Brenda Louise Frye

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• Acebron, A., Bergamini, P., Rosati, P., Tozzi, P., Meneghetti, M., Caminha, G. B., Ertl, S., Granata, G., Koekemoer, A. M., Grillo, C., Schuldt, S., Frye, B. L., & Diego, J. M. (2025). Enhanced strong-lensing model of MACS J0138.0- 2155 based on new JWST and VLT/MUSE observations. Astronomy and Astrophysics, 699(Issue). doi:10.1051/0004-6361/202554468
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  We present a new parametric strong-lensing analysis of the galaxy cluster MACS J0138.0- 2155 at zL = 0.336. This is the first lens cluster known to show two multiply imaged supernova (SN) siblings, SN Requiem and SN Encore at zSNe = 1.949, enabling a new measurement of the Hubble constant value from the measured relative time delays. We exploited Hubble Space Telescope and James Webb Space Telescope multi-band imaging in synergy with new Multi Unit Spectroscopic Explorer follow-up spectroscopy to develop an improved lens mass model. Specifically, we included 84 cluster members (∼ 60% of which are spectroscopically confirmed) and two perturber galaxies along the line of sight. Our observables consisted of 23 spectroscopically confirmed multiple images from eight background sources, spanning a fairly wide redshift range from 0.767 to 3.420. To accurately characterise the sub-halo mass component, we calibrated the Faber-Jackson scaling relation based on the stellar kinematic measurements of a subset of 14 bright cluster galaxies. We built several lens models by implementing different cluster total mass parametrisations to assess the statistical and systematic uncertainties on the predicted values of the position and magnification of the observed and future multiple images of SN Requiem and SN Encore. Our reference best-fit lens model reproduces the observed positions of the multiple images with a root mean square offset of 0".36 and the multiple-image positions of the SNe and their host galaxy with a remarkable mean precision of only 0".05. We measure a projected total mass of M(
• Adams, N. J., Ferrami, G., Westcott, L., Harvey, T., Estrada-Carpenter, V., Conselice, C. J., Austin, D., Wyithe, J. S., Goolsby, C. M., Li, Q., Rusakov, V., Windhorst, R. A., Cohen, S. H., Jansen, R. A., Summers, J., O’Brien, R., Koekemoer, A. M., Driver, S. P., Frye, B., , Hathi, N. P., et al. (2025). JWSTs PEARLS: NIRCam imaging and NIRISS spectroscopy of a z = 3.6 star-forming galaxy lensed into a near-Einstein ring by a z = 1.258 massive elliptical galaxy. Monthly Notices of the Royal Astronomical Society, 543(Issue 4). doi:10.1093/mnras/staf1518
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  We present the discovery, and initial lensing analysis, of a high-redshift galaxy–galaxy lensing system within the JWSTPEARLS/HST–TREASUREHUNT North Ecliptic Pole Time Domain Field (designated NEPJ172238.9+655143.1). The lensing geometry shears a z = 3.6 ± 0.1 star-forming galaxy into a near-Einstein ring with a radius of 0.92 arcsec, consisting of 4 images, around a foreground massive elliptical galaxy at z = 1.258 ± 0.005. The system isfortuitously located within the NIRISS F200W footprint of the PEARLS survey, enabling spectroscopic identification of the 8500 Å TiO band in the foreground galaxy and allowing tight constraints to be placed on the redshift of the background galaxy based on its continuum detection and lack of strong emission lines. We calculate magnification factors of 2.6 < μ < 8.4 for the four images and a total lensing mass of (4.08 ± 0.07) × 1011 M. SED fitting of the foreground elliptical galaxy within the Einstein radius reveals a stellar mass of 1.26 × 1011 M under a Kroupa IMF, providing 31 per cent of the estimated lensing mass. Employing simple scaling relations and assumptions, an NFW dark matter halo is found to provide the correct remaining mass within 0.12+0.21−0.09 dex. However, if a modified IMF for elliptical galaxies is employed (e.g. bottom-heavy or bottom-and-top-heavy), stellar mass estimations increase and can account for the majority of the lensing mass, reducing the need for dark matter. This system further demonstrates the new discovery space that the combined wavelength coverage, sensitivity and resolution of James Webb Space Telescope (JWST) now enables.
• Carranza-Escudero, M., Conselice, C. J., Adams, N., Harvey, T., Austin, D., Behroozi, P., Ferreira, L., Ormerod, K., Duan, Q., Trussler, J., Li, Q., Westcott, L., Windhorst, R. A., Coe, D., Cohen, S. H., Cheng, C., Driver, S. P., Frye, B., Furtak, L. J., , Grogin, N. A., et al. (2025). Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions. Astrophysical Journal Letters, 989(Issue 2). doi:10.3847/2041-8213/adf73d
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  Observations with the James Webb Space Telescope reveal a previously unseen population of compact red objects, known as “little red dots” (LRDs). We study a new photometrically selected sample of 124 LRDs in the redshift range z ∼ 3-10 selected from Near Infrared Camera coverage of the Cosmic Evolution Early Release Science Survey (CEERS), North Ecliptic Pole Time Domain Field (NEP-TDF), James Webb Space Telescope Advanced Deep Extragalactic Survey (JADES), and JEMS. For JADES, the NEP-TDF, and CEERS, we compare spectral energy distribution (SED) models with and without active galactic nucleus (AGN) components and analyze the impact of an AGN component on the goodness of fit using the Bayesian information criterion (BIC). We find that while the χ2 of the majority of models containing AGN components is improved compared to models without AGN components, we show that the BIC suggests that models without AGN are a more appropriate fit to LRD SEDs, especially when MIRI data are available. We also measure LRD clustering in the CEERS field, JADES field, and NEP-TDF, where we compare the spatial distribution of LRDs and galaxies with Kolmogorov-Smirnov tests of equality of distribution. We find that the neighbourhood of LRDs tends to be less dense compared to galaxies at all selections and masses and at similar redshifts. We further measure upper limit estimates for the halo masses of LRDs using abundance matching. While the population of LRDs could be a mixture of several different inherent populations, as a whole, it does appear that these systems are mostly hosting compact galaxies or star clusters in formation.
• Conselice, C. J., Adams, N., Harvey, T., Austin, D., Ferreira, L., Ormerod, K., Duan, Q., Trussler, J., Li, Q., Juodžbalis, I., Westcott, L., Harris, H., Seeyave, L. T., Bluck, A. F., Windhorst, R. A., Bhatawdekar, R., Coe, D., Cohen, S. H., Cheng, C., , Driver, S. P., et al. (2025). EPOCHS. I. The Discovery and Star-forming Properties of Galaxies in the Epoch of Reionization at 6.5 < z < 18 with PEARLS and Public JWST Data. Astrophysical Journal, 983(Issue 1). doi:10.3847/1538-4357/ada608
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  We present in this paper the discovery, properties, and a catalog of 1165 high-redshift 6.5 < z < 18 galaxies found in deep JWST NIRCam imaging from the GTO PEARLS survey combined with data from JWST public fields. We describe our bespoke homogeneous reduction process and our analysis of these areas including the NEP, CEERS, GLASS, NGDEEP, JADES, and ERO SMACS-0723 fields with over 214 arcmin2 imaged to depths of ∼30 mag. We describe our rigorous methods for identifying these galaxies, involving the use of Lyman-break strength, detection significance criteria, visual inspection, and integrated photometric redshift probability distributions predominately at high redshift. Our sample is a robust and highly pure collection of distant galaxies from which we also remove brown dwarf stars, and calculate completeness and contamination from simulations. We include a summary of the basic properties of these z > 6.5 galaxies, including their redshift distributions, UV absolute magnitudes, and star formation rates. Our study of these young galaxies reveals a wide range of stellar population properties as seen in their colors and SED fits, which we compare to stellar population models, indicating a range of star formation histories (SFHs), dust, active galactic nuceli, and/or nebular emission. We find that a strong trend exists between stellar mass and (U − V) color, as well as the existence of the “main-sequence” of star formation for galaxies as early as z ∼ 12. This indicates that stellar mass, or an underlying variable correlating with stellar mass, is driving galaxy formation, in agreement with simulation predictions. We also discover ultra-high-redshift candidates at z > 12 in our sample and describe their properties. Finally, we note a significant observed excess of galaxies compared to models at z > 12, revealing a tension between predictions and our observations.
