedback from galactic winds, and may favor momentum-driven models for the wind physics. © 2009. The American Astronomical Society. All rights reserved.
• Yan, R., Newman, J. A., Faber, S. M., Coil, A. L., Cooper, M. C., Davis, M., Weiner, B. J., Gerke, B. F., & Koo, D. C. (2009). The DEEP2 Galaxy Redshift Survey: Environments of post-starburst galaxies at z ∼ 0.1 and ∼0.8. Monthly Notices of the Royal Astronomical Society, 398(Issue 2). doi:10.1111/j.1365-2966.2009.15192.x
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  Post-starburst (also known as K+A) galaxies exhibit spectroscopic signatures indicating that their star formation was recently quenched; they are candidates for galaxies in transition from a star-forming phase to a passively evolving phase. We have spectroscopically identified large samples of post-starburst galaxies both in the Sloan Digital Sky Survey (SDSS) at z ∼ 0.1 and in the DEEP2 Galaxy Redshift Survey at z ∼ 0.8, using a uniform and robust selection method based on a cut in Hβ line emission rather than the more problematic [O ii] λ3727. Based on measurements of the overdensity of galaxies around each object, we find that post-starburst galaxies brighter than 0.4L*B at low redshift have a similar, statistically indistinguishable environment distribution as blue galaxies, preferring underdense environments, but dramatically different from that of red galaxies. However, at higher-z, the environment distribution of post-starburst galaxies is more similar to red galaxies than to blue galaxies. We conclude that the quenching of star formation and the build-up of the red sequence through the K+A phase is happening in relatively overdense environments at z ∼ 1 but in relatively underdense environments at z ∼ 0. Although the relative environments where quenching occurs are decreasing with time, the corresponding absolute environment may have stayed the same along with the quenching mechanisms, because the mean absolute environments of all galaxies has to grow with time. In addition, we do not find any significant dependence on luminosity in the environment distribution of K+As. The existence of a large K+A population in the field at both redshifts indicates that cluster-specific mechanisms cannot be the dominant route by which these galaxies are formed. Our work also demonstrates that studying post-starburst-environment relations by measuring the K+A fraction in different environments, as is the common practice, is highly non-robust; modest changes in the comparison population used to define the fraction can drastically alter conclusions. Statistical comparisons of the overall environment distributions of different populations are much better behaved. © 2009 RAS.
• Yan, R., Newman, J. A., Faber, S. M., Coil, A. L., Cooper, M. C., Davis, M., Weiner, B. J., Gerke, B. F., & Koo, D. C. (2009). The DEEP2 Galaxy Redshift Survey: environments of post-starburst galaxies at z similar to 0.1 and similar to 0.8. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 398(2), 735-753.
• Coil, A. L., Newman, J. A., Croton, D., Cooper, M. C., Davis, M., Faber, S. M., Gerke, B. F., Koo, D. C., Padmanabhan, N., Wechsler, R. H., & Weiner, B. J. (2008). The DEEP2 Galaxy Redshift Survey: Color and luminosity dependence of galaxy clustering at z similar to 1. ASTROPHYSICAL JOURNAL, 672(1), 153-176.
• Cooksey, K. L., Prochaska, J. X., Chen, H., Mulchaey, J. S., & Weiner, B. J. (2008). Characterizing the low-redshift intergalactic medium toward PKS 1302-102. ASTROPHYSICAL JOURNAL, 676(1), 262-285.
• Cooper, M. C., Guhathakurta, P., Kirby, E. N., Konidaris, N. P., Koo, D. C., Lemaux, B. C., Martin, C. L., Newman, J. A., Sawicki, M., & Weiner, B. J. (2008). The DEEP2 Redshift Survey: Lyα Emitters in the Spectroscopic Database*. The Astrophysical Journal, 687(2), 884-898. doi:10.1086/591779
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  We present the first results of a search for Lyα emitters (LAEs) in the DEEP2 spectroscopic database that uses a search technique that is different from but complementary to traditional narrowband imaging surveys. We have visually inspected ~20% of the available DEEP2 spectroscopic data and have found nine high-quality LAEs with clearly asymmetric line profiles and an additional 10 objects of lower quality, some of which may also be LAEs. Our survey is most sensitive to LAEs at z = 4.4–4.9 and that is indeed where all but one of our high-quality objects are found. We find the number density of our spectroscopically discovered LAEs to be consistent with those found in narrowband imaging searches. The combined, averaged spectrum of our nine high-quality objects is well fit by a two-component model, with a second, lower amplitude component redshifted by ~420 km s−1 with respect to the primary Lyα line, consistent with large-scale outflows from these objects. We conclude by discussing the advantages and future prospects of blank-sky spectroscopic surveys for high-z LAEs.
• Cooper, M. C., Newman, J. A., Weiner, B. J., Yan, R., Willmer, C., Bundy, K., Coil, A. L., Conselice, C. J., Davis, M., Faber, S. M., Gerke, B. F., Guhathakurta, P., Koo, D. C., & Noeske, K. G. (2008). The DEEP2 Galaxy Redshift Survey: the role of galaxy environment in the cosmic star formation history. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 383(3), 1058-1078.
• Lin, L., Patton, D. R., Koo, D. C., Casteels, K., Conselice, C. J., Faber, S. M., Lotz, J., Willmer, C., Hsieh, B. C., Chiueh, T., Newman, J. A., Novak, G. S., Weiner, B. J., & Cooper, M. C. (2008). The redshift evolution of wet, dry, and mixed galaxy mergers from close galaxy pairs in the DEEP2 galaxy Redshift Survey. ASTROPHYSICAL JOURNAL, 681(1), 232-243.
• Lotz, J. M., Davis, M., Faber, S. M., Guhathakurta, P., Gwyn, S., Huang, J., Koo, D. C., Le, F. E., Lin, L., Newman, J., Noeske, K., Papovich, C., Willmer, C., Coil, A., Conselice, C. J., Cooper, M., Hopkins, A. M., Metevier, A., Primack, J., , Rieke, G., et al. (2008). The evolution of galaxy mergers and morphology at z < 1.2 in the Extended Groth Strip. ASTROPHYSICAL JOURNAL, 672(1), 177-197.
• Marcillac, D., Rieke, G. H., Papovich, C., Willmer, C. N., Weiner, B. J., Coil, A. L., Cooper, M. C., Gerke, B. F., Woo, J., Newman, J. A., Georgakakis, A., Laird, E. S., Nandra, K., Fazio, G. G., Huang, J. S., & Koo, D. C. (2008). The Environment on a Few Mpc Scales of Infrared Luminous Galaxies at Redshift z~1. The Astrophysical Journal, 675(2), 1156-1170. doi:10.1086/527031
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  We investigate the environment of infrared-luminous galaxies [ -->LIR(8–1000 μ m) > 1011 L☉]. We focus on the redshift range -->0.7 ≤ z≤ 1, where these galaxies dominate the star formation activity and play a significant role in galaxy evolution. We employ MIPS 24 μm data to identify infrared galaxies in the Extended Groth Strip (EGS). We use a local density indicator to probe the environment on a few Mpc scales and a group member catalog, both of which make use of the DEEP2 spectroscopic redshift catalog, to quantify the environment of these galaxies. We find that the local environment of LIRGs and ULIRGs is intermediate between that of blue and red galaxies. LIRGs and ULIRGs avoid underdense environments and inhabit local environments that are more dense on average than those of other DEEP2 galaxies at similar redshifts. However, when the comparison sample of the non-IR DEEP2 galaxies is restricted to have the same range of stellar mass, color, or luminosity as the IR galaxies, there is no longer any significant difference in environment: the IR galaxies follow the same trends in the color-environment and luminosity-environment relations observed at -->z ~ 1. We also find that about 30% of the LIRGs and ULIRGs belong to groups, associated with a minimum dark matter halo of -->6 × 1012 M☉ h−1. The group members constitute 20% of the sources responsible for the IR star formation rate density and comoving energy density at -->z ~ 1.
• Sanchez, R. Z., Sellwood, J. A., Weiner, B. J., & Williams, T. B. (2008). Modeling the Gas Flow in the Bar of NGC 1365. The Astrophysical Journal, 674(2), 797-813. doi:10.1086/524940
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  We present new observations of the strongly barred galaxy NGC 1365, including new photometric images and Fabry-Perot spectroscopy, as well as a detailed reanalysis of the neutral hydrogen observations from the VLA archive. We find the galaxy to be at once remarkably bisymmetric in its I-band light distribution and strongly asymmetric in the distribution of dust and in the kinematics of the gas in the bar region. The velocity field mapped in the Hα line reveals bright H II regions with velocities that differ by 60-80 km s−1 from that of the surrounding gas, which may be due to remnants of infalling material. We have attempted hydrodynamic simulations of the bar flow to estimate the separate disk and halo masses, using two different dark matter halo models and covering a wide range of mass-to-light ratios () and bar pattern speeds (Ωp). None of our models provides a compelling fit to the data, but they seem most nearly consistent with a fast bar, corotation at ~1.2rB, and ΥI 2.0 ± 1.0, implying a massive, but not fully maximal, disk. The fitted dark halos are unusually concentrated, a requirement driven by the declining outer rotation curve.
• Sawicki, M., Lemaux, B. C., Guhathakurta, P., Kirby, E. N., Konidaris, N. P., Martin, C. L., Cooper, M. C., Koo, D. C., Newman, J. A., & Weiner, B. J. (2008). THE DEEP2 REDSHIFT SURVEY: Ly alpha EMITTERS IN THE SPECTROSCOPIC DATABASE. ASTROPHYSICAL JOURNAL, 687(2), 884-898.
• Conselice, C. J., Bundy, K., Trujillo, I., Coil, A., Eisenhardt, P., Ellis, R. S., Georgakakis, A., Huang, J., Lotz, J., Nandra, K., Newman, J., Papovich, C., Weiner, B., & Willmer, C. (2007). The properties and evolution of a K-band selected sample of massive galaxies at z similar to 0.4-2 in the Palomar/DEEP2 survey. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 381(3), 962-986.