• Duan, Q., Conselice, C. J., Li, Q., Austin, D., Harvey, T., Adams, N. J., Duncan, K. J., Trussler, J., Ferreira, L., Westcott, L., Harris, H., Windhorst, R. A., Holwerda, B. W., Broadhurst, T. J., Coe, D., Cohen, S. H., Du, X., Driver, S. P., Frye, B., , Grogin, N. A., et al. (2025). Galaxy mergers in the epoch of reionization - I. A JWST study of pair fractions, merger rates, and stellar mass accretion rates at z = 4.5-11.5. Monthly Notices of the Royal Astronomical Society, 540(Issue 1). doi:10.1093/mnras/staf638
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  We present a full analysis of galaxy major merger pair fractions, merger rates, and mass accretion rates, thus uncovering the role of mergers in galaxy formation at the earliest previously unexplored epoch of
• D’Silva, J. C., Driver, S. P., Lagos, C. D., Robotham, A. S., Adams, N. J., Conselice, C. J., Frye, B., Hathi, N. P., Harvey, T., Koekemoer, A. M., Ortiz, R., Ricotti, M., Robertson, C., Rutkowski, M. J., Silver, R. M., Wilkins, S. M., Willmer, C. N., Windhorst, R. A., Cohen, S. H., , Jansen, R. A., et al. (2025). Self-consistent JWST Census of Star Formation and AGN Activity at z = 5.5-13.5. Astrophysical Journal, 990(Issue 1). doi:10.3847/1538-4357/adf19e
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  The cosmic star formation history (CSFH) and cosmic active galactic nuclei (AGN) luminosity history (CAGNH) are self consistently measured at z = 5.5-13.5. This is achieved by analyzing galaxies detected by the James Webb Space Telescope from ≈ 400 arcmin 2 fields from the Prime Extragalactic Areas of Reionization and Lensing Science, Cosmic Evolution Early Release Science, Next Generation Deep Extragalactic Exploratory Public, JWST Advanced Deep Extragalactic Survey, and Public Release IMaging for Extragalactic Research surveys. In particular, the combination of spectral energy distribution fitting codes, EAZY and ProSpect, is employed to estimate the photometric redshifts and astrophysical quantities of 3751 distant galaxies, from which we compute the stellar mass, star formation rate, and AGN luminosity distribution functions in four redshift bins. Integrating the distribution functions, we find that the CSFH rises by ≈1 dex over z = 13.5-5.5, and the CAGNH rises by ≈1 dex over z = 10.5-5.5. We connect our results of the CSFH and CAGNH at z = 13.5-5.5 to that from z = 5-0 to determine the summary of ≳13 Gyr of star formation and AGN activity, from the very onset of galaxy formation to the present day.
• Fudamoto, Y., Sun, F., Diego, J. M., Dai, L., Oguri, M., Zitrin, A., Zackrisson, E., Jauzac, M., Lagattuta, D. J., Egami, E., Iani, E., Windhorst, R. A., Abe, K. T., Bauer, F. E., Bian, F., Bhatawdekar, R., Broadhurst, T. J., Cai, Z., Chen, C. C., , Chen, W., et al. (2025). Identification of more than 40 gravitationally magnified stars in a galaxy at redshift 0.725. Nature Astronomy, 9(Issue 3). doi:10.1038/s41550-024-02432-3
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  Strong gravitational magnification enables the detection of faint background sources and allows researchers to resolve their internal structures and even identify individual stars in distant galaxies. Highly magnified individual stars are useful in various applications, including studies of stellar populations in distant galaxies and constraining dark matter structures in the lensing plane. However, these applications have been hampered by the small number of individual stars observed, as typically one or a few stars are identified from each distant galaxy. Here, we report the discovery of more than 40 microlensed stars in a single galaxy behind Abell 370 at redshift of 0.725 (dubbed ‘the Dragon arc’) when the Universe was half of its current age, using James Webb Space Telescope observations with the time-domain technique. These events were found near the expected lensing critical curves, suggesting that these are magnified stars that appear as transients from intracluster stellar microlenses. Through multi-wavelength photometry, we constrained their stellar types and found that many of them are consistent with red giants or supergiants magnified by factors of hundreds. This finding reveals a high occurrence of microlensing events in the Dragon arc and demonstrates that time-domain observations by the James Webb Space Telescope could lead to the possibility of conducting statistical studies of high-redshift stars.
• Harris, W. E., Reina-Campos, M., Koekemoer, A. M., Berkheimer, J. M., Carleton, T., Cohen, S. H., Frye, B. L., Hinrichs, T. R., Holwerda, B. W., Honor, R., Ricotti, M., Willner, S. P., Windhorst, R. A., & Yan, H. (2025). PEARLS: Globular Clusters and Ultracompact Dwarfs in the El Gordo Galaxies at z = 0.87. Astrophysical Journal, 991(Issue 1). doi:10.3847/1538-4357/adf8dc
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  JWST/NIRCam 0.9 to 2.0 μm images reveal a population of point sources around the major galaxies in the El Gordo cluster at redshift z = 0.87. Their distribution in the color-magnitude diagrams shows a narrow sequence well separated from field-galaxy contamination and consistent with their identification as ultracompact dwarf galaxies (UCDs) or luminous globular clusters (GCs). The point-source sequence is more luminous by almost a magnitude than the corresponding sequence in Abell 2744 at z = 0.31, matching the predicted evolutionary change for GC/UCDs over the 4 Gyr difference in look-back time between these two clusters. Deeper observations should allow direct JWST imaging of GC/UCD populations, even without the help of lensing, up to z ∼ 1.4, a look-back time of more than 9 Gyr. Such observations would directly reveal the evolution of these compact stellar systems two-thirds of the way back to the Big Bang.
• Harvey, T., Conselice, C. J., Adams, N. J., Austin, D., Juodžbalis, I., Trussler, J., Li, Q., Ormerod, K., Ferreira, L., Lovell, C. C., Duan, Q., Westcott, L., Harris, H., Bhatawdekar, R., Coe, D., Cohen, S. H., Caruana, J., Cheng, C., Driver, S. P., , Frye, B., et al. (2025). EPOCHS. IV. SED Modeling Assumptions and Their Impact on the Stellar Mass Function at 6.5 ≤ z ≤ 13.5 Using PEARLS and Public JWST Observations. Astrophysical Journal, 978(Issue 1). doi:10.3847/1538-4357/ad8c29
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  We utilize deep JWST Near Infrared Camera (NIRCam) observations for the first direct constraints on the Galaxy Stellar Mass Function (GSMF) at z > 10. Our EPOCHS v1 sample includes 1120 galaxy candidates at 6.5 < z < 13.5 taken from a consistent reduction and analysis of publicly available deep JWST NIRCam data covering the Prime Extragalactic Areas for Reionization Science, CEERS, GLASS, JADES GOOD-S, NGDEEP, and SMACS0723 surveys, totaling 187 arcmin2. We investigate the impact of spectral energy distribution fitting methods, assumed star formation histories (SFHs), dust laws, and priors on galaxy masses and the resultant GSMF. While our fiducial GSMF agrees with the literature at z < 13.5, we find that the assumed SFH model has a large impact on the GSMF and stellar mass density (SMD), finding a 0.75 dex increase in the SMD at z = 10.5 between a flexible nonparametric and standard parametric SFH. Overall, we find a flatter SMD evolution at z ≥ 9 than some studies predict, suggesting a rapid buildup of stellar mass in the early Universe. We find no incompatibility between our results and those of standard cosmological models, as suggested previously, although the most massive galaxies may require a high star formation efficiency. We find that the “little red dot” galaxies dominate the z = 7 GSMF at high masses, necessitating a better understanding of the relative contributions of active galactic nucleus and stellar emission. We show that assuming a theoretically motivated top-heavy initial mass function (IMF) reduces stellar mass by 0.5 dex without affecting fit quality, but our results remain consistent with existing cosmological models with a standard IMF.
• Li, Q., Conselice, C. J., Sarron, F., Harvey, T., Austin, D., Adams, N., Trussler, J. A., Duan, Q., Ferreira, L., Westcott, L., Harris, H., Dole, H., Grogin, N. A., Frye, B., Koekemoer, A. M., Robertson, C., Windhorst, R. A., Polletta, M. D., Hathi, N. P., & Jansen, R. A. (2025). EPOCHS paper - X. Environmental effects on Galaxy formation and protocluster Galaxy candidates at 4.5 < z < 10 from JWST observations. Monthly Notices of the Royal Astronomical Society, 539(Issue 2). doi:10.1093/mnras/staf543
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  In this paper, we describe our search for galaxy protocluster candidates at 4.5 < z < 10 and explore the environmental and physical properties of their member galaxies identified through JWST wide-field surv e ys within the CEERS (Cosmic Evolution Early Release Science), JADES (JWST Advanced Deep Extragalactic Surv e y), and PEARLS (Prime Extragalactic Areas for Reionization and Lensing Science) NEP-TDF (North Ecliptic Pole Time-Domain Fields). Combining with Hubble Space Telescope ( HST ) data, we identify 2948 robust z > 4.5 galaxy candidates within an area of 185.4 arcmin 2 . We determine nearest neighbour statistics and galaxy environments. We find that high- z galaxies in o v erdense environments e xhibit higher star formation activity compared to those in underdense regions. Galaxies in dense environments have a slightly increased star formation rate (SFR) at a given mass compared with galaxies in the lower density environments. At the high-mass end, we also find a gradual flattening of the M∗-SFR slope. We find that galaxies in high-density regions often have redder ultraviolet slopes than those in low-density regions, suggesting more dust extinction, weaker Ly aemission, and/or a higher damped Lyα absorption. The mass-size relation shows a weak positive correlation between galaxy size and local density. Furthermore, we quantitatively assess the probability of a galaxy belonging to a protocluster candidate. In total, we identified 26 o v erdensities at z = 5 -7 and estimate their dark matter halo masses. We find that all proto-cluster candidates could evolve into clusters with Mhalo > 1014 M⊙ at z = 0, thereby supporting the theoretical and simulation predictions of cluster formation. Notably, this marks an early search for protocluster candidates in JWST wide field based on photometric data, providing valuable candidates to study cosmic structure formation at the early stages.