• Conselice, C. J., Newman, J. A., Georgakakis, A., Almaini, O., Coil, A. L., Cooper, M. C., Eisenhardt, P., Foucaud, S., Koekemoer, A., Lotz, J., Noeske, K., Weiner, B., & Wlllmer, C. N. (2007). AEGIS: The Diversity of Bright Near-IR Selected Distant Red Galaxies. The Astrophysical Journal, 660(1), L55-L58. doi:10.1086/517921
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  AEGIS: The Diversity of Bright Near-IR Selected Distant Red Galaxies C. J. Conselice 1 , J. A. Newman 2,3 , A. Georgakakis 4 , O. Almaini 1 , A. L. Coil 3,5 , M.C. Cooper 6 , P. Eisenhardt 7 , S. Foucaud 1 , A. Koekemoer 8 , J. Lotz 9 , K. Noeske 10 , B. Weiner 11 , C.N.A Willmer 5 arXiv:astro-ph/0607242 v1 11 Jul 2006 ABSTRACT We use deep and wide near infrared (NIR) imaging from the Palomar telescope combined with DEEP2 spectroscopy and Hubble Space Telescope (HST) and Chandra Space Telescope imaging to investigate the nature of galaxies that are red in NIR colors. We locate these ‘distant red galaxies’ (DRGs) through the color cut (J − K) vega > 2.3 over 0.7 deg 2 , where we find 1010 DRG candidates down to K s = 20.5. We combine 95 high quality spectroscopic redshifts with photometric redshifts from BRIJK photometry to determine the redshift and stellar mass distributions for these systems, and morphological/structural and X-ray properties for 107 DRGs in the Extended Groth Strip. We find that many bright (J − K) vega > 2.3 galaxies with K s 2 systems massive with M ∗ > 10 11 M ⊙ . HST imaging shows that the structural properties and morphologies of DRGs are also diverse, with the majority elliptical/compact School of Physics and Astronomy, University of Nottingham, NG7 2RD, UK Lawrence Berkeley National Laboratory, Berkeley, CA 94720 Hubble Fellow Imperial College, London Stewart Observatory, University of Arizona, Tucson, AZ University of California, Berkeley NASA Jet Propulsion Laboratory, California Institute of Technology Space Telescope Science Institute, Baltimore, MD Goldberg Fellow, National Optical Astronomy Observatory, Tucson, AZ 85726 University of California, Santa Cruz, Santa Cruz, CA Department of Physics, University of Maryland, College Park, MD 20742
• Cooper, M. C., Newman, J. A., Coil, A. L., Croton, D. J., Gerke, B. F., Yan, R., Davis, M., Faber, S. M., Guhathakurta, P., Koo, D. C., Weiner, B. J., & Willmer, C. (2007). The DEEP2 galaxy redshift survey: evolution of the colour-density relation at 0.4 < z < 1.35. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 376(4), 1445-1459.
• Cooper, M. C., Newman, J. A., Weiner, B. J., Yan, R., Willmer, C. N., Bundy, K., Coil, A. L., Conselice, C. J., Davis, M., Faber, S. M., Gerke, B. F., Guhathakurta, P., Koo, D. C., & Noeske, K. G. (2007). The DEEP2 Galaxy Redshift Survey: the role of galaxy environment in the cosmic star formation history. Monthly Notices of the Royal Astronomical Society, 383(3), 1058-1078. doi:10.1111/j.1365-2966.2007.12613.x
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  Using galaxy samples drawn from the Sloan Digital Sky Survey and the DEEP2 Galaxy Redshift Survey, we study the relationship between star formation and environment at z ∼ 0.1 and 1. We estimate the total star formation rate (SFR) and specific star formation rate (sSFR) for each galaxy according to the measured [O II] λ 3727 A nebular line luminosity, corrected using empirical calibrations to match more robust SFR indicators. Echoing previous results, we find that in the local Universe star formation depends on environment such that galaxies in regions of higher overdensity, on average, have lower SFRs and longer star formation time-scales than their counterparts in lower density regions. At z ∼ 1, we show that the relationship between sSFR and environment mirrors that found locally. However, we discover that the relationship between total SFR and overdensity at z ∼ 1 is inverted relative to the local relation. This observed evolution in the SFR-density relation is driven, in part, by a population of bright, blue galaxies in dense environments at z ∼ 1. This population, which lacks a counterpart at z ∼ 0, is thought to evolve into members of the red sequence from z ∼ 1 to ∼ 0. Finally, we conclude that environment does not play a dominant role in the cosmic star formation history at z < 1: the dependence of the mean galaxy SFR on local galaxy density at constant redshift is small compared to the decline in the global SFR space density over the last 7 Gyr.
• Dave, R., Ashby, M. L., Conselice, C. J., Cooray, A., Dekel, A., Dickinson, M., Faber, S. M., Fazio, G. G., Ferguson, H. C., Finkelstein, S. L., Giavalisco, M., Grogin, N. A., Guo, Y., Hathi, N. P., Huang, K., Kocevski, D. D., Koekemoer, A. M., Lai, K., Lee, K., , Lucas, R. A., et al. (2007). Luminous and High Stellar Mass Candidate Galaxies at z\approx8 Discovered in CANDELS. The Astrophysical Journal.
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  One key goal of the Hubble Space Telescope Cosmic Assembly Near-Infrared Deep Extragalactic Legacy Survey is to track galaxy evolution back to z ≈ 8. Its two-tiered “wide and deep” strategy bridges significant gaps in existing near-infrared surveys. Here we report on z ≈ 8 galaxy candidates selected as F105W-band dropouts in one of its deep fields, which covers∼ 62.9 arcmin to 4 ks per filter depth in the Great Observatories Origins Deep Survey southern field. We construct two independent samples using different but legitimate photometry and procedure. While they differ significantly on an object-by-object basis, our conclusions based on these two samples are similar. Two of our candidates have J 1 mag brighter than any previously known F105W-dropouts. We derive constraints on the bright-end of the rest-frame ultraviolet luminosity function of galaxies at z ≈ 8, and show that the number density of such very bright objects is higher than expected from the previous Schechter luminosity function estimates at this redshift. Another two candidates are securely detected in Spitzer Infrared Array Camera images. These are the first such detections at z ≈ 8. Their derived stellar masses are on the order of a few ×10 M⊙, from which we obtain the first measurement of the high-mass end of the galaxy stellar mass function at z ≈ 8. The high number density of very luminous and very massive galaxies at z ≈ 8, if real, could imply a large stellar-to-halo mass ratio and an efficient conversion of baryons to stars at such an early time. Subject headings: cosmology: observations — galaxies: luminosity function, mass function 1 Department of Physics & Astronomy, University of Missouri, Columbia, MO 65211, USA 2 Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, USA 3 Department of Physics & Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD, USA, 21218 4 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 5 National Optical Astronomy Observatory, 950 N. Cherry Ave., Tucson, AZ 85719, USA 6 Department of Physics and Astronomy, University of Pittsburgh, 3941 O’Hara Street, Pittsburgh, PA 15260, USA 7 Physics & Astronomy Department, Rutgers University, Piscataway, NJ 08854, USA 8 Astronomy Department, The University of Arizona, Tucson, AZ 85721, USA 9 University of California Observatories/Lick Observatory, University of California, Santa Cruz, CA 95064, USA 10 George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University, College Station, TX 778434242, USA 11 Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA 12 Department of Physics, Purdue University, 525 Northwestern Ave., West Lafayette, IN 47907, USA 13 Department of Physics & Astronomy, University of California, Riverside, CA 92521, USA 14 Deptment of Physics & Astronomy, University of California, Irvine, CA 92697 15 Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA 16 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS65, Cambridge, MA02138, USA 17 Steward Observatory, University of Arizona, 933 N. Cherry St., Tucson, AZ 85721, USA 18 Racah Institute of Physics, The Hebrew University of
• Davis, M., Guhathakurta, P., Konidaris, N. P., Newman, J. A., Ashby, M., Biggs, A. D., Barmby, P., Bundy, K., Chapman, S. C., Coil, A. L., Conselice, C. J., Cooper, M. C., Croton, D. J., Eisenhardt, P., Ellis, R. S., Faber, S. M., Fang, T., Fazio, G. G., Georgakakis, A., , Gerke, B. F., et al. (2007). The All-Wavelength Extended Groth Strip International Survey (AEGIS) data sets. ASTROPHYSICAL JOURNAL, 660(1), L1-L6.
• Faber, S. M., Willmer, C. N., Wolf, C., Koo, D. C., Weiner, B. J., Newman, J. A., Im, M., Coil, A. L., Conroy, C., Cooper, M. C., Davis, M., Finkbeiner, D. P., Gerke, B. F., Gebhardt, K., Groth, E. J., Guhathakurta, P., Harker, J., Kaiser, N., Kassin, S., , Kleinheinrich, M., et al. (2007). Galaxy luminosity functions to z∼ 1 from DEEP2 and COMBO-17: Implications for red galaxy formation. The Astrophysical Journal, 665(1), 265-294. doi:10.1086/519294
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  The DEEP2 and COMBO-17 surveys are compared to study luminosity functions of red and blue galaxies to z ~ 1. The two surveys have different methods and sensitivities, but nevertheless results agree. After z ~ 1, M has dimmed by 1.2-1.3 mag for all colors of galaxies, * for blue galaxies has hardly changed, and * for red galaxies has at least doubled (our formal value is ~0.5 dex). Luminosity density jB has fallen by 0.6 dex for blue galaxies but has remained nearly constant for red galaxies. These results imply that the number and total stellar mass of blue galaxies have been substantially constant since z ~ 1, whereas those of red galaxies (near L*) have been significantly rising. To explain the new red galaxies, a ``mixed'' scenario is proposed in which star formation in blue cloud galaxies is quenched, causing them to migrate to the red sequence, where they merge further in a small number of stellar mergers. This mixed scenario matches the local boxy-disky transition for nearby ellipticals, as well as red sequence stellar population scaling laws such as the color-magnitude and Mg-? relations (which are explained as fossil relics from blue progenitors). Blue galaxies enter the red sequence via different quenching modes, each of which peaks at a different characteristic mass and time. The red sequence therefore likely builds up in different ways at different times and masses, and the concept of a single process that is ``downsizing'' (or upsizing) probably does not apply. Our claim in this paper of a rise in the number of red galaxies applies to galaxies near L*. Accurate counts of brighter galaxies on the steep part of the Schechter function require more accurate photometry than is currently available.
• Faber, S. M., Willmer, C., Wolf, C., Koo, D. C., Weiner, B. J., Newman, J. A., Im, M., Coil, A. L., Conroy, C., Cooper, M. C., Davis, M., Finkbeiner, D. P., Gerke, B. F., Gebhardt, K., Groth, E. J., Guhathakurta, P., Harker, J., Kaiser, N., Kassin, S., , Kleinheinrich, M., et al. (2007). Galaxy luminosity functions to z similar to 1 from deep2 and combo-17: Implications for red galaxy formation. ASTROPHYSICAL JOURNAL, 665(1), 265-294.
• Gerke, B. F., Newman, J. A., Faber, S. M., Cooper, M. C., Croton, D. J., Davis, M., Willmer, C., Yan, R., Coil, A. L., Guhathakurta, P., Koo, D. C., & Weiner, B. J. (2007). The DEEP2 galaxy redshift survey: the evolution of the blue fraction in groups and the field. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 376(4), 1425-1444.
• Gerke, B. F., Newman, J. A., Lotz, J., Yan, R., Barmby, P., Coil, A. L., Conselice, C. J., Ivison, R. J., Lin, L., Koo, D. C., Nandra, K., Salim, S., Small, T., Weiner, B. J., Cooper, M. C., Davis, M., Faber, S. M., & Guhathakurta, P. (2007). The DEEP2 Galaxy Redshift Survey: AEGIS observations of a dual AGN at z=0.7. ASTROPHYSICAL JOURNAL, 660(1), L23-L26.
• Kassin, S. A., Weiner, B. J., Faber, S. M., Koo, D. C., & Lotz, J. M. (2007). The stellar mass tully-fisher relation to z=1.2. AT THE EDGE OF THE UNIVERSE: LATEST RESULTS FROM THE DEEPEST ASTRONOMICAL SURVEYS, 380, 477-482.
• Kassin, S. A., Weiner, B. J., Faber, S. M., Koo, D. C., Lotz, J. M., Diemand, J., Harker, J. J., Bundy, K., Metevier, A. J., Phillips, A. C., Cooper, M. C., Croton, D. J., Konidaris, N., Noeske, K. G., & Willmer, C. (2007). The stellar mass Tully-Fisher relation to z=1.2 from AEGIS. ASTROPHYSICAL JOURNAL, 660(1), L35-L38.