• Limousin, M., Beauchesne, B., Niemiec, A., Diego, J. M., Jauzac, M., Koekemoer, A., Sharon, K., Acebron, A., Lagattuta, D., Mahler, G., Williams, L. L., Richard, J., Jullo, E., Furtak, L. J., Faisst, A. L., Frye, B. L., Hibon, P., Natarajan, P., & Rich, M. (2025). Mass and light in galaxy clusters: The case of Abell 370. Astronomy and Astrophysics, 693(Issue). doi:10.1051/0004-6361/202451969
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  In the cold dark matter (CDM) paradigm, an association between the hypothetic dark matter (DM) and its stellar counterpart is expected. However, parametric strong-lensing studies of galaxy clusters often display misleading features: DM components on the group or cluster scale without any stellar counterpart, offsets between the two components that are larger than what might be allowed by CDM or self-interacting DM models, or significant unexplained external shear components. This is the case in the galaxy cluster Abell 370, whose mass distribution has been the subject of several studies that were motivated by a wealth of data. The cluster was described parametrically with strong-lensing techniques by a model with four dark matter clumps and galaxy-scale perturbers, and with a significant external shear component, whose physical origin remains a challenge. The dark matter distribution features a mass clump without a stellar counterpart and a significant offset between one of the dark matter clumps and its associated stellar counterpart. This paper is based on BUFFALO data, and we begin by revisiting this mass model. Sampling this complex parameter space with Markov chain Monte Carlo (MCMC) techniques, we find a solution that does not require any external shear and provides a slightly better root mean square (RMS) than previous models (0.7″ compared to 0.9″). Investigating this new solution further, in particular, by varying the parameters that lead the MCMC sampler, we present a class of models that can accurately reproduce the strong-lensing data, but whose parameters for the dark matter component are poorly constrained. This limits any insights into its properties. We then developed a model in which each large-scale dark matter component must be associated with a stellar counterpart. This model with three dark matter clumps cannot reproduce the observational constraints with an RMS smaller than 2.3″, and the parameters describing this dark matter component remain poorly constrained. Examining the total projected mass maps, we find a good agreement between the total mass and the stellar distribution, which are both bimodal to first order. We interpret the misleading features of the mass model with four dark matter clumps and the failure of the mass model with three dark matter clumps as being symptomatic of the lacking realism of a parametric description of the dark matter distribution in such a complex merging cluster. We encourage caution and attention on the outputs of parametric strong-lensing modelling. We briefly discuss the implications of our results for using Abell 370 as a gravitational telescope. With the class of models that reproduce the strong- lensing data, we computed the magnifications for background Lyα emitters, and we present the critical curves obtained for the redshift of the Dragon arc, whose recent observations with the James Webb Space Telescope prompted interest. Finally, in light of our results, we discuss the strategy of choosing merging (multi-modal) clusters as gravitational telescopes compared to simple (unimodal) clusters.
• Manzoni, G., Broadhurst, T., Lim, J., Liu, T., Smoot, G., Baugh, C. M., Tompkins, S., Windhorst, R., Driver, S., Carleton, T., Frye, B., Fung, L., Zhang, J., Cohen, S. H., Conselice, C. J., Grogin, N. A., Jansen, R. A., Koekemoer, A. M., Ortiz, R., , Pirzkal, N., et al. (2025). Explaining JWST Counts with Galaxy Formation Models. Astrophysical Journal, 988(Issue 2). doi:10.3847/1538-4357/ade700
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  A distinct power-law break is apparent at mAB ∼ 21 in the deep near-infrared PEARLS-JWST galaxy counts. The break becomes more pronounced at longer wavelengths, with the slope flattening smoothly with apparent magnitude in the shortest band used at 0.9 μm, and trending toward an increasingly broken slope by the longest wavelength passband of JWST’s Near Infrared Camera, 4.4 μm. This behaviour is remarkably well predicted by the GALFORM semi-analytical model of galaxy formation. We use the model to diagnose the origin of this behaviour. The features that are responsible for the break are (1) the inherent break in the luminosity function (LF); (2) the change in the volume element with redshift; (3) the redshift-dependent nature of the k-correction (with 1 contributing to the existence of the break and 2-3 contributing to its shape). We study the contribution to these effects by their morphology using the bulge-to-total stellar mass ratio. The way in which bulge-dominated galaxies populate the bright end of the LF while disk-dominated galaxies dominate the faint end is preserved in the galaxy number counts, with a characteristic stellar mass at a break of ∼1010M⊙. The shape of the number counts is mainly driven by galaxies with relatively low redshift (z ≲ 2) for a limit of mAB ≲ 28. We give a comprehensive description of why the galaxy number counts in the near-infrared PEARLS-JWST observation look the way they do and which population of galaxies is dominant at each apparent magnitude.
• Marshall, M. A., Windhorst, R. A., Ferrami, G., Willner, S. P., Del Carmen Polletta, M., Keel, W. C., Fazio, G. G., Cohen, S. H., Carleton, T., Jansen, R. A., Honor, R., Ortiz, R., Summers, J., D’Silva, J. C., Koekemoer, A. M., Coe, D., Conselice, C. J., Diego, J. M., Driver, S. P., , Frye, B., et al. (2025). JWST’s PEARLS: A z ≃ 6 quasar in a train-wreck galaxy merger system. Astronomy and Astrophysics, 702(Issue). doi:10.1051/0004-6361/202554307
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  We present JWST NIRSpec integral field spectroscopy observations of the z = 5.89 quasar NDWFS J1425+3254 from 0.6–5.3 μm, covering the rest-frame ultraviolet and optical at a spectral resolution of R ∼ 100. The quasar has a black hole mass of MBH = (1.4+3.1−1.0) × 109 M☉ and an Eddington ratio of L Bol/L Edd = 0.3+0.6−0.2, as implied from the broad Balmer Hα and Hβ lines. The quasar host has significant ongoing obscured star formation, as well as a quasar-driven outflow with velocity 6050+460−630 km s−1 and ionised outflow rate of 1650+130−1230 M☉ yr−1. This is possibly one of the most extreme outflows in the early Universe. The data also reveal that two companion galaxies are merging with the quasar host. The north-eastern companion galaxy is relatively old and very massive, with a luminosity-weighted stellar age of 65+9−4 Myr, stellar mass of (3.6+0.6−0.3 #x00D7; 1011 M☉, and star-formation rate (SFR) of ∼15–30 M☉ yr−1. A bridge of gas connects this companion galaxy and the host, confirming their ongoing interaction. A second merger is occurring between the quasar host and a much younger companion galaxy to the south, with a stellar age of 6.7 ± 1.8 Myr, stellar mass of (1.9 ± 0.4)×1010 M☉, and SFR of ∼40–65 M☉ yr−1. There is also another galaxy in the field, likely in the foreground at z = 1.135, which could be gravitationally lensing the quasar with a magnification of 1 < μ < 2 and, thus, < 0.75 mag. Overall, the system is a ‘train-wreck’ merger of three galaxies, with star formation and extreme quasar activity that were likely triggered by these ongoing interactions.
• Messa, M., Vanzella, E., Loiacono, F., Bergamini, P., Castellano, M., Sun, B., Willott, C., Windhorst, R. A., Yan, H., Angora, G., Rosati, P., Adamo, A., Annibali, F., Bolamperti, A., Bradač, M., Bradley, L. D., Calura, F., Claeyssens, A., Comastri, A., , Conselice, C. J., et al. (2025). Anatomy of a z = 6 Lyman- α emitter down to parsec scales: Extreme UV slopes, metal-poor regions, and possibly leaking star clusters. Astronomy and Astrophysics, 694(Issue). doi:10.1051/0004-6361/202451695
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  We present a detailed JWST/NIRSpec and NIRCam analysis of a gravitationally lensed galaxy (μ = 17 - 21) at a redshift of 6.14 magnified by the Hubble Frontier Field galaxy cluster MACS J0416. The target galaxy is a typical compact and UV-faint (MUV = - 17.8) Lyman-α emitter, yet the large magnification allows the detailed characterization of structures on sub-galactic scales (down to a few parsecs). Prominent optical Hα, Hβ, and [OIII]λλ4959, 5007 lines are spatially resolved with the high-spectral-resolution grating (G395H, R 2700), with large equivalent widths, EW(Hβ+OIII) ≳ 1000 Å, and elevated ionizing photon production efficiencies, log(ξion/erg- 1Hz) = 25.2-25.7. NIRCam deep imaging reveals the presence of compact rest-UV-bright regions along with individual star clusters of Reff = 3 - 8 pc in size and M ~ 2 · 105 - 5 · 106 M⊙ in mass. These clusters are characterized by steep UV slopes, βUV ≲ - 2.5, which in some cases are associated with a dearth of line emission, indicating possible leaking of the ionizing radiation, as also supported by a Lyman-α emission peaking at ~100 km s- 1 from the systemic redshift. While the entire system is characterized by low metallicity, ~0.1 Z⊙, the NIRSpec-IFU map also reveals the presence of a low-luminosity, metal-poor region with Z ≲ 2% Z⊙, which is barely detected in NIRCam imaging; this region is displaced by > 200 pc from one of the brightest structures of the system in UV, and would have been too faint to detect if not for the large magnification of the system.
• Pascale, M., Dai, L., Frye, B. L., & Beverage, A. G. (2025). Is Earendel a Star Cluster?: Metal-poor Globular Cluster Progenitors at z ∼ 6. Astrophysical Journal Letters, 988(Issue 2). doi:10.3847/2041-8213/aded93
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  The strongly lensed z ∼ 6 Sunrise galaxy offers an incredible opportunity to investigate star formation in the early Universe on parsec or smaller scales. The highly magnified object Earendel within the Sunrise was previously identified as a candidate star or binary owing to size constraints placed by the lensing magnification; however, recent works have suggested that this constraint may be relaxed to even the size of star clusters. Here we explore the hypothesis that Earendel may actually be a star cluster, and we simultaneously evaluate other star clusters within the host galaxy. Leveraging deep, archival James Webb Space Telescope NIRSpec PRISM spectroscopy, we determine a spectroscopic redshift for the Sunrise galaxy z = 5.926 ± 0.013, and we fit simple stellar population (SSP) models from three premier libraries to evaluate the physical parameters of Earendel and another distinct star cluster in the Sunrise dubbed “1b.” We find the rest-UV through optical continuum of Earendel to be well described by an SSP, nearly equivalently to 1b, which is confidently a star cluster. We infer that they have intermediate ages tage ∼ 30-150 Myr, are metal-poor (Z⋆ ≲ 0.1 Z⊙), and are consistent with the formation age-metallicity trend seen in local globular clusters. Such intermediate-age clusters are seldom probed spectroscopically in the high-redshift Universe, and we explore the extent to which these clusters can be characterized via the spectroscopic continuum.
• Pascale, M., Frye, B. L., Pierel, J. D., Chen, W., Kelly, P. L., Cohen, S. H., Windhorst, R. A., Riess, A. G., Kamieneski, P. S., Diego, J. M., Meena, A. K., Cha, S., Oguri, M., Zitrin, A., Jee, M. J., Foo, N., Leimbach, R., Koekemoer, A. M., Conselice, C. J., , Dai, L., et al. (2025). SN H0pe: The First Measurement of H0 from a Multiply Imaged Type Ia Supernova, Discovered by JWST. Astrophysical Journal, 979(Issue 1). doi:10.3847/1538-4357/ad9928
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  The first James Webb Space Telescope (JWST) Near InfraRed Camera imaging in the field of the galaxy cluster PLCK G165.7+67.0 (z = 0.35) uncovered a Type Ia supernova (SN Ia) at z = 1.78, called “SN H0pe.” Three different images of this one SN were detected as a result of strong gravitational lensing, each one traversing a different path in spacetime, thereby inducing a relative delay in the arrival of each image. Follow-up JWST observations of all three SN images enabled photometric and rare spectroscopic measurements of the two relative time delays. Following strict blinding protocols which oversaw a live unblinding and regulated postunblinding changes, these two measured time delays were compared to the predictions of seven independently constructed cluster lens models to measure a value for the Hubble constant, H0 = 71.8 + 9.2 − 8.1 km s−1 Mpc−1. The range of admissible H0 values predicted across the lens models limits further precision, reflecting the well-known degeneracies between lens model constraints and time delays. It has long been theorized that a way forward is to leverage a standard candle, but this has not been realized until now. For the first time, the lens models are evaluated by their agreement with the SN absolute magnifications, breaking degeneracies and producing our best estimate, H0 = 75.7 − 5.5 + 8.1 km s−1 Mpc−1. This is the first precise measurement of H0 from a multiply imaged SN Ia and only the second from any multiply imaged SN.
• Saikia, P., Wrzosek, R., Gelfand, J., Brisken, W., Cotton, W., Willner, S. P., Gim, H. B., Windhorst, R. A., Estrada-Carpenter, V., Katkov, I. Y., Zaw, I., Nicandro Rosenthal, M. J., Shafi, H., Kellermann, K., Condon, J., Koekemoer, A. M., Conselice, C. J., Ortiz, R., Willmer, C. N., , Frye, B., et al. (2025). Peering into the Heart of Darkness with VLBA: Radio-quiet Active Galactic Nucleus in the JWST North Ecliptic Pole Time-domain Field. Astrophysical Journal, 989(Issue 1). doi:10.3847/1538-4357/ade709
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  We present initial results from the 4.8 GHz Very Long Baseline Array (VLBA) survey of the JWST North Ecliptic Pole Time-Domain Field (TDF). From 106 radio sources found in the Karl G. Jansky Very Large Array (VLA) observations in the TDF, we detected 12 sources (∼11% detection rate) at ∼3.3 μJy rms sensitivity and ∼4 mas resolution. Most detections exhibit parsec-scale emission (less than 40 pc) with high VLBA/VLA flux density ratios and brightness temperatures exceeding 105 K, confirming nonthermal active galactic nucleus (AGN) activity. Spectral indices α ≳ −0.5 correlate with higher VLBA/VLA flux ratios, consistent with synchrotron emission from AGN coronae or jets. In the majority of our sources, star formation contributes less than 50% of the total VLBA radio emission, with a few cases where the emission is almost entirely AGN driven. Although the radio emission from radio quiet AGN is thought to be primarily driven by star formation, our VLBA observations confirm that there is also often a contribution at various levels from black hole driven AGN. Eight VLBA detections have JWST/NIRCam counterparts, predominantly early-type, bulge-dominated galaxies, which we use to get an estimate of the redshift and star formation rate (SFR). Wide-field Infrared Survey Explorer colors indicate that VLBA detections are either AGN or intermediate-disk-dominated systems, while VLBA nondetections correspond to extended, star-forming galaxies. We compare SFRs derived from previous SCUBA-2 850 μm observations with new JWST-based estimates, and discuss the observed discrepancies, highlighting JWST’s improved capability to disentangle AGN activity from star formation.
• Valentino, F., Heintz, K. E., Brammer, G., Ito, K., Kokorev, V., Whitaker, K. E., Gallazzi, A., De Graaff, A., Weibel, A., Frye, B. L., Kamieneski, P. S., Jin, S., Ceverino, D., Faisst, A., Farcy, M., Fujimoto, S., Gillman, S., Gottumukkala, R., Hamadouche, M., , Harrington, K. C., et al. (2025). Gas outflows in two recently quenched galaxies at z = 4 and 7. Astronomy and Astrophysics, 699(Issue). doi:10.1051/0004-6361/202553908
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  Outflows are a key element in the baryon cycle of galaxies, impacting their evolution by extracting gas, momentum, and energy and then injecting them into the surrounding medium. The properties of gas outflows provide a fundamental test for our models of how galaxies transition from a phase of active star formation to quiescence. Here we report the detection of outflowing gas signatures in two recently quenched, massive (M∗∼14;1010.2 MO;) galaxies at z = 4.106 (NS_274) and z = 7.276 (RUBIES-UDS-QG-z7) observed at rest-frame ultraviolet to near-infrared wavelengths with JWST/NIRSpec. The outflows are traced by blueshifted magnesium (MgII) absorption lines, and in the case of the z = 4.1 system, also by iron (FeII) and sodium (NaI) features. Together, these transitions broadly trace the chemically enriched neutral phase of the gaseous medium. The rest-frame optical spectra of the two sources are similar to those of local post-starburst galaxies, showing deep Balmer stellar features, a relatively low Dn4000 index, and minimal ongoing star formation on 10 Myr timescales, as traced by the lack of bright nebular and recombination emission lines. This also suggests the absence of strong and radiatively efficient active galactic nucleus activity. The galaxies star formation histories are consistent with a recent and abrupt quenching, prior to which the average star formation rate was ∼14;15 MO; yr-1 over the last 100 Myr of their lives. In the case of NS_274, dedicated millimeter observations allowed us to also strongly constrain the dust obscured star formation rate to 10 for the z = 4.1 and z = 7.3 systems, respectively, and a similarly pronounced difference in the energy carried by the outflows. Supernova feedback could account for the mass and energy of the outflow in NS_274. However, the low mass loading factor and average gas velocity (∼14;180 km s-1, which is lower than the stellar velocity dispersion) suggest that the observed outflow is likely not the primary factor behind the quenching of NS_274, but it might represent a relic of the star formation process winding down. Star-formation-related processes seem to also be insufficient to explain the extreme mass outflow rate of RUBIES-UDS-QG-z7, which would require an additional ejective mechanism such as an undetected active galactic nucleus. Finally, the average outflow velocities per unit stellar mass, star formation rate, and surface density of star formation rate are consistent with those of lower-redshift post-starburst galaxies, suggesting that outflows in rapidly quenched galaxies might occur similarly across cosmic time. Our findings hint at the existence of a rich tapestry of galaxy quenching pathways at high redshifts, and they highlight the importance of using large spectroscopic samples that map different spectral features to account for the different timescales on which different mechanisms contribute to this process.