• Kirby, E. N., Guhathakurta, P., Faber, S. M., Koo, D. C., Weiner, B. J., & Cooper, M. C. (2007). The DEEP2 galaxy redshift survey: Redshift identification of single-line emission galaxies. Astrophysical Journal, 660(Issue 1 I). doi:10.1086/513464
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  We present two methods for determining spectroscopic redshifts of galaxies in the DEEP2 survey which display only one identifiable feature, an emission line, in the observed spectrum ("single-line galaxies"). First, we assume each single line is one of the four brightest lines accessible to DEEP2: Hα, [O III] λ5007, Hβ, or [O II] λ3727. Then, we supplement spectral information with BRI photometry. The first method, parameter-space proximity (PSP), calculates the distance of a single-line galaxy to galaxies of known redshift in (B - R), (R - I), R, λ observed parameter space. The second method is an artificial neural network (ANN). Prior information, such as allowable line widths and ratios, rules out one or more of the four lines for some galaxies in both methods. Based on analyses of evaluation sets, both methods are nearly perfect at identifying blended [O II] doublets. Of the lines identified as Hα in the PSP and ANN methods, 91.4% and 94.2%, respectively, are accurate. Although the methods are not this accurate at discriminating between [O III] and Hβ, they can identify a single line as one of the two, and the ANN method in particular unambiguously identifies many [O III] lines. From a sample of 640 single-line spectra, the methods determine the identities of 401 (62.7%) and 472 (73.8%) single lines, respectively, at accuracies similar to those found in the evaluation sets. © 2007. The American Astronomical Society. All rights reserved.
• Kirby, E. N., Guhathakurta, P., Faber, S. M., Koo, D. C., Weiner, B. J., & Cooper, M. C. (2007). The deep2 galaxy redshift survey: Redshift identification of single-line emission galaxies. ASTROPHYSICAL JOURNAL, 660(1), 62-71.
• Lin, L., Koo, D. C., Weiner, B. J., Chiueh, T., Coil, A. L., Lotz, J., Conselice, C. J., Willner, S. P., Smith, H. A., Guhathakurta, P., Huang, J., Le, F. E., Noeske, K. G., Willmer, C., Cooper, M. C., & Phillips, A. C. (2007). AEGIS: Enhancement of dust-enshrouded star formation in close galaxy pairs and merging galaxies up to z similar to 1. ASTROPHYSICAL JOURNAL, 660(1), L51-L54.
• Noeske, K. G., Faber, S. M., Weiner, B. J., Koo, D. C., Primack, J. R., Dekel, A., Papovich, C., Conselice, C. J., Le, F. E., Rieke, G. H., Coil, A. L., Lotz, J. M., Somerville, R. S., & Bundy, K. (2007). Star formation in AEGIS field galaxies since z=1.1: Staged galaxy formation and a model of mass-dependent gas exhaustion. ASTROPHYSICAL JOURNAL, 660(1), L47-L50.
• Noeske, K. G., Weiner, B. J., Faber, S. M., Papovich, C., Koo, D. C., Somerville, R. S., Bundy, K., Conselice, C. J., Newman, J. A., Schiminovich, D., Le, F. E., Coil, A. L., Rieke, G. H., Lotz, J. M., Primack, J. R., Barmby, P., Cooper, M. C., Davis, M., Ellis, R. S., , Fazio, G. G., et al. (2007). Star formation in AEGIS field galaxies since z=1.1: The dominance of gradually declining star formation, and the main sequence of star-forming galaxies. ASTROPHYSICAL JOURNAL, 660(1), L43-L46.
• Pierce, C. M., Lotz, J. M., Laird, E. S., Lin, L., Nandra, K., Primack, J. R., Faber, S. M., Barmby, P., Park, S. Q., Willner, S. P., Gwyn, S., Koo, D. C., Coil, A. L., Cooper, M. C., Georgakakis, A., Koekemoer, A. M., Noeske, K. G., Weiner, B. J., & Willmer, C. (2007). Aegis: Host galaxy morphologies of X-ray-selected and infrared-selected active galactic nuclei at 0.2 <= z < 1.2. ASTROPHYSICAL JOURNAL, 660(1), L19-L22.
• Weiner, B. J., Papovich, C., Bundy, K., Conselice, C. J., Cooper, M. C., Ellis, R. S., Ivison, R. J., Noeske, K. G., Phillips, A. C., & Yan, R. (2007). AEGIS: Extinction and Star Formation Tracers from Line Emission. Astrophys.J., 660.
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  Strong nebular emission lines are a sensitive probe of star formation andextinction in galaxies, and the [O II] line detects star forming populationsout to z>1. However, star formation rates from emission lines depend oncalibration of extinction and the [O II]/H-alpha line ratio, and separatingstar formation from AGN emission. We use calibrated line luminosities from theDEEP2 survey and Palomar K magnitudes to show that the behavior of emissionline ratios depends on galaxy magnitude and color. For galaxies on the blueside of the color bimodality, the vast majority show emission signatures ofstar formation, and there are strong correlations of extinction and [OII]/H-alpha with restframe H magnitude. The conversion of [O II] toextinction-corrected H-alpha and thus to star formation rate has a significantslope with M_H, 0.23 dex/mag. Red galaxies with emission lines have a muchhigher scatter in their line ratios, and more than half show AGN signatures. Weuse 24 micron fluxes from Spitzer/MIPS to demonstrate the differing populationsprobed by nebular emission and by mid-IR luminosity. Although extinction iscorrelated with luminosity, 98% of IR-luminous galaxies at z~1 are stilldetected in the [O II] line. Mid-IR detected galaxies are mostly bright andintermediate color, while fainter, bluer galaxies with high [O II] luminosityare rarely detected at 24 microns.[Journal_ref: Astrophys.J.660:L39-L42,2007]
• Weiner, B. J., Papovich, C., Bundy, K., Conselice, C. J., Cooper, M. C., Ellis, R. S., Ivison, R. J., Noeske, K. G., Phillips, A. C., & Yan, R. (2007). AEGIS: Extinction and star formation tracers from line emission. ASTROPHYSICAL JOURNAL, 660(1), L39-L42.
• Bundy, K., Ellis, R. S., Conselice, C. J., Taylor, J. E., Cooper, M. C., Willmer, C., Weiner, B. J., Coil, A. L., Noeske, K. G., & Eisenhardt, P. (2006). The mass assembly history of field galaxies: Detection of an evolving mass limit for starforming galaxies. ASTROPHYSICAL JOURNAL, 651(1), 120-141.
• Coil, A. L., Cooper, M. C., Davis, M., Faber, S. M., Graves, G. J., Harker, J., Konidaris, N. P., Koo, D. C., Newman, J. A., Schiavon, R. P., Weiner, B. J., Willmer, C. N., & Yan, R. (2006). The Deep2 Galaxy Redshift Survey: Mean Ages and Metallicities of Red Field Galaxies at Z ~; 0.9 from Stacked Keck/Deimos Spectra. Lawrence Berkeley National Laboratory, 651(Issue 2). doi:10.1086/509074
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  Version: Aug 29, 2006 A Preprint typeset using L TEX style emulateapj v. 04/21/05 THE DEEP2 GALAXY REDSHIFT SURVEY: MEAN AGES AND METALLICITIES OF RED FIELD GALAXIES AT Z ∼ 0.9 FROM STACKED KECK/DEIMOS SPECTRA 1 Ricardo P. Schiavon 2 , S. M. Faber 3 , Nicholas Konidaris 3 , Genevieve Graves 3 , Christopher N.A. Willmer 3,4 , Benjamin J. Weiner 5 , Alison L. Coil 4,6,8 , Michael C. Cooper 6 , Marc Davis 6 , Justin Harker 3 , David C. Koo 3 , Jeffrey A. Newman 6,7,8 & Renbin Yan 6 2 Department of Astronomy, University of Virginia, P.O. Box 3818, Charlottesville, VA 22903-0818 UCO/Lick Observatory/Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064 4 Steward Observatory, University of Arizona, Tucson, AZ 85721 5 Department of Astronomy, University of Maryland, College Park, MD 20742-2421 6 Department of Astronomy, University of California, Berkeley, 601 Campbell Hall, Berkeley, CA 94720-3411 7 Lawrence Berkeley National Laboratory, Berkeley, CA 94720 and 8 Hubble Fellow Version: Aug 29, 2006 ABSTRACT As part of the DEEP2 galaxy redshift survey, we analyze absorption line strengths in stacked Keck/DEIMOS spectra of red field galaxies with weak to no emission lines, at redshifts 0.7 ≤ z ≤ 1. Comparison with models of stellar population synthesis shows that red galaxies at z ∼ 0.9 have mean luminosity-weighted ages of the order of only 1 Gyr and at least solar metallicities. These ages cannot be reconciled with a scenario where all stars evolved passively after forming at very high z. Rather, a significant fraction of stars can be no more than 1 Gyr old, which means that some star formation in the stacked populations continued to at least z ∼ 1.2. Furthermore, a comparison of these distant galaxies with a local SDSS sample, using stellar populations synthesis models, shows that the drop in the equivalent width of Hδ from z ∼ 0.9 to 0.1 is less than predicted by passively evolving models. This admits of two interpretations: either each individual galaxy experiences continuing low-level star formation, or the red-sequence galaxy population from z ∼ 0.9 to 0.1 is continually being added to by new galaxies with younger stars. Subject headings: Galaxies: evolution — Galaxies: stellar content — Galaxies: distances and redshifts 1. INTRODUCTION The formation of early-type galaxies is one of the on- going riddles of modern cosmology. According to the leading models, massive early-type galaxies have been assembled hierarchically from the merging of less mas- sive structures. Because such mergers are seen locally to be accompanied by star formation (e.g., Schweizer & Seitzer 1992), one of the best ways to test the hierarchical formation paradigm is by determining the star formation history of early-type galaxies. This can be achieved by estimating the ages of stars in galaxies from their inte- grated light, through comparison with stellar population synthesis models. Several groups have attempted this from observations of distant massive galaxies (e.g., Le Borgne et al. 2006, Treu et al. 2005, Daddi et al. 2005, Longhetti et al. 2005, and references therein). However, spectroscopic dating of stellar populations older than ∼ 1 Gyr is best achieved by simultaneously matching the strengths of Balmer and metal lines in their integrated spectra, in order to break the age-metallicity degener- acy. So far, observational difficulties have prevented such detailed studies for all but local samples (e.g., Gonz´ lez a 1993, Trager et al. 2000, Kuntschner 2000, Caldwell et al. 2003, Eisenstein et al. 2003, Thomas et al. 2005, Schiavon 2006, and references therein). In this Letter we present the analysis of absorption line strengths measured in stacked integrated Keck/DEIMOS spectra of red galaxies with redshifts between 0.7 and 1, as part of the DEEP2 survey (Davis et al. 2003). We find that these galaxies have mean light-weighted single stellar population (SSP) ages of order only 1 Gyr and metallicities at least solar. Since these objects are ob- served several billion years after the big bang, this result suggests that stars populating these galaxies were formed during an extended period of time. 2. SAMPLE AND DATA The data used in this Letter consist of k-corrected U and B absolute magnitudes in the Vega system and 1- hour exposure Keck/DEIMOS (Faber et al. 2003) spec- tra from DEEP2 (Davis et al. 2003). Redshift deter- minations are described in Davis et al. (2003), and rest- frame M B magnitudes and U–B colors were derived from CFHT BRI photometry and redshifts by Willmer et al. (2006). The S/N of each 1-hour exposure spectrum is not high enough for accurate measurement of absorption line indices, so we stack spectra of hundreds of galaxies, selected in bins of color, luminosity, and redshift. 2.1. Sample Selection Based on observations taken at the W. M. Keck Observatory Our goal is to study the evolution of red-sequence galaxies, so we first select galaxies by color, as illustrated in left panel of Figure 1, where data for 17,745 DEEP2 galaxies with 0.7 ≤ z ≤ 1.05 were used to produce a contour plot in restframe color-magnitude space. Red- sequence galaxies (RSGs) are chosen to be those with U–B ≥ 0.25, making up a total of 1941 objects. Ideally, we would also like to select galaxies on the basis of mor- phology, but we lack that information for this sample. In order to minimize contamination by reddened late-
• Cooper, M. C., Newman, J. A., Croton, D. J., Weiner, B. J., Willmer, C., Gerke, B. F., Madgwick, D. S., Faber, S. M., Davis, M., Coil, A. L., Finkbeiner, D. P., Guhathakurta, P., & Koo, D. C. (2006). The DEEP2 Galaxy Redshift Survey: the relationship between galaxy properties and environment at z similar to 1. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 370(1), 198-212.