• Westcott, L., Conselice, C. J., Harvey, T., Austin, D., Adams, N., Ferrari, F., Ferreira, L., Trussler, J., Li, Q., Rusakov, V., Duan, Q., Harris, H., Goolsby, C., Broadhurst, T. J., Coe, D., Cohen, S. H., Driver, S. P., D’Silva, J. C., Frye, B., , Grogin, N. A., et al. (2025). EPOCHS. XI. The Structure and Morphology of Galaxies in the Epoch of Reionization to z ∼ 12.5. Astrophysical Journal, 983(Issue 2). doi:10.3847/1538-4357/adb968
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  We present a structural analysis of 520 galaxy candidates at 6.5 < z < 12.5 with a signal-to-noise ratio of >10σ in the F444W filter taken from the EPOCHS v1 sample, consisting of uniformly reduced deep JWST NIRCam data covering the CEERS, JADES GOODS-S, NGDEEP, SMACS-0723, GLASS, and PEARLS surveys. We use standard software to fit single Sérsic models to each galaxy in the rest-frame optical and extract their parametric structural parameters (Sérsic index, half-light radius, and axis ratio) and Morfometryka to measure their nonparametric concentration and asymmetry parameters. We find a wide range of sizes for these early galaxies, with galaxy sizes overall continuing to become progressively smaller in the high-redshift regime, following R e = 2.12 ± 0.28 1 + z − 0.67 ± 0.06 kpc. We further find a galaxy size-mass correlation up to z ∼ 12, with galaxies of a given mass also becoming smaller. Using nonparametric methods, we find that galaxy merger fractions, classified through asymmetry parameters, at these redshifts remain consistent with those in the literature, maintaining a value of fm ∼ 0.12 ± 0.07 showing little dependence with redshift when combined with the literature at z > 4. We find that galaxies that are smaller in size also appear rounder, with an excess of high axis ratio objects. Finally, we artificially redshift a subsample of our objects to determine how robust the observational trends we see are, determining that the observed trends are due to real evolutionary effects, rather than being a consequence of redshift effects.
• Frye, B. L. (2021). A Planck-selected dusty proto-cluster at z=2.16 associated with a strong over-density of massive H$α$ emitting galaxies. Koyama et al. 2021, MNRAS, 503, 1, 503.
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  We discovered an over-density of H-alpha-emitting galaxies associated with aPlanck compact source in the COSMOS field (PHzG237.0+42.5) through narrow-bandimaging observations with Subaru/MOIRCS. This Planck-selected dustyproto-cluster at z=2.16 has 38 H-alpha emitters including six spectroscopicallyconfirmed galaxies in the observed MOIRCS 4'x7' field (corresponding to~2.0x3.5~Mpc^2 in physical scale). We find that massive H-alpha emitters withlog(M*/Msun)>10.5 are strongly clustered in the core of the proto-cluster(within ~300-kpc from the density peak of the H-alpha emitters). Most of theH-alpha emitters in this proto-cluster lie along the star-forming main sequenceusing H-alpha-based SFR estimates, whilst the cluster total SFR derived byintegrating the H-alpha-based SFRs is an order of magnitude smaller than thoseestimated from Planck/Herschel FIR photometry. Our results suggest that H-alphais a good observable for detecting moderately star-forming galaxies and tracingthe large-scale environment in and around high-z dusty proto-clusters, butthere is a possibility that a large fraction of star formation could beobscured by dust and undetected in H-alpha observations.[Journal_ref: ]
• Frye, B. L. (2021). Spectroscopic observations of PHz G237.01+42.50: A galaxy protocluster at z=2.16 in the Cosmos field. Polletta et al. 2021, A&A, 654, 121.
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  The Planck satellite has identified more than 2000 protocluster candidateswith extreme star formation rates (SFRs). Here, we present the spectroscopicidentification of a Planck-selected protocluster located in the Cosmos field,PHz G237.01+42.50 (G237). G237 contains a galaxy overdensity of 31spectroscopically identified galaxies at z~2.16 (significant at 5.4 sigma) in a10'x11' region. The overdensity contains two substructures or protoclusters at~2.16 and 2.195 with estimated halo masses at z=0 of ~(5-6)x10^14 Msun. Theoverdensity total SFR, ~4000 Msun/yr, is higher than predicted by simulationsbut much smaller than the SFR derived from the Planck data. The analysis of theHerschel data, in combination with the available ancillary data, shows thatsuch a difference is due to an effect of source alignment along the line ofsight that produces a 5 sigma overdensity of red Herschel sources in the field.We analyze the members' UV spectra and UV-far-infrared spectral energydistributions to derive their SFR, stellar mass, and metallicity. Galaxymembers include blue star-forming galaxies and AGN with SFRs and stellar massesconsistent with the main sequence. AGN, identified through optical spectroscopyor X-ray data, represent a significant fraction (20+/-10%) of all members ofthe protocluster at z=2.16, and they are powerful enough to produce radiativefeedback. The core of this protocluster, besides being denser, includes membersthat are, on average, more massive and star-forming and contains a largerfraction of AGN and Herschel-detected galaxies than the full sample, suggestingan environmental effect on galaxy growth. A comparison between G237 and otherprotoclusters in the literature at similar redshifts reveals some common traitsand differences that reflect both observational biases and a diversity inintrinsic properties that is not yet fully understood.[Journal_ref: A&A 654, A121 (2021)]
• Frye, B. L., Harrington, K., Yun, M., Weiss, A., Magnelli, B., Sharon, C., Leung, T., Vishwas, A., Wang, Q., Frayer, D., Jimenez-Andrade, E., Liu, D., & Dannerbauer, H. (2021). Turbulent Gas in Lensed Planck-selected Starbursts at z = 1-3.5. Harrington et al. 2021, ApJ, 908, 30, 908, 54.
• Frye, B. L., Salmon, B., Coe, D., Bradley, L., Bouwens, R., Bradac, M., Huang, K., Oesch, P., Stark, D., & Trenti, M. (2021). VizieR Online Data Catalog: Brightest high-z galaxies in RELICS clusters. Data Release in July, 2021, from source paper: Salmon et al. (2020), ApJ, 889, 189S.
• Frye, B. L., Salmon, B., Coe, D., Bradley, L., Bouwens, R., Bradac, M., Huang, K., Oesch, P., Stark, D., & Trenti, M. (2021). VizieR Online Data Catalog: RELICS. Data Release in May 2021, from source paper: Coe et al. (2019), ApJ.
• Frye, B. L., Smith, G., Anguita, T., Birrer, S., Schechter, P., Verma, A., Collett, T., Courbin, F., Gavazzi, T., Lemon, C., More, A., Ryczanowski, D., & Suyu, S. (2021). Strong Lensing Science Collaboration input to the on-sky commissioning of the Vera Rubin Observatory. Astro-ph archives: arXiv:2111.09216, 8.
• Frye, B. L., Strait, V., Bradac, M., Coe, D., Lemaux, B., Carnall, A., Bradley, L., Pelliccia, D., Zitrin, A., Sharon, K., Acebron, A., Nonino, M., Oguri, M., & Ouchi, M. (2021). RELICS-DP7: Spectroscopic Confirmation of a Dichromatic Primeval Galaxy at z ∼ 7. Pelliccia et al. 2021, ApJ, 908, 30, 908, 8 pp.
• Frye, B. L., Strait, V., Bradac, M., Coe, D., Lemaux, B., Carnall, A., Bradley, L., Pelliccia, D., Zitrin, A., Sharon, K., Acebron, A., Nonino, M., Oguri, M., & Ouchi, M. (2021). RELICS: Properties of z ≥ 5.5 Galaxies Inferred from Spitzer and Hubble Imaging, Including A Candidate z ∼ 6.8 Strong [O III] emitter. Strait et al. 2021, ApJ, 910, 135, 910, 20 pp.
• Acebron, A., Zitrin, A., Coe, D., Mahler, G., Sharon, K., Oguri, M., Brada{v{c}}, M., Bradley, L. D., Frye, B., Forman, C. J., Strait, V., Su, Y., Umetsu, K., Andrade-Santos, F., Avila, R. J., Carrasco, D., Cerny, C., Czakon, N. G., Dawson, W. A., , Fox, C., et al. (2020). "RELICS: A Very Large (theta_E ~40″) Cluster Lens-RXC J0032.1+1808}". apj, 898(1), 6.
• Dai, L., Kaurov, A. A., Sharon, K., Florian, M. K., Miralda-Escud{'e}, J., Venumadhav, T., Frye, B., Rigby, J. R., & Bayliss, M. (2020). Asymmetric Surface Brightness Structure of Lensed Arc in SDSS J1226+2152: A Case for Dark Matter Substructure. arXiv e-prints, arXiv:2001.00261.
• Dai, L., Kaurov, A. A., Sharon, K., Florian, M., Miralda-Escud{'e}, J., Venumadhav, T., Frye, B., Rigby, J. R., & Bayliss, M. (2020). "Asymmetric surface brightness structure of caustic crossing arc in SDSS J1226+2152: a case for dark matter substructure". mnras, 495(3), 3192-3208.
• Mainali, R., Stark, D. P., Tang, M., Chevallard, J., Charlot, S., Sharon, K., Coe, D., Salmon, B., Bradley, L. D., Johnson, T. L., Frye, B., Avila, R. J., Ogaz, S., Zitrin, A., Brada{v{c}}, M., Lemaux, B. C., Mahler, G., Paterno-Mahler, R., Strait, V., & Andrade-Santos, F. (2020). "RELICS: spectroscopy of gravitationally lensed z ≃ 2 reionization-era analogues and implications for C III] detections at z > 6". mnras, 494(1), 719-735.
• Poudel, S., Kulkarni, V. P., Cashman, F. H., Frye, B., P{'eroux}, C., Rahmani, H., & Quiret, S. (2020). "Metal-enriched galaxies in the first {ensuremath{sim}1 billion years: evidence of a smooth metallicity evolution at z ensuremath{sim} 5}". mnras, 491(1), 1008-1025.
• Poudel, S., Kulkarni, V. P., Cashman, F. H., Frye, B., P{'eroux}, C., Rahmani, H., & Quiret, S. (2020). Metal-enriched galaxies in the first ~1 billion years: evidence of a smooth metallicity evolution at z ~ 5. MNRAS, 491(1), 1008-1025.
• Saha, A., Vivas, A., Olszewski, E., Smith, V., Olsen, K., Blum, R., Valdes, F., Claver, J., Calamida, A., Walker, A., Matheson, T., Narayan, G., Soraisam, M., Cunha, K., Axelrod, T., Bloom, J., Cenko, S., Frye, B., Juric, M., , Kaleida, C., et al. (2020). "VizieR Online Data Catalog: RRab stars toward Baade's window with Blanco/DECam (Saha+, 2019)". VizieR Online Data Catalog, J/ApJ/874/30.
• Salmon, B., Coe, D., Bradley, L., Bouwens, R., Brada{v{c}}, M., Huang, K., Oesch, P. A., Stark, D., Sharon, K., Trenti, M., Avila, R. J., Ogaz, S., Andrade-Santos, F., Carrasco, D., Cerny, C., Dawson, W., Frye, B. L., Hoag, A., Johnson, T. L., , Jones, C., et al. (2020). "RELICS: The Reionization Lensing Cluster Survey and the Brightest High-z Galaxies". apj, 889(2), 189.
• Steinhardt, C. L., Jauzac, M., Acebron, A., Atek, H., Capak, P., Davidzon, I., Eckert, D., Harvey, D., Koekemoer, A. M., Lagos, C. D., Mahler, G., Montes, M., Niemiec, A., Nonino, M., Oesch, P., Richard, J., Rodney, S. A., Schaller, M., Sharon, K., , Strolger, L., et al. (2020). "The BUFFALO HST Survey". apjs, 247(2), 64.
• Steinhardt, C. L., Jauzac, M., Acebron, A., Atek, H., Capak, P., Davidzon, I., Eckert, D., Harvey, D., Koekemoer, A. M., Lagos, C. D., Mahler, G., Montes, M., Niemiec, A., Nonino, M., Oesch, P., Richard, J., Rodney, S. A., Schaller, M., Sharon, K., , Strolger, L., et al. (2020). The BUFFALO HST Survey. arXiv e-prints, arXiv:2001.09999.
• Strait, V., Bradac, M., Coe, D., Lemaux, B. C., Carnall, A., Bradley, L., Pelliccia, D., Sharon, K., Zitrin, A., Acebron, A., Neufeld, C., Andrade-Santos, F., Avila, R. J., Frye, B. L., Mahler, G., Nonino, M., Ogaz, S., Oguri, M., Ouchi, M., , Paterno-Mahler, R., et al. (2020). "RELICS: Properties of z>5.5 Galaxies Inferred from Spitzer and Hubble Imaging Including A Candidate zraisebox{-0.5extextasciitilde6.8 Strong [OIII] Emitter}". arXiv e-prints, arXiv:2009.00020.
• Strait, V., Brada{v{c}}, M., Coe, D., Bradley, L., Salmon, B., Lemaux, B. C., Huang, K., Zitrin, A., Sharon, K., Acebron, A., Andrade-Santos, F., Avila, R. J., Frye, B. L., Hoag, A., Mahler, G., Nonino, M., Ogaz, S., Oguri, M., Ouchi, M., , Paterno-Mahler, R., et al. (2020). Stellar Properties of z >/= 8 Galaxies in the Reionization Lensing Cluster Survey. ApJ, 888(2), 124.
• Zitrin, A., Acebron, A., Coe, D., Kelly, P. L., Koekemoer, A. M., Nonino, M., Windhorst, R. A., Frye, B., Pascale, M., Broadhurst, T., Cohen, S. H., Diego, J. M., Finkelstein, S. L., Jansen, R. A., Larson, R. L., Yan, H., Alpaslan, M., Bhatawdekar, R., Conselice, C. J., , Griffiths, A., et al. (2020). "A Strong-lensing Model for the WMDF JWST/GTO Very Rich Cluster A1489". apj, 903(2), 137.
• Acebron, A., Alon, M., Zitrin, A., Mahler, G., Coe, D., Sharon, K., Cibirka, N., Brada{v{c}}, M., Trenti, M., Umetsu, K., Andrade-Santos, F., Avila, R. J., Bradley, L., Carrasco, D., Cerny, C., Czakon, N. G., Dawson, W. A., Frye, B., Hoag, A. T., , Huang, K., et al. (2019). RELICS: High-resolution Constraints on the Inner Mass Distribution of the z = 0.83 Merging Cluster RXJ0152.7-1357 from Strong Lensing. ApJ, 874(2), 132.
• Acebron, A., Zitrin, A., Coe, D., Mahler, G., Sharon, K., Oguri, M., Brada{v{c}}, M., Bradley, L., Frye, B., Forman, C. J., Strait, V., Su, Y., Umetsu, K., Andrade-Santos, F., Avila, R. J., Carrasco, D., Cerny, C., Czakon, N. G., Dawson, W. A., , Fox, C., et al. (2019). RELICS: A Very Large ($theta_Esim40"$) Cluster Lens -- RXC J0032.1+1808. arXiv e-prints, arXiv:1912.02702.
• Bechtol, K., Drlica-Wagner, A., Abazajian, K. N., Abidi, M., Adhikari, S., Ali-Ha{iensuremath{ddot{}}moud}, Y., Annis, J., Ansarinejad, B., Armstrong, R., Asorey, J., Baccigalupi, C., Banerjee, A., Banik, N., Bennett, C., Beutler, F., Bird, S., Birrer, S., Biswas, R., Biviano, A., , Blazek, J., et al. (2019). Dark Matter Science in the Era of LSST. baas, 51(3), 207.
• Coe, D., Salmon, B., Brada{v{c}}, M., Bradley, L. D., Sharon, K., Zitrin, A., Acebron, A., Cerny, C., Cibirka, N., Strait, V., Paterno-Mahler, R., Mahler, G., Avila, R. J., Ogaz, S., Huang, K., Pelliccia, D., Stark, D. P., Mainali, R., Oesch, P. A., , Trenti, M., et al. (2019). RELICS: Reionization Lensing Cluster Survey. ApJ, 884(1), 85.
• Dannerbauer, H., Kampen, E., Afonso, J., Andreani, P., Battaia, F. A., Bertoldi, F., Casey, C., Chen, C., Clements, D. L., De, B. C., Frye, B., Geach, J., Harrington, K., Hayashi, M., Jin, S., Klaassen, P., Kohno, K., Lehnert, M. D., Matute, I., , Mroczkowski, T., et al. (2019). Mapping Galaxy Clusters in the Distant Universe. baas, 51(3), 293.