• Harker, J. J., Schiavon, R. P., Weiner, B. J., & Faber, S. M. (2006). Population Synthesis Models for Late Build-Up of the Red Sequence. Astrophys.J., 647.
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  We present population synthesis models designed to represent the starformation histories of L* red sequence galaxies (RSGs). Earlier work has shownthat single-burst stellar populations (SSPs) are unable to match Balmer linestrengths simultaneously at high and low redshift. We therefore consideralternative star formation histories in which RSGs contain intermediate-agedstars even at late epochs. The models are compared to Balmer Hdelta absorptionstrengths, U-B color data, and the number density of red sequence galaxies fromz=1 to z=0. We find that quenched models (which consist of constant starformation histories truncated at regularly-spaced intervals) average to an RSGpopulation that matches the data well, showing slow evolution in color andBalmer line strength and a rise in number density by a factor of a few afterz=1. The data are best fit by a turn-on of quenching at redshifts z=1.5-2.[Journal_ref: Astrophys.J.647:L103-L106,2006]
• Harker, J. J., Schiavon, R. P., Weiner, B. J., & Faber, S. M. (2006). Population synthesis models for late buildup of the red sequence. ASTROPHYSICAL JOURNAL, 647(2), L103-L106.
• Jong, R. S., Kassin, S. A., & Weiner, B. J. (2006). Dark and Baryonic Matter in Bright Spiral Galaxies. II. Radial Distributions for 34 Galaxies. The Astrophysical Journal, 643(2), 804-824. doi:10.1086/502959
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  We decompose the rotation curves of 34 bright spiral galaxies into baryonic and dark matter components. Stellar mass profiles are created by applying color-M/L relations to near-infrared and optical photometry. We find that the radial profile of the baryonic-to-dark-matter ratio is self-similar for all galaxies, when scaled to the radius at which the contribution of the baryonic mass to the rotation curve equals that of the dark matter (RX). We argue that this is due to the quasi-exponential nature of disks and rotation curves that are nearly flat after an initial rise. The radius RX is found to correlate most strongly with baryonic rotation speed, such that galaxies with RX measurements that lie further out in their disks rotate faster. This quantity also correlates very strongly with stellar mass, Hubble type, and observed rotation speed; B-band central surface brightness is less related to RX than these other galaxy properties. Most of the galaxies in our sample appear to be close to maximal disk. For these galaxies, we find that maximum observed rotation speeds are tightly correlated with maximum rotation speeds predicted from the baryon distributions, such that one can create a Tully-Fisher relation based on surface photometry and redshifts alone. Finally, we compare our data to the NFW parameterization for dark matter profiles with and without including adiabatic contraction as it is most commonly implemented. Fits are generally poor, and all but two galaxies are better fit if adiabatic contraction is not performed. In order to have better fits, and especially to accommodate adiabatic contraction, baryons would need to contribute very little to the total mass in the inner parts of galaxies, seemingly in contrast with other observational constraints.
• Kassin, S. A., de Jong, R. S., & Weiner, B. J. (2006). Dark and Baryonic Matter in Bright Spiral Galaxies: II. Radial Distributions for 34 Galaxies. Astrophys.J., 804-824.
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  We decompose the rotation curves of 34 bright spiral galaxies into baryonicand dark matter components. Stellar mass profiles are created by applyingcolor-M/L relations to near-infrared and optical photometry. We find that theradial profile of the baryonic-to-dark-matter ratio is self-similar for allgalaxies, when scaled to the radius where the contribution of the baryonic massto the rotation curve equals that of the dark matter (R_X). We argue that thisis due to the quasi-exponential nature of disks and rotation curves that arenearly flat after an initial rise. The radius R_X is found to correlate moststrongly with baryonic rotation speed, such that galaxies with R_X measurementsthat lie further out in their disks rotate faster. This quantity alsocorrelates very strongly with stellar mass, Hubble type, and observed rotationspeed; B-band central surface brightness is less related to R_X than theseother galaxy properties. Most of the galaxies in our sample appear to be closeto maximal disk. For these galaxies, we find that maximum observed rotationspeeds are tightly correlated with maximum rotation speeds predicted from thebaryon distributions, such that one can create a Tully-Fisher relation based onsurface photometry and redshifts alone. Finally, we compare our data to the NFWparameterization for dark matter profiles with and without including adiabaticcontraction as it is most commonly implemented. Fits are generally poor, andall but 2 galaxies are better fit if adiabatic contraction is not performed. Inorder to have better fits, and especially to accommodate adiabatic contraction,baryons would need to contribute very little to the total mass in the innerparts of galaxies, seemingly in contrast with other observational constraints.[Journal_ref: Astrophys.J. 643 (2006) 804-824]
• Prochaska, J. X., Weiner, B. J., Chen, H., & Mulchaey, J. S. (2006). Probing the intergalactic medium-galaxy connection toward PKS 0405-123. III. The galaxy survey and correlations with OVI absorbers. ASTROPHYSICAL JOURNAL, 643(2), 680-691.
• Schiavon, R. P., Faber, S. M., Konidaris, N., Graves, G., Willmer, C., Weiner, B. J., Coil, A. L., Cooper, M. C., Davis, M., Harker, J., Koo, D. C., Newman, J. A., & Yan, R. (2006). The DEEP2 galaxy redshift survey: Mean ages and metallicities of red field galaxies at z similar to 0.9 from stacked Keck DEIMOS spectra. ASTROPHYSICAL JOURNAL, 651(2), L93-L96.
• Weiner, B. J., Willmer, C. N., Faber, S. M., Harker, J., Kassin, S. A., Phillips, A. C., Melbourne, J., Metevier, A. J., Vogt, N. P., & Koo, D. C. (2006). A Survey of Galaxy Kinematics to z ~ 1 in the TKRS/GOODS-N Field. II. Evolution in the Tully-Fisher Relation. Astrophys.J., 653, 1049-1069.
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  We use kinematic measurements of a large sample of galaxies from the TeamKeck Redshift Survey in the GOODS-N field to measure evolution in the opticaland near-IR Tully-Fisher relations to z = 1.2. We construct Tully-Fisherrelations with integrated line-of-sight velocity widths of ~ 1000 galaxies in Band ~ 670 in J-band; these relations have large scatter, and we derive amaximum-likelihood least squares method for fitting in the presence of scatter.The B-band Tully-Fisher relations, from z=0.4 to z=1.2, show evolution of ~1.0-1.5 mag internal to our sample without requiring calibration to a local TFrelation. There is evolution in both Tully-Fisher intercept and slope,suggesting differential luminosity evolution. In J-band, there is evolution inslope but little evolution in overall luminosity. The slope measurements implythat bright, massive blue galaxies fade {\it more strongly} than fainter bluegalaxies from z ~ 1.2 to now. This conclusion runs counter to some previousmeasurements and to our naive expectations, but we present a simple set of starformation histories to show that it arises naturally if massive galaxies haveshorter timescales of star formation, forming most of their stars before z ~ 1,while less massive galaxies form stars at more slowly declining rates. Thismodel predicts that the higher global star formation rate at z ~ 1 is mostlydue to higher SFR in massive galaxies. The amount of fading in B-bandconstrains star formation timescale more strongly than redshift of formation.Tully-Fisher and color-magnitude relations can provide global constraints onthe luminosity evolution and star formation history of blue galaxies.[Journal_ref: Astrophys.J.653:1049-1069,2006]
• Weiner, B. J., Willmer, C. N., Faber, S. M., Melbourne, J., Kassin, S. A., Phillips, A. C., Harker, J., Metevier, A. J., Vogt, N. P., & Koo, D. C. (2006). A Survey of Galaxy Kinematics to z ~ 1 in the TKRS/GOODS-N Field. I. Rotation and Dispersion Properties. Astrophys.J., 653, 1027-1048.
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  We present kinematic measurements of a large sample of galaxies from the TKRSSurvey in the GOODS-N field. We measure line-of-sight velocity dispersions fromintegrated emission for 1089 galaxies with median z=0.637, and spatiallyresolved kinematics for a subsample of 380 galaxies. This is the largest sampleof galaxies to z ~ 1 with kinematics to date, and allows us to measurekinematic properties without morphological pre-selection. Emission linewidthsprovide kinematics for the bulk of blue galaxies. To fit the spatially resolvedkinematics, we fit models with both line-of-sight rotation amplitude andvelocity dispersion. Integrated linewidth correlates well with a combination ofthe rotation gradient and dispersion, and is a robust measure of galaxykinematics. The spatial extents of emission and continuum are similar and thereis no evidence that linewidths are affected by nuclear or clumpy emission. Themeasured rotation gradient depends strongly on slit PA alignment with galaxymajor axis, but integrated linewidth does not. Even for galaxies withwell-aligned slits, some have kinematics dominated by dispersion (V/sigma
• Weiner, B. J., Willmer, C., Faber, S. M., Harker, J., Kassin, S. A., Phillips, A. C., Melbourne, J., Metevier, A. J., Vogt, N. P., & Koo, D. C. (2006). A survey of galaxy kinematics to z similar to 1 in the TKRS/GOODS-N field. II. Evolution in the Tully-Fisher relation. ASTROPHYSICAL JOURNAL, 653(2), 1049-1069.
• Weiner, B. J., Willmer, C., Faber, S. M., Melbourne, J., Kassin, S. A., Phillips, A. C., Harker, J., Metevier, A. J., Vogt, N. P., & Koo, D. C. (2006). A survey of galaxy kinematics to z similar to 1 in the TKRS/GOODS-N field. I. Rotation and dispersion properties. ASTROPHYSICAL JOURNAL, 653(2), 1027-1048.
• Willmer, C., Faber, S. M., Koo, D. C., Weiner, B. J., Newman, J. A., Coil, A. L., Connolly, A. J., Conroy, C., Cooper, M. C., Davis, M., Finkbeiner, D. P., Gerke, B. F., Guhathakurta, P., Harker, J., Kaiser, N., Kassin, S., Konidaris, N. P., Lin, L., Luppino, G., , Madgwick, D. S., et al. (2006). The deep evolutionary exploratory probe 2 galaxy redshift survey: The galaxy luminosity function to z similar to 1. ASTROPHYSICAL JOURNAL, 647(2), 853-873.
• Blandford, R., Brunner, R. J., Connolly, A. J., Faber, S. M., Gebhardt, K., Gronwall, C., Groth, E. J., Guzman, R., Illingworth, G. D., Im, M., Koo, D. C., Kron, R. G., Phillips, A. C., Rhodes, J., Sarajedini, V. L., Simard, L., Szalay, A. S., Vogt, N. P., Weiner, B. J., , Willmer, C. N., et al. (2005). The DEEP Groth Strip Survey. I. The Sample. Astrophysical Journal Supplement Series, 159(1), 41-59. doi:10.1086/430313
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  The Deep Extragalactic Exploratory Probe (DEEP) is a multiphase research program dedicated to the study of the formation and evolution of galaxies and of large-scale structure in the distant universe. This paper describes the first five-year phase, denoted DEEP1. A series of 10 DEEP1 papers will discuss a range of scientific topics (e.g., the study of photometric and spectral properties of a general distant galaxy survey, the evolution observed in galaxy populations of varied morphologies). The observational basis for these studies is the Groth Survey Strip field, a 127 arcmin2 region that has been observed with the Hubble Space Telescope (HST) in both broad I-band and V-band optical filters and with the Low Resolution Imaging Spectrograph on the Keck Telescopes. Catalogs of photometric and structural parameters have been constructed for 11,547 galaxies and stars at magnitudes brighter than 29, and spectroscopy has been conducted for a magnitude-color weighted subsample of 818 objects. We evaluate three independent techniques for constructing an imaging catalog for the field from the HST data and discuss the depth and sampling of the resultant catalogs. The selection of the spectroscopic subsample is discussed, and we describe the multifaceted approach taken to prioritizing objects of interest for a variety of scientific subprograms. A series of Monte Carlo simulations then demonstrates that the spectroscopic subsample can be adequately modeled as a simple function of magnitude and color cuts in the imaging catalog.
• Chen, H. W., Prochaska, J. X., Weiner, B. J., Mulchaey, J. S., & Williger, G. M. (2005). Probing the Intergalactic Medium-Galaxy Connection toward PKS 0405–123. II. A Cross-Correlation Study of Lyα Absorbers and Galaxies at z < 0.5*. The Astrophysical Journal, 629(1), L25-L28. doi:10.1086/444377
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  We present a pilot study of the clustering properties of Lyα absorbers with respect to known galaxies based on 112 Lyα absorbers and 482 galaxies identified at z < 0.5 along the sight line toward PKS 0405-123. The principal goal is to determine the origin of Lyα absorbers based on their cross-correlation amplitude with known galaxies and to investigate a possible N(H I) dependence of the cross-correlation function. The main results of our study are as follows: (1) The cross-correlation function ξga measured using only emission-line-dominated galaxies and Lyα absorbers with log N(H I) ≥ 14 shows a comparable strength to the galaxy autocorrelation function ξgg on comoving, projected distance scales of less than 1 h-1 Mpc, while there remains a lack of cross-correlation signal when using only absorption-line-dominated galaxies. This signifies a morphology-dependent ξga and indicates that strong absorbers with log N(H I) ≥ 14 and emission-line galaxies reside in the same halo population. (2) A maximum likelihood analysis shows that Lyα absorbers with log N(H I) < 13.6 are consistent with being more randomly distributed with respect to known galaxies. (3) Finally, we find based on this single sight line that the amplitude of ξga does not depend sensitively on N(H I) for strong absorbers, with log N(H I) ≥ 13.6.
• Gerke, B. F., Newman, J. A., Davis, M., Marinoni, C., Yan, R., Coil, A. L., Conroy, C., Cooper, M. C., Faber, S. M., Finkbeiner, D. P., Guhathakurta, P., Kaiser, N., Koo, D. C., Phillips, A. C., Weiner, B. J., & Willmer, C. N. (2005). The DEEP2 Galaxy Redshift Survey: First results on galaxy groups. The Astrophysical Journal, 625(1), 6-22. doi:10.1086/429579
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  We use the first 25% of the DEEP2 Galaxy Redshift Survey spectroscopic data to identify groups and clusters of galaxies in redshift space. The data set contains 8370 galaxies with confirmed redshifts in the range 0.7 ≤ z ≤ 1.4, over 1 deg2 on the sky. Groups are identified using an algorithm (the Voronoi-Delaunay method) that has been shown to accurately reproduce the statistics of groups in simulated DEEP2-like samples. We optimize this algorithm for the DEEP2 survey by applying it to realistic mock galaxy catalogs and assessing the results using a stringent set of criteria for measuring group-finding success, which we develop and describe in detail here. We find in particular that the group finder can successfully identify ~78% of real groups and that ~79% of the galaxies that are true members of groups can be identified as such. Conversely, we estimate that ~55% of the groups we find can be definitively identified with real groups and that ~46% of the galaxies we place into groups are interloper field galaxies. Most importantly, we find that it is possible to measure the distribution of groups in redshift and velocity dispersion, n(σ, z), to an accuracy limited by cosmic variance, for dispersions greater than 350 km s-1. We anticipate that such measurements will allow strong constraints to be placed on the equation of state of the dark energy in the future. Finally, we present the first DEEP2 group catalog, which assigns 32% of the galaxies to 899 distinct groups with two or more members, 153 of which have velocity dispersions above 350 km s-1. We provide locations, redshifts and properties for this high-dispersion subsample. This catalog represents the largest sample to date of spectroscopically detected groups at z ~ 1.
• Koo, D. C., Simard, L., Willmer, C. N., Gebhardt, K., Bouwens, R. J., Kauffmann, G., Crosby, T., Faber, S. M., Harker, J., Sarajedini, V. L., Vogt, N. P., Weiner, B. J., Phillips, A. J., Myungshin, I. M., & Wu, K. L. (2005). The DEEP groth strip survey - VIII. The evolution of luminous field bulges at redshift z ~ 1. Astrophysical Journal Supplement Series, 157(2), 175-217. doi:10.1086/427845
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  We present a candidate sample of luminous bulges (including ellipticals) found within the Groth Strip Survey (GSS), with spectroscopic redshifts of 0.73 1.5. Only small amounts of residual star formation are needed to explain both the absence of bluening of bulges to today and the presence of emission lines seen in the Keck spectra of the very red distant galaxies.
• Weiner, B. J., Phillips, A. C., Faber, S. M., Willmer, C. N., Vogt, N. P., Simard, L., Geshardi, K., Im, M., Koo, D. C., Sarajedini, V. L., Wu, K. L., Forbes, D. A., Gronwall, C., Groth, E. J., Illingworth, G. D., Kron, R. G., Rhodes, J., Szalay, A. S., & Takamiya, M. (2005). THE DEEP GROTH STRIP GALAXY REDSHIFT SURVEY. III. REDSHIFT CATALOG AND PROPERTIES OF GALAXIES. The Astrophysical Journal, 620(2), 595-617. doi:10.1086/427256
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  The Deep Extragalactic Evolutionary Probe (DEEP) is a series of spectroscopic surveys of faint galaxies, targeted at understanding the properties and clustering of galaxies at redshifts z ~ 1. We present the redshift catalog of the DEEP1 Groth Strip pilot phase of this project, a Keck LRIS survey of faint galaxies in the Groth Survey Strip imaged with HST WFPC2. The redshift catalog and data, including reduced spectra, are made publicly available through a Web-accessible database. The catalog contains 658 secure galaxy redshifts with a median z = 0.65. The distribution of these galaxies shows large-scale structure walls to z ~ 1. We find a bimodal distribution in the galaxy color-magnitude diagram that persists to the same distance. A similar color division has been seen locally by the SDSS and to z ~ 1 by the COMBO-17 survey. The HST imaging allows us to measure structural properties of the galaxies, and we find that the color division corresponds generally to a structural division. Most red galaxies, ~75%, are centrally concentrated, with a red bulge or spheroidal stellar component, while blue galaxies usually have exponential profiles. However, there are two subclasses of red galaxies that are not bulge dominated: edge-on disks and a second category that we term diffuse red galaxies (DIFRGs). Comparison to a local sample drawn from the RC3 suggests that distant edge-on disks are similar in appearance and frequency to those at low redshift, but analogs of DIFRGs are rare among local red galaxies. DIFRGs have significant emission lines, indicating that they are reddened mainly by dust rather than age. The DIFRGs in our sample are all at z > 0.64, suggesting that DIFRGs are more prevalent at high redshifts; they may be related to the dusty or irregular extremely red objects beyond z > 1.2 that have been found in deep K-selected surveys. We measure the color evolution of both red and blue galaxies by comparing our U - B colors to those from the RC3. For red galaxies, we find a reddening of only 0.11 mag from z ~ 0.8 to now, about half the color evolution measured by COMBO-17. Larger, more carefully defined samples with better colors are needed to improve this measurement. Reconciling evolution in color, luminosity, mass, morphology, and star formation rates will be an active topic of future research.
• Chen, H., Howk, J. C., Mulchaey, J. S., Prochaska, J. X., & Weiner, B. J. (2004). Probing the Intergalactic Medium-Galaxy Connection toward PKS 0405–123. I. Ultraviolet Spectroscopy and Metal-Line Systems. The Astrophysical Journal, 617(2), 718-745. doi:10.1086/425558
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  We present results from an analysis of FUSE spectroscopy of the zem = 0.57 quasar PKS 0405-123. We focus on the intervening metal-line systems identified along the sight line and investigate their ionization mechanism, ionization state, and chemical abundances. Including Hubble Space Telescope STIS spectroscopy, we survey the entire sight line and identify six O VI absorbers to a 3 σ equivalent width (EW) limit of 60 mA. This implies an incidence dN/dz = 16 consistent with previous O VI studies. In half of the O VI systems we report positive detections of C III, suggesting that the gas is predominantly photoionized, has multiple ionization phases, or is in a nonequilibrium state. This contrasts with the general description of the warm-hot intergalactic medium (WHIM) as described by numerical simulations in which the gas is predominantly in collisional ionization equilibrium. An appreciable fraction of O VI absorbers may therefore have a different origin. We have also searched the sight line for the Ne VIII doublet (a better probe of the WHIM at T > 106 K) over the redshift range 0.2 1014 cm-2 is [M/H] > -1.5, with large scatter. This significantly exceeds the median metallicity of C IV and O VI systems at z ~ 3 and indicates enrichment of the intergalactic medium over the past ≈10 Gyr.