• Fogarty, K., Postman, M., Li, Y., Dannerbauer, H., Liu, H. B., Donahue, M., Ziegler, B., Koekemoer, A., & Frye, B. (2019). The Dust and Molecular Gas in the Brightest Cluster Galaxy in MACS 1931.8-2635. ApJ, 879(2), 103.
• Frye, B. L., Bowen, D. V., Tripp, T. M., Jenkins, E. B., Pettini, M., & Ellison, S. L. (2019). A Sub-damped Lyman-alpha Absorber with Unusual Abundances: Evidence of Gas Recycling in a Low-redshift Galaxy Group. ApJ, 872(2), 129.
• Frye, B. L., McGreer, I., Clement, B., Mainali, R., Stark, D., Gronke, M., Dijkstra, M., Fan, X., Bian, F., Jiang, L., Kneib, J., Limousin, M., & Walth, G. (2017). A bright lensed galaxy at $z=5.4$ with strong Ly$alpha$ emission. MNRAS, 19.
• Frye, B. L., Pascale, M., Qin, Y., Zitrin, A., Diego, J., Walth, G., Yan, H., Conselice, C. J., Alpaslan, M., Bauer, A., Busoni, L., Coe, D., Cohen, S. H., Dole, H., Donahue, M., Georgiev, I., Jansen, R. A., Limousin, M., Livermore, R., , Norman, D., et al. (2019). PLCK G165.7+67.0: Analysis of a Massive Lensing Cluster in a Hubble Space Telescope Census of Submillimeter Giant Arcs Selected Using Planck/Herschel. ApJ, 871(1), 51.
• Kaurov, A. A., Dai, L., Venumadhav, T., Miralda-Escud{'e}, J., & Frye, B. (2019). Highly Magnified Stars in Lensing Clusters: New Evidence in a Galaxy Lensed by MACS J0416.1-2403. ApJ, 880(1), 58.
• Kneissl, R., Polletta, M., Martinache, C., Hill, R., Clarenc, B., Dole, H. A., Nesvadba, N. P., Scott, D., B{'ethermin}, M., Frye, B., Giard, M., Lagache, G., & Montier, L. (2019). Using ALMA to resolve the nature of the early star-forming large-scale structure PLCK G073.4-57.5. A&A, 625, A96.
• Koekemoer, A., Foley, R., Spergel, D., Bagley, M., Bezanson, R., Bianco, F., Capak, P., De Rosa, G., Dickinson, M., Dore, O., Fan, X., Fazio, G., Ferguson, H., Filippenko, A., Finkelstein, S., Frye, B., Gawiser, E., Grogin, N., Hathi, N., , Hirata, C., et al. (2019). Ultra Deep Field Science with WFIRST. baas, 51(3), 550.
• 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/Virgotextquoterights Third Observing Run. ApJL, 881(2), L26.
• Mahler, G., Sharon, K., Fox, C., Coe, D., Jauzac, M., Strait, V., Edge, A., Acebron, A., Andrade-Santos, F., Avila, R. J., Brada{v{c}}, M., Bradley, L. D., Carrasco, D., Cerny, C., Cibirka, N., Czakon, N. G., Dawson, W. A., Frye, B. L., Hoag, A. T., , Huang, K., et al. (2019). RELICS: Strong Lensing Analysis of MACS J0417.5-1154 and Predictions for Observing the Magnified High-redshift Universe with JWST. ApJ, 873(1), 96.
• Mainali, R., Stark, D. P., Tang, M., Chevallard, J., Charlot, S., Sharon, K., Coe, D., Salmon, B., Bradley, L. D., Johnson, T. L., Frye, B., Avila, R. J., Ogaz, S., Zitrin, A., Brada{v{c}}, M., Lemaux, B. C., Mahler, G., Paterno-Mahler, R., Strait, V., & Andrade-Santos, F. (2019). RELICS: Spectroscopy of gravitationally-lensed z ~ 2 reionization-era analogs and implications for CIII] detections at z > 6. arXiv e-prints, arXiv:1909.09212.
• Mantz, A., Allen, S. W., Battaglia, N., Benson, B., Canning, R., Ettori, S., Evrard, A., Linden, A., McDonald, M., Abidi, M., Ahmed, Z., Amin, M. A., Ansarinejad, B., Armstrong, R., Avestruz, C., Baccigalupi, C., Bandura, K., Barkhouse, W., Basu, K. m., , Bavdhankar, C., et al. (2019). The Future Landscape of High-Redshift Galaxy Cluster Science. baas, 51(3), 279.
• Rabien, S., Angel, R., Barl, L., Beckmann, U., Busoni, L., Belli, S., Bonaglia, M., Borelli, J., Brynnel, J., Buschkamp, P., Cardwell, A., Contursi, A., Connot, C., Davies, R., Deysenroth, M., Durney, O., Eisenhauer, F., Elberich, M., Esposito, S., , Frye, B., et al. (2019). ARGOS at the LBT. Binocular laser guided ground-layer adaptive optics. A&A, 621, A4.
• Rieke, M., Arribas, S., Bunker, A., Charlot, S., Finkelstein, S., Maiolino, R., Robertson, B., Willott, C., Windhorst, R., Eisenstein, D., Nelson, E., Tacchella, S., Egami, E., Endsley, R., Frye, B., Hainline, K., Hviding, R., Rieke, G., Williams, C., , Willmer, C., et al. (2019). JWST GTO/ERS Deep Surveys. baas, 51(3), 45.
• Saha, A., Vivas, A. K., Olszewski, E. W., Smith, V., Olsen, K., Blum, R., Valdes, F., Claver, J., Calamida, A., Walker, A. R., Matheson, T., Narayan, G., Soraisam, M., Cunha, K., Axelrod, T., Bloom, J. S., Cenko, S. B., Frye, B., Juric, M., , Kaleida, C., et al. (2019). Mapping the Interstellar Reddening and Extinction toward Baadetextquoterights Window Using Minimum Light Colors of ab-type RR Lyrae Stars: Revelations from the De-reddened Color-Magnitude Diagrams. ApJ, 874(1), 30.
• Windhorst, R., Alpaslan, M., Andrews, S., Ashcraft, T., Broadhurst, T., Coe, D., Conselice, C., Cohen, S., Diego, J., Dijkstra, M., Driver, S., Duncan, K., Finkelstein, S., Frye, B., Griffiths, A., Grogin, N., Hathi, N., Hopkins, A., Jansen, R., , Joshi, B., et al. (2019). On the observability of individual Population III stars and their stellar-mass black hole accretion disks through cluster caustic transits. baas, 51(3), 449.
• Acebron, A., Cibirka, N., Zitrin, A., Coe, D., Agulli, I., Sharon, K., Bradac, M., Frye, B. L., Livermore, R., Mahler, G., & (total of 40 authors), e. a. (2018). RELICS: Strong-lensing Analysis of the Massive Clusters MACS J0308.9+2645 and PLCK G171.9-40.7. ApJ, 858, 42A.
• Cerny, C., Sharon, K., Andrade-Santos, F., Avila, R., Bradac, M., Bradley, L., Carrasco, D., Coe, D., Czakon, N., Frye, B. L., & (total of 34 authors), e. a. (2018). RELICS: Strong Lens Models for Five Galaxy Clusters from the Reionization Lensing Cluster Survey. ApJ, 859, 159C.
• Cibirka, N., Acebron, A., Zitrin, A., Coe, D., Agulli, I., Andrade-Santos, F., Bradac, M., Frye, B. L., Livermore, R., Mahler, G., & (total of 40 authors), e. a. (2018). RELICS: Strong Lensing Analysis of the Galaxy Clusters Abell S295, Abell 697, MACS J0025.4-1222, and MACS J0159.8-0849. ApJ, 863, 145C.
• Diego, J., Kaiser, N., Broadhurst, T., Kelly, P., Rodney, S., Morishita, T., Oguri, M., Ross, T., Zitrin, A., Jauzac, M., Richard, J., Williams, L., Vega-Ferrero, J., Frye, B. L., & Filippenko, A. (2018). Dark Matter under the Microscope: Constraining Compact Dark Matter with Caustic Crossing Events. ApJ, 857, 25.
• Griffiths, A., Conselice, C., Alpaslan, M., Frye, B. L., Diego, J., Zitrin, A., Yan, H., Ma, Z., Barone-Nugent, R., Bhatawdekhar, R., Driver, S., Robotham, A., Windhorst, R., & Wyithe, S. (2018). MUSE spectroscopy and deep observations of a unique compact JWST target, lensing cluster CLIO. MNRAS, 475, 2853G.
• Jimenez-Teja, Y., Dupke, R., Benitez, N., Koekemoer, A., Zitrin, A., Umetsu, K., Ziegler, B., Frye, B. L., Ford, H., Bouwens, R., & (total of 37 authors), e. a. (2018). Unveiling the Dynamical State of Massive Clusters through the ICL Fraction. ApJ, 857, 79J.