• Coil, A. L., Davis, M., Madgwick, D. S., Newman, J. A., Conselice, C. J., Cooper, M., Ellis, R. S., Faber, S. M., Finkbeiner, D. P., Guhathakurta, P., Kaiser, N., Koo, D. C., Phillips, A. C., Steidel, C. C., Weiner, B. J., Willmer, C. N., & Yan, R. (2004). The DEEP2 Galaxy Redshift Survey: Clustering of Galaxies in Early Data. The Astrophysical Journal, 609(2), 525-538. doi:10.1086/421337
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  We measure the two-point correlation function ξ(rp, π) in a sample of 2219 galaxies between z = 0.7 and 1.35 to a magnitude limit of RAB = 24.1 from the first season of the DEEP2 Galaxy Redshift Survey. From ξ(rp, π) we recover the real-space correlation function, ξ(r), which we find can be approximated within the errors by a power law, ξ(r) = (r/r0)-γ, on scales ~0.1-10 h-1 Mpc. In a sample with an effective redshift of zeff = 0.82, for a ΛCDM cosmology we find r0 = 3.53 ± 0.81 h-1 Mpc (comoving) and γ = 1.66 ± 0.12, while in a higher redshift sample with zeff = 1.14 we find r0 = 3.12 ± 0.72 h-1 Mpc and γ = 1.66 ± 0.12. These errors are estimated from mock galaxy catalogs and are dominated by the cosmic variance present in the current data sample. We find that red, absorption-dominated, passively evolving galaxies have a larger clustering scale length, r0, than blue, emission-line, actively star-forming galaxies. Intrinsically brighter galaxies also cluster more strongly than fainter galaxies at z 1. Our results imply that the DEEP2 galaxies have an effective bias b = 0.96 ± 0.13 if σ8DM = 1 today or b = 1.19 ± 0.16 if σ8DM = 0.8 today. This bias is lower than that predicted by semianalytic simulations at z 1, which may be the result of our R-band target selection. We discuss possible evolutionary effects within our survey volume, and we compare our results with galaxy-clustering studies at other redshifts, noting that our star-forming sample at z 1 has selection criteria very similar to the Lyman break galaxies at z 3 and that our red, absorption-line sample displays a clustering strength comparable to the expected clustering of the Lyman break galaxy descendants at z 1. Our results demonstrate that galaxy-clustering properties as a function of color, spectral type, and luminosity seen in the local universe were largely in place by z 1.
• Kobulnicky, H. A., Willmer, C. N., Phillips, A. C., Koo, D. C., Faber, S. M., Weiner, B. J., Sarajedini, V. L., Simard, L., & Vogt, N. P. (2004). Erratum: “The DEEP Groth Strip Survey. VII. The Metallicity of Field Galaxies at 0.26 < z < 0.82 and the Evolution of the Luminosity-Metallicity Relation” (ApJ, 599, 1006 [2003]). The Astrophysical Journal, 610(2), 1234-1237. doi:10.1086/422574
• Weiner, B. J. (2004). The dark matter density problem in massive disk galaxies. Symposium - International Astronomical Union, 220, 265-270. doi:10.1017/s0074180900183342
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  I discuss measurements of disk mass from non-circular streaming motions of gas in the barred galaxies NGC 3095 and NGC 4123. In these galaxies with strong shocks and non-circular motions, the inner regions must be disk-dominated to reproduce the shocks. This requires dark matter halos of low central density and low concentration, compared to LCDM halo predictions. In addition, the baryonic collapse to a disk should have compressed the halo and increased the dark matter density, which sharpens the disagreement. One possible resolution is a substantial amount of angular momentum transfer from disk to halo, but this is not particularly attractive nor elegant.
• Coil, A. L., Conselice, C. J., Cooper, M. C., Davis, M., Ellis, R. S., Faber, S. M., Finkbeiner, D. P., Gerke, B. F., Guhathakurta, P., Kaiser, N., Koo, D. C., Madgwick, D. S., Newman, J. A., Phillips, A. C., Steidel, C. C., Weiner, B. J., Willmer, C. N., & Yan, R. (2003). The DEEP2 Galaxy Redshift Survey: Spectral Classification of Galaxies at z ∼ 1. The Astrophysical Journal, 599(2), 997-1005. doi:10.1086/379626
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  We present a principal component analysis (PCA)-based spectral classification, η, for the first 5600 galaxies observed in the DEEP2 Redshift Survey. This parameter provides a very pronounced separation between absorption- and emission-dominated galaxy spectra—corresponding to passively evolving and actively star-forming galaxies in the survey, respectively. In addition it is shown that, despite the high resolution of the observed spectra, this parameter alone can be used to quite accurately reconstruct any given galaxy spectrum, suggesting there are not many "degrees of freedom" in the observed spectra of this galaxy population. It is argued that this form of classification, η, will be particularly valuable in making future comparisons between high- and low-redshift galaxy surveys for which very large spectroscopic samples are now readily available, particularly when used in conjunction with high-resolution spectral synthesis models, which will be made public in the near future. We also discuss the relative advantages of this approach to distant galaxy classification compared to other methods such as colors and morphologies. Finally, we compare the classification derived here with that adopted for the 2dF Galaxy Redshift Survey and in so doing show that the two systems are very similar. This will be particularly useful in subsequent analyses when making comparisons between results from each of these surveys to study evolution in the galaxy populations and large-scale structure.
• Davis, M., Faber, S. M., Newman, J. A., Phillips, A. C., Ellis, R. S., Steidel, C. C., Conselice, C., Coil, A. L., Finkbeiner, D. P., Koo, D. C., Guhathakurta, P., Weiner, B., Schiavon, R., Willmer, C., Kaiser, N., Luppino, G., Wirth, G., Connolly, A., Eisenhardt, P., , Cooper, M., et al. (2003). Science objectives and early results of the DEEP2 Redshift Survey. DISCOVERIES AND RESEARCH PROSPECTS FROM 6- TO 10- METER-CLASS TELESCOPES II, 4834, 161-172.
• Faber, S. M., Kobulnicky, H. A., Koo, D. C., Phillips, A. C., Sarajedini, V. L., Simard, L., Vogt, N. P., Weiner, B. J., & Willmer, C. N. (2003). The DEEP Groth Strip Survey. VII. The Metallicity of Field Galaxies at 0.26 < z < 0.82 and the Evolution of the Luminosity-Metallicity Relation. The Astrophysical Journal, 599(2), 1006-1030. doi:10.1086/379360
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  Using spectroscopic data from the Deep Extragalactic Evolutionary Probe Groth Strip Survey (DGSS), we analyze the gas-phase oxygen abundances in the warm ionized medium for 64 emission-line field galaxies in the redshift range 0.26 -19) end of the sample and is vanishingly small for objects at the high-luminosity end of the sample (MB ~ -22). We compare these data to simple single-zone, exponential-infall PEGASE2 models, which follow the chemical and luminous evolution of galaxies from formation to z = 0. A narrow range of model parameters can qualitatively produce the slope of the L-Z relation and the observed evolution of slope and zero point with redshift when at least two of the following are true: (1) low-mass galaxies have lower effective chemical yields than massive galaxies, (2) low-mass galaxies assemble on longer timescales than massive galaxies, and (3) low-mass galaxies begin the assembly process at a later epoch than massive galaxies. The single-zone models do a reasonable job of reproducing the observed evolution for the low-luminosity galaxies (MB ~ -19) in our sample but fail to predict the relative lack of evolution in the L-Z plane observed for the most luminous galaxies (MB ~ -22). More realistic multizone models will be required to explain the chemoluminous evolution of large galaxies.
• Gebhardt, K., Faber, S. M., Koo, D. C., Im, M., Simard, L., Illingworth, G. D., Phillips, A. C., Sarajedini, V. L., Vogt, N. P., Weiner, B., & Willmer, C. (2003). The deep Groth Strip survey. IX. Evolution of the fundamental plane of field galaxies. ASTROPHYSICAL JOURNAL, 597(1), 239-262.
• Faber, S. M., Illingworth, G. D., Im, M., Koo, D. C., Phillips, A. C., Sarajedini, V. L., Simard, L., Vogt, N. P., Weiner, B. J., & Willmer, C. N. (2002). The DEEP Groth Strip Survey. II. Hubble Space Telescope Structural Parameters of Galaxies in the Groth Strip. Astrophysical Journal Supplement Series, 142(1), 1-33. doi:10.1086/341399
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  The quantitative morphological classification of distant galaxies is essential to the understanding of the evolution of galaxies over the history of the universe. This paper presents Hubble Space Telescope WFPC2 F606W and F814W photometric structural parameters for 7450 galaxies in the Groth Strip. These parameters are based on a two-dimensional bulge + disk surface brightness model and were obtained using an automated reduction and analysis pipeline described in detail here. A first set of fits was performed separately in each bandpass, and a second set of fits was performed simultaneously on both bandpasses. The information produced by these two types of fits can be used to explore different science goals. Systematic and random fitting errors in all structural parameters as well as bulge and disk colors are carefully characterized through extensive sets of simulations. The results of these simulations are given in catalogs similar to the real science catalogs so that both real and simulated measurements can be sampled according to the same selection criteria to show biases and errors in the science data subset of interest. The effects of asymmetric structures on the recovered bulge+disk fitting parameters are also explored through simulations. The full multidimensional photometric survey selection function of the Groth Strip is also computed. This selection function, coupled to bias maps from simulations, provides a complete and objective reproduction of the observational limits, and these limits can be applied to theoretical predictions from galaxy evolution models for direct comparisons with the data.
• Gorkom, J. H., Sellwood, J. A., Weiner, B. J., & Williams, T. B. (2001). The Disk and Dark Halo Mass of the Barred Galaxy NGC 4123. I. Observations. The Astrophysical Journal, 546(2), 916-930. doi:10.1086/318288
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  The noncircular streaming motions in barred galaxies are sensitive to the mass of the bar and can be used to lift the degeneracy between disk and dark matter halo encountered when fitting axisymmetric rotation curves of disk galaxies. In this paper we present photometric and kinematic observations of NGC 4123, a barred galaxy of modest size (Vrot = 130 km s-1, L = 0.7L*), that reveal strong noncircular motions. The bar has straight dust lanes and an inner Lindblad resonance. The disk of NGC 4123 has no sign of truncation out to 10 scale lengths, and star-forming regions are found well outside R25. A Fabry-Perot Hα velocity field shows velocity jumps of greater than 100 km s-1 at the location of the dust lanes within the bar, indicating shocks in the gas flow. VLA observations yield the velocity field of the H I disk. Axisymmetric mass models yield good fits to the rotation curve outside the bar region for disk I-band M/L of 2.25 or less, and dark halos with either isothermal or power-law profiles can fit the data well. In a companion paper we model the full two-dimensional velocity field, including noncircular motions, to determine the stellar M/L and the mass of the dark halo.
• Sellwood, J. A., Weiner, B. J., & Williams, T. B. (2001). The Disk and Dark Halo Mass of the Barred Galaxy NGC 4123. II. Fluid-Dynamical Models. The Astrophysical Journal, 546(2), 931-951. doi:10.1086/318289
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  We report a dynamical determination of the separate contributions of disk and dark halo masses to the rotation curve of a spiral galaxy. We use fluid-dynamical models of gas flow in the barred galaxy NGC 4123 to constrain the dynamical properties of the galaxy: disk M/L, bar pattern speed, and the central density and scale radius of the dark halo. We derive a realistic barred potential directly from the light distribution. For each model we assume a value of the stellar M/L and a bar pattern speed Ωp and add a dark halo to fit the rotation curve. We then compute the gas flow velocities with a two-dimensional gasdynamical code and compare the model flow patterns to a two-dimensional velocity field derived from Fabry-Perot observations. The strong shocks and noncircular motions in the observed gas flow require a high stellar M/L and a fast-rotating bar. Models with I-band disk M/L of 2.0-2.5 h75, or 80%-100% of the maximum disk value, are highly favored. The corotation radius of the bar must be ≤1.5 times the bar semimajor axis. These results contradict some recent claimed "universal" galaxy disk/halo relations, since NGC 4123 is of modest size (rotation curve maximum 145 km s-1 and Vflat = 130 km s-1) yet quite disk-dominated. The dark halo of NGC 4123 is less concentrated than favored by current models of dark halos based on cosmological simulations. Since some 30% of bright disk galaxies are strongly barred and have dust lanes indicating shock morphology similar to that of NGC 4123, it is likely that they also have high stellar M/L and low-density halos. We suggest that luminous matter dominates inside the optical radius R25 of high surface brightness disk galaxies.
• Weiner, B. J., Sellwood, J. A., & Williams, T. B. (2001). The Disk and Dark Halo Mass of the Barred Galaxy NGC 4123. II. Fluid-Dynamical Models. Astrophys.J., 546, 931-951.
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  We report a dynamical determination of the separate contributions of disk anddark halo masses to the rotation curve of a spiral galaxy. We usefluid-dynamical models of gas flow in the barred galaxy NGC 4123 to constrainthe dynamical properties of the galaxy: disk M/L, bar pattern speed, and thecentral density and scale radius of the dark halo. We derive a realistic barredpotential directly from the light distribution. For each model we assume avalue of the stellar M/L and a bar pattern speed Omega_p and add a dark halo tofit the rotation curve. We then compute the gas flow velocities with a 2-D gasdynamical code, and compare the model flow patterns to a 2-D velocity fieldderived from Fabry-Perot observations. The strong shocks and non-circularmotions in the observed gas flow require a high stellar M/L and a fast-rotatingbar. Models with I-band disk M/L of 2.0 -- 2.5 h_75, or 80 -- 100% of themaximum disk value, are highly favored. The corotation radius of the bar mustbe
• Weiner, B. J., Williams, T. B., Gorkom, V. J., & Sellwood, J. A. (2001). The Disk and Dark Halo Mass of the Barred Galaxy NGC 4123. I. Observations. Astrophys.J., 546, 916-930.
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  The non-circular streaming motions in barred galaxies are sensitive to themass of the bar and can be used to lift the degeneracy between disk and darkmatter halo encountered when fitting axisymmetric rotation curves of diskgalaxies. In this paper, we present photometric and kinematic observations ofNGC 4123, a barred galaxy of modest size (V_rot = 130 km/sec, L = 0.7 L_*),which reveal strong non-circular motions. The bar has straight dust lanes andan inner Lindblad resonance. The disk of NGC 4123 has no sign of truncation outto 10 scale lengths, and star-forming regions are found well outside R_25. AFabry-Perot H-alpha velocity field shows velocity jumps of >100 km/sec at thelocation of the dust lanes within the bar, indicating shocks in the gas flow.VLA observations yield the velocity field of the H I disk. Axisymmetric massmodels yield good fits to the rotation curve outside the bar regionfor diskI-band M/L of 2.25 or less, and dark halos with either isothermal or power-lawprofiles can fit the data well. In a companion paper, we model the full 2-Dvelocity field, including non-circular motions, to determine the stellar M/Land the mass of the dark halo.[Journal_ref: Astrophys.J.546:916-930,2001]
• Sellwood, J. A., & Weiner, B. J. (1999). The Properties of the Galactic Bar Implied by Gas Kinematics in the Inner Milky Way. The Astrophysical Journal, 524(1), 112-128. doi:10.1086/307786
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  Longitude-velocity (l-V) diagrams of H I and CO gas in the inner Milky Way have long been known to be inconsistent with circular motion in an axisymmetric potential. Several lines of evidence suggest that the Galaxy is barred, and gas flow in a barred potential could be consistent with the observed "forbidden" velocities and other features in the data. We compare the H I observations to l-V diagrams synthesized from two-dimensional fluid dynamical simulations of gas flows in a family of barred potentials. The gas flow pattern is very sensitive to the parameters of the assumed potential, which allows us to discriminate among models. We present a model that reproduces the outer contour of the H I l-V diagram reasonably well; this model has a strong bar with a semimajor axis of 3.6 kpc, an axis ratio of approximately 3 : 1, an inner Lindblad resonance (ILR), and a pattern speed of 42 km s-1 kpc-1, and it matches the data best when viewed from 34° to the bar major axis. The behavior of the models, combined with the constraint that the shocks in the Milky Way bar should resemble those in external barred galaxies, leads us to conclude that wide ranges of parameter space are incompatible with the observations. In particular we suggest that the bar must be fairly strong, must have an ILR, and cannot be too end-on, with the bar major axis at 35° ± 5° to the line of sight. The H I data exhibit larger forbidden velocities over a wider longitude range than are seen in molecular gas; this important difference is the reason our favored model differs so significantly from other recently proposed models.
• Weiner, B. J., & Sellwood, J. A. (1999). The properties of the Galactic bar implied by gas kinematics in the inner Milky Way. Astrophys.J., 524, 112-128.
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  Longitude-velocity (l-V) diagrams of H I and CO gas in the inner Milky Wayhave long been known to be inconsistent with circular motion in an axisymmetricpotential. Several lines of evidence suggest that the Galaxy is barred, and gasflow in a barred potential could be consistent with the observed ``forbidden''velocities and other features in the data. We compare the H I observations tol-V diagrams synthesized from 2-D fluid dynamical simulations of gas flows in afamily of barred potentials. The gas flow pattern is very sensitive to theparameters of the assumed potential, which allows us to discriminate amongmodels. We present a model that reproduces the outer contour of the H I l-Vdiagram reasonably well; this model has a strong bar with a semimajor axis of3.6 kpc, an axis ratio of approximately 3:1, an inner Lindblad resonance (ILR),and a pattern speed of 42 km/s/kpc, and matches the data best when viewed from34\deg to the bar major axis. The behavior of the models, combined with theconstraint that the shocks in the Milky Way bar should resemble those inexternal barred galaxies, leads us to conclude that wide ranges of parameterspace are incompatible with the observations. In particular we suggest that thebar must be fairly strong, must have an ILR, and cannot be too end-on, with thebar major axis at 35\deg +/- 5\deg to the line of sight. The H I data exhibitlarger forbidden velocities over a wider longitude range than are seen inmolecular gas; this important difference is the reason our favored modeldiffers so significantly from other recently proposed models.[Journal_ref: Astrophys.J.524:112-128,1999]
• Sellwood, J. A., Weiner, B. J., & Williams, T. B. (1996). Fabry-Perot Observations and Hydrodynamical Simulations of the Barred Spiral NGC 4123. International Astronomical Union Colloquium, 157, 489-491. doi:10.1017/s0252921100050302
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  We present Fabry-Perot observations of the velocity field of gas in the barred spiral NGC 4123, and 2-D hydrodynamical simulations of the gas flow in model potentials derived from I -band photometry. The simulated gas flow is quite sensitive to the details of the potential, which enables us to constrain parameters such as the M / L I of the bar and the bar pattern speed. The observations confirm that the dust lanes along the leading edges of the bar are the locations of shocks. Requiring models to produce shocks with the correct alignment constrains the Lagrange point L 1 (corotation) to be at a radius 1.1 – 1.4 times the semimajor axis of the bar, i . e . the bar is a fast rotator.
• Weiner, B. J., & Williams, T. B. (1996). Detection of H(alpha) Emission From The Magellanic Stream: Evidence For an Extended Gaseous Galactic Halo. The Astronomical Journal, 111(Issue 3), 1156-1163. doi:10.1086/117860
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  We have detected faint, diffuse H$\alpha emission from several points along the Magellanic Stream, using the Rutgers Fabry--Perot Interferometer at the CTIO 1.5-m telescope. At points on the leading edges of the H I clouds MS II, MS III, and MS IV, we detect H$\alpha emission of surface brightness $0.37 \pm 0.02$ Rayleighs, $0.21 \pm 0.04$ R, and $0.20 \pm 0.02$ R respectively, corresponding to emission measures of 1.0 to 0.5 \cmsixpc. We have observed several positions near the MS IV concentration, and find that the strongest emission is on the sharp leading-edge density gradient. There is less emission at points away from the gradient, and halfway between MS III and MS IV the H$\alpha surface brightness is $< 0.04$ R. We attribute the H$\alpha emission at cloud leading edges to heating of the Stream clouds by ram pressure from ionized gas in the halo of the Galaxy. These observations suggest that ram pressure from halo gas plays a large role in stripping the Stream out of the Magellanic Clouds. They also suggest the presence of a relatively large density of gas, $n_{\rm H} \sim 10^{-4} cm^{-3}$, in the Galactic halo at $\sim 50$ kpc radius, and far above the Galactic plane, $b \sim -80\deg$. This implies that the Galaxy has a very large baryonic, gaseous extent, and supports models of Lyman-$\alpha and metal-line QSO absorption lines in which the absorption systems reside in extended galactic halos.
• Weiner, B. J., & Williams, T. B. (1996). Detection of H-alpha emission from the Magellanic Stream: evidence for an extended gaseous Galactic halo. Astron.J., 111, 1156-1163.
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  We have detected faint, diffuse H$\alpha emission from several points alongthe Magellanic Stream, using the Rutgers Fabry--Perot Interferometer at theCTIO 1.5-m telescope. At points on the leading edges of the H I clouds MS II,MS III, and MS IV, we detect H$\alpha emission of surface brightness $0.37 \pm0.02$ Rayleighs, $0.21 \pm 0.04$ R, and $0.20 \pm 0.02$ R respectively,corresponding to emission measures of 1.0 to 0.5 \cmsixpc. We have observedseveral positions near the MS IV concentration, and find that the strongestemission is on the sharp leading-edge density gradient. There is less emissionat points away from the gradient, and halfway between MS III and MS IV theH$\alpha surface brightness is $< 0.04$ R. We attribute the H$\alpha emission at cloud leading edges to heating of theStream clouds by ram pressure from ionized gas in the halo of the Galaxy. Theseobservations suggest that ram pressure from halo gas plays a large role instripping the Stream out of the Magellanic Clouds. They also suggest thepresence of a relatively large density of gas, $n_{\rm H} \sim 10^{-4}cm^{-3}$, in the Galactic halo at $\sim 50$ kpc radius, and far above theGalactic plane, $b \sim -80\deg$. This implies that the Galaxy has a very largebaryonic, gaseous extent, and supports models of Lyman-$\alpha and metal-lineQSO absorption lines in which the absorption systems reside in extendedgalactic halos.[Journal_ref: Astron.J.111:1156-1163,1996]

Proceedings Publications

• Pearce, E. C., & Weiner, B. J. (2019, september). Examining the Effects of On-Orbit Aging of SL-12 Rocket Bodies using Visible Band Spectra with the MMT Telescope. In Advanced Maui Optical and Space Surveillance Technologies (AMOS) Conference.
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  The characterization of deep space debris has posed a significant challenge in SSA. To be most operationally effective, characterization must be performed quickly and under non-ideal operational conditions, generally using non-resolved techniques. The use of multi-color photometry and the resultant color indices offer the potential to rapidly discriminate between debris and intact space objects such as rocket bodies and satellites. However, these studies are not well informed by high resolution spectra of these same objects due to the lack of prior measurements with large astronomical telescopes. High resolution spectroscopy is not routinely collected by our SSA network. Nonetheless, several researchers have collected satellite spectra for research purposes. Several researchers have also noted the progressive reddening of spacecraft surfaces. Jorgensen measured reflectance spectra over a range of years on orbit (YOO) of 10-13 years of foreign discarded rocket bodies and noted significant increase in relative reflectance above 750 nm. Similarly, aging has been noted on GPS payloads using BVRI photometry by Fliegel.In this study, we have collected high resolution spectra of a group of five Russian SL-12 rocket bodies in geosynchronous orbit. The spectra were collected with the Blue Channel Spectrograph on the 6.5 m MMT telescope at Mt. Hopkins. The measurements were taken using the 300-line grating, which is blazed for the red, and can cover a 5200 Å range at dispersion 1.96 Å/pixel. The large collecting aperture of the MMT allowed the rapid collection of multiple high signal-to-noise spectra with only 2 minutes per exposure. This short exposure allowed us to have confidence the solar phase angle was near constant during each collection, but that the spectra were averaged over the rotation of the rocket body. These spectra allow analysis of both the variation in albedo over a large wavelength range, and searches for discrete absorption features. The SL-12 (also called the “Proton K”) was a mainstay Russian four-stage to GEO launch vehicle that was used from 1974 to 2012 (Gunter 2017). The SL-12 fourth stage rocket bodies (henceforth referred to as “SL-12 RB”) offer a convenient ensemble of objects for which photometric techniques can be developed and tested. For this study, five SL-12s with a range of years-on-orbit (YOO) ranging from 23-35 years were collected, allowing a comparative study of the evolution of the spectra over a 12-year difference in age. Additionally, all these objects have been previously observed with the UKIRT WFCAM. The spectra are analyzed for evidence of the effects of on-orbit reddening and other changes over time.
• Pearce, E., Weiner, B., Block, A., Krantz, H., Rockowitz, K., Sease, B., Hennessy, G., & Wilson, M. (2019, sep). Examining the Effects of On-Orbit Aging of SL-12 Rocket Bodies using Visible Band Spectra with the MMT Telescope and 5-Color Photometry with the UKIRT/WFCAM. In Proceedings of the Advanced Maui Optical and Space Surveillance Technologies Conference.
• Weiner, B. J., Sand, D., Gabor, P., Johnson, C., Swindell, S., Kub{\'anek}, P., Gasho, V., Golota, T., Jannuzi, B., Milne, P., Smith, N., & Zaritsky, D. (2018, Jul). Development of the Arizona Robotic Telescope Network. In Observatory Operations: Strategies, Processes, and Systems VII, 10704.
• Hart, M., Hart, M., Furfaro, R., Furfaro, R., Weiner, B. J., Weiner, B. J., Corral, E. L., Corral, E. L., Lyons, E. H., Lyons, E. H., Surdeanu, M., Surdeanu, M., Butcher, E., Butcher, E., Gaylor, D., Gaylor, D., Jah, M. K., Jah, M. K., Merchant, N. C., , Merchant, N. C., et al. (2016, May). A New Approach to Space Domain Awareness at the University of Arizona. In NATO Symposium on Considerations for Space and Space-Enabled Capabilities in NATO Coalition Operations, SCI-283.
• Hart, M., Hart, M., Hart, M., Hart, M., Jah, M. K., Jah, M. K., Jah, M. K., Jah, M. K., Gaylor, D., Gaylor, D., Gaylor, D., Gaylor, D., Butcher, E., Butcher, E., Butcher, E., Butcher, E., Ten Eyck, B., Ten Eyck, B., Ten Eyck, B., , Ten Eyck, B., et al. (2016, May). A New Approach to Space Domain Awareness at the University of Arizona. In NATO Symposium on "Considerations for Space and Space-Enabled Capabilities in NATO Coalition Operations".
• {Simons}, R., {Kassin}, S., {Trump}, J., {Weiner}, B., {Barro}, G., {Koo}, D., {Faber}, S., , Y. (2015, aug). "{When are Galaxy Disks Formed? Multi-PA Galaxy Kinematics at z~{}2 with Keck/MOSFIRE}". In IAU General Assembly, 22, 2257477.
• Alberts, S., Pope, A., Brodwin, M., Atlee, D. W., Lin, Y., Chary, R., Dey, A., Eisenhardt, P. R., Gettings, D., Gonzalez, A. H., Jannuzi, B., Mancone, C., Moustakas, J., Snyder, G. F., Stanford, S. A., Stern, D., Weiner, B. J., & Zeimann, G. (2014, jan). How Environment Affects Star Formation: Tracing Activity in High Redshift Galaxy Clusters. In American Astronomical Society Meeting Abstracts, 223, #130.02.
• Mei, S., Scarlata, C., Pentericci, L., Newman, J., Teplitz, H. I., Weiner, B. J., Ashby, M., Castellano, M., Conselice, C., Finkelstein, S. L., Galametz, A., Koekemoer, A. M., Lucas, R. A., Rafelski, M., & Team, C. (2014, jan). A progenitor of today rsquos typical galaxy clusters at z=1.84. In American Astronomical Society Meeting Abstracts, 223, #145.08.
• Simons, R., Kassin, S. A., Weiner, B. J., & Lee, J. C. (2014, jan). A Characteristic Mass in the Low Redshift Tully Fisher Relation. In American Astronomical Society Meeting Abstracts, 223, #205.04.
• Trump, J. R., Brandt, W. N., Weiner, B. J., Juneau, S., CANDELS, ., & 3D-HST, . (2014, jan). The AGN Census at Cosmic Noon: the Unbiased Galaxy-AGN Connection from Spatially Resolved Line Ratios. In American Astronomical Society Meeting Abstracts, 223, #402.05.
• Weiner, B. J. (2014, jan). Occupy Hard Drives: Making your work more valuable by giving it away. In American Astronomical Society Meeting Abstracts, 223, #225.01.
• Weiner, B. J., & Team, A. (2014, jan). Star formation rates and extinction at z=1-2 from the AGHAST HST infrared grism survey. In American Astronomical Society Meeting Abstracts, 223, #227.07.
• Kassin, S. A., Weiner, B. J., Faber, S. M., Gardner, J. P., & Team, D. (2013, jan). The Epoch of Disk Settling: 1 to Today. In American Astronomical Society Meeting Abstracts, 221, #304.06.
• Mostek, N. J., Coil, A. L., Cooper, M. C., Davis, M., Newman, J., & Weiner, B. J. (2013, jan). The DEEP2 Galaxy Redshift Survey: Clustering Dependence on Galaxy Stellar Mass and Star Formation Rate at 1. In American Astronomical Society Meeting Abstracts, 221, #434.01.
• Trump, J. R., Barro, G., Weiner, B. J., Konidaris, N., Koo, D. C., Kocevski, D., Yan, R., Juneau, S., Faber, S. M., & CANDELS, . (2013, jan). Do z gt1 Clumpy Galaxies in CANDELS Fuel AGNs?. In American Astronomical Society Meeting Abstracts, 221, #133.07.
• Hibon, P. M., Rhoads, J. E., Malhotra, S., Cooper, M., & Weiner, B. (2012, jan). A Lyman-Alpha Galaxy at Redshift z=6.944. In American Astronomical Society Meeting Abstracts #219, 219, #246.31.
• Ono, Y., Ouchi, M., Mobasher, B., Dickinson, M., Penner, K., Shimasaku, K., Weiner, B. J., Kartaltepe, J. S., Nakajima, K., Nayyeri, H., Stern, D., Kashikawa, N., & Spinrad, H. (2012, may). Spectroscopic Confirmation of Three z-Dropout Galaxies at z = 6.844-7.213: Demographics of Lya Emission in z sim 7 Galaxies. In American Astronomical Society Meeting Abstracts #220, 220, #429.03.
• Sheth, K., Melbourne, J., Kassin, S., Elmegreen, D. M., Elmegreen, B. G., Athanassoula, E., Abraham, R. G., Ellis, R. S., & Weiner, B. (2012, may). A Plausible Explanation for the Steep Redshift Decline in Barred Spirals: Dynamically Hot Disks. In American Astronomical Society Meeting Abstracts #220, 220, #409.05.
• Shipley, H. V., Papovich, C., Dey, A., Jannuzi, B., Rieke, G., & Weiner, B. (2012, jan). Spitzer Infrared Spectrograph Observations of Infrared-Luminous Galaxies at Moderate Redshift: Diagnostics of AGN and Star Formation. In American Astronomical Society Meeting Abstracts #219, 219, #246.17.
• Trump, J. R., Weiner, B. J., Koo, D. C., Faber, S. M., & Kocevski, D. D. (2012, jan). Emission-Line Diagnostics of Nuclear Activity and Star Formation in Galaxies at 0 ltz $ epsilon$ with CANDELS. In American Astronomical Society Meeting Abstracts #219, 219, #131.01.
• Weiner, B. J. (2012, jan). Infrared Spectroscopy with HST: Grism Results in the CANDELS Fields. In American Astronomical Society Meeting Abstracts #219, 219, #406.06.
• Weiner, B. J. (2009). Star Formation Driven Galactic Winds at z∼1.4. In AIP Conference Proceedings, 1201, 142-145.
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  Galactic winds are a prime suspect for driving metals out of galaxies, creating the mass‐metallicity relation, probably enriching the IGM, and explaining the low baryon fraction in galaxies. They may also be related to the quenching of star formation in red galaxies. However, it is unclear how efficiently winds couple to the ISM, and which types and masses of galaxies drove winds in the past. Spectroscopy of blueshifted Mg II absorption in galaxies at z∼1.4 in the DEEP2 survey shows that winds are ubiquitous at that redshift (where the SFR in the bulk of galaxies is higher than today), and that they are driven by star formation. Many of these galaxies will become spirals rather than ellipticals, showing that SF‐driven winds are part of the past history of many galaxies, but that such winds do not directly lead to quenching or deterrence of subsequent star formation.
• Davis, M., Faber, S. M., Newman, J. A., Phillips, A. C., Ellis, R. S., Steidel, C. C., Conselice, C., Coil, A. L., Finkbeiner, D. P., Koo, D. C., Guhathakurta, P., Weiner, B., Schiavon, R., Willmer, C., Kaiser, N., Luppino, G., Wirth, G., Connolly, A., Eisenhardt, P., , Cooper, M., et al. (2002). Science objectives and early results of the DEEP2 redshift survey. In Discoveries and Research Prospects from 6- to 10- Meter-Class telescopes II, 4834.
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  The DEIMOS spectrograph has now been installed on the Keck-II telescope and commissioning is nearly complete. The DEEP2 Redshift Survey, which will take approximately 120 nights at the Keck Observatory over a three year period and has been designed to utilize the power of DEIMOS, began in the summer of 2002. The multiplexing power and high efficiency of DEIMOS enables us to target 1000 faint galaxies per clear night. Our goal is to gather high-quality spectra of ≈ 60,000 galaxies with z > 0.75 in order to study the properties and large scale clustering of galaxies at z ≈ 1. The survey will be executed at high spectral resolution, R = λ/δλ ≈ 5000, allowing us to work between the bright OH sky emission lines and to infer linewidths for many of the target galaxies (for several thousand objects, we will obtain rotation curves as well). The linewidth data will facilitate the execution of the classical redshift-volume cosmological test, which can provide a precision measurement of the equation of state of the Universe. This talk reviews the project, summarizes our science goals and presents some early DEIMOS data.