• Kelly, P., Diego, J., Rodney, S., Kaiser, N., Broadhurst, T., Zitrin, A., Treu, T., Perez-Gonzales, P., Morishita, T., Frye, B. L., & (total of 45 authors), e. a. (2018). Extreme magnification of an individual star at redshift 1.5 by a galaxy-cluster lens. Nature, 2, 334-342.
• Martinache, C., Rettura, A., Dole, H., Lehnert, M., Frye, B. L., Altieri, B., Beelen, A., Bethermin, M., Le Floc'h, E., Giard, M., Hurier, G., Lagache, L., Montier, L., Omont, A., Pointecouteau, E., Polletta, M., Puget, J., Scott, D., Soucail, G., & Welikala, N. (2018). Spitzer Planck Herschel Infrared Cluster (SPHerIC) survey: Candidate galaxy clusters at 1.3 < z < 3 selected by high star-formation rate. A&A, 620, 198M.
• McGreer, I., Clement, B., Mainali, R., Stark, D., Gronke, M., Dijkstra, M., Fan, X., Bian, F., Frye, B. L., L., J., Kneib, J., Limousin, M., & Walth, G. (2018). A bright-lensed galaxy at z = 5.4 with strong Ly α emission. ApJ, 864, 22S.
• Paterno-Mahler, R., Sharon, K., Coe, D., Mahler, G., Cerny, C., Johnson, T., Schrabback, T., Andrade-Santos, F., Avila, R., Bradac, M., Bradley, L., Frye, B. L., & (total of 33 authors), e. a. (2018). RELICS: A Strong Lens Model for SPT-CLJ0615–5746, a z = 0.972 Cluster. ApJ, 863, 154P.
• Rabien, S., Angel, R., Barl, L., Beckmann, U., Busoni, L., Belli, S., Bonaglia, M., Borelli, J., Brynnel, J., Bushcamp, P., Cardwell, A., Contursi, A., Connot, C., Davies, R., Deysenroth, M., Durney, O., Eisenhauer, F., Elberich, M., Esposito, S., , Frye, B. L., et al. (2018). ARGOS at the LBT. Binocular laser guided ground-layer adaptive optics. A&A, 621, 4.
• Salmon, B., Coe, D., Bradley, L., Bradac, M., Strait, V., Paterno-Mahler, R., Huang, K., Oesch, P., Zitrin, A., Acebron, A., Cibirka, N., Frye, B. L., & (total of 30 authors), e. a. (2018). RELICS: A Candidate z ∼ 10 Galaxy Strongly Lensed into a Spatially Resolved Arc. ApJ, 864, 22S.
• Umetsu, K., Sereno, M., Tam, S., Chiu, I., Fan, Z., Ettori, S., Gruen, D., Okumura, T., Medezinski, E., Donahue, M., Meneghetti, M., Frye, B. L., & (total of 27 authors), e. a. (2018). The Projected Dark and Baryonic Ellipsoidal Structure of 20 CLASH Galaxy Clusters. ApJ, 860, 104U.
• Frye, B. L., Cai, Z., Fan, X., Bian, F., Zabludoff, A., Yang, Y., Prochaska, X., McGreer, I., Zheng, Z., Kashikawa, N., Wang, R., Green, R., & Jiang, L. (2017). Mapping the Most Massive Overdensities through Hydrogen (MAMMOTH). II. Discovery of the Extremely Massive Overdensity BOSS1441 at z = 2.32. ApJ, 839, 131- 142.
• Frye, B. L., Cai, Z., Yang, Y., Bian, F., Prochaska, X., Zabludoff, A., McGreer, I., Zheng, Z., Green, R., Cantolupo, S., Hamden, E., Jiang, L., Kashikawa, N., & Wang, R. (2017). Discovery of an Enormous Lyα Nebula in a Massive Galaxy Overdensity at z = 2.3. ApJ, 837(1), 71 - 81.
• Frye, B. L., Canameras, R., Nesvadba, N., Kneissl, R., Gavazzi, R., Koenig, S., Le Floc 'h, E., Limousin, M., Oteo, I., & Scott, D. (2017). Planck's dusty GEMS. IV. Star formation and feedback in a maximum starburst at z = 3 seen at 60-pc resolution. A&A, 604, 11.
• Frye, B. L., Canameras, R., Nesvadba, N., Kneissl, R., Limousin, M., Gavazzi, R., Scott, D., Dole, H., Koenig, S., Le Floc 'h, E., & Oteo, I. (2017). Planck's dusty GEMS. III. A massive lensing galaxy with a bottom-heavy stellar initial mass function at z = 1.5. A&A, 600, 3-8.
• Frye, B. L., Malhotra, S., Rhoads, J., Finkelstein, K., Yang, H., Carilli, C., Combes, F., Dassas, K., Finkelstein, S., Gerin, M., Guillard, P., Nesvadba, N., Rigby, J., Shin, M., Spaans, M., Strauss, M., & Papovich, C. (2017). Herschel Extreme Lensing Line Observations: [CII] Variations in Galaxies at Redshifts z=1-. ApJ, 835(1), 110-119.
• Frye, B. L., Monna, A., Seitz, S., Balestra, I., Rosati, P., Grillo, C., Halkola, A., Suyu, S., Coe, D., Caminha, G., Koekemoer, A., Mercurio, A., Nonino, M., Postman, M., & Zitrin, A. (2017). Precise strong lensing mass profile of the CLASH galaxy cluster MACS 2129. MNRAS, 466, 4094-4106.
• , D. V., , D. C., , E. B., , T. M., , M. P., , D. G., & , B. L. (2016). The Structure of the Circumgalactic Medium of Galaxies: Cool Accretion Inflow Around NGC 1097.
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  We present Hubble Space Telescope far-UV spectra of 4 QSOs whose sightlinespass through the halo of NGC 1097 at impact parameters of 48 -165 kpc. NGC 1097is a nearby spiral galaxy that has undergone at least two minor merger events,but no apparent major mergers, and is relatively isolated with respect to othernearby bright galaxies. This makes NGC 1097 a good case study for exploringbaryons in a paradigmatic bright-galaxy halo. Lyman-alpha absorption isdetected along all sightlines and Si III 1206 is found along the 3 smallestimpact parameter sightlines; metal lines of C II, Si II and Si IV are onlyfound with certainty towards the inner-most sightline. The kinematics of theabsorption lines are best replicated by a model with a disk-like distributionof gas approximately planar to the observed 21 cm H I disk, that is rotatingmore slowly than the inner disk, and into which gas is infalling from theintergalactic medium. Some part of the absorption towards the inner-mostsightline may arise either from a small-scale outflow, or from tidal debrisassociated with the minor merger that gives rise to the well known `dog-leg'stellar stream that projects from NGC 1097. When compared to other studies, NGC1097 appears to be a `typical' absorber, although the large dispersion inabsorption line column density and equivalent width in a single halo goesperhaps some way in explaining the wide range of these values seen inhigher-redshift studies.[Journal_ref: ]
• , G. B., , C. G., , P. R., , I. B., , W. K., , M. L., , A. M., , M. N., , P. T., , A. Z., , A. B., , M. G., , A. M., , P. M., , M. M., , E. M., , S. H., , K. U., , M. A., , , S. B., et al. (2016). CLASH-VLT: A Highly Precise Strong Lensing Model of the Galaxy Cluster RXC J2248.7-4431 (Abell S1063) and Prospects for Cosmography. A&A.
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  We perform a comprehensive study of the total mass distribution of the galaxycluster RXCJ2248 ($z=0.348$) with a set of high-precision strong lensingmodels, which take advantage of extensive spectroscopic information on manymultiply lensed systems. In the effort to understand and quantify inherentsystematics in parametric strong lensing modelling, we explore a collection of22 models where we use different samples of multiple image families,parametrizations of the mass distribution and cosmological parameters. As inputinformation for the strong lensing models, we use the CLASH HST imaging dataand spectroscopic follow-up observations, carried out with the VIMOS and MUSEspectrographs, to identify bona-fide multiple images. A total of 16 backgroundsources, over the redshift range $1.0-6.1$, are multiply lensed into 47 images,24 of which are spectroscopically confirmed and belong to 10 individualsources. The cluster total mass distribution and underlying cosmology in themodels are optimized by matching the observed positions of the multiple imageson the lens plane. We show that with a careful selection of a sample ofspectroscopically confirmed multiple images, the best-fit model reproducestheir observed positions with a rms of $0.3$ in a fixed flat $\Lambda$CDMcosmology, whereas the lack of spectroscopic information lead to biases in thevalues of the model parameters. Allowing cosmological parameters to varytogether with the cluster parameters, we find (at $68\%$ confidence level)$\Omega_m=0.25^{+0.13}_{-0.16}$ and $w=-1.07^{+0.16}_{-0.42}$ for a flat$\Lambda$CDM model, and $\Omega_m=0.31^{+0.12}_{-0.13}$ and$\Omega_\Lambda=0.38^{+0.38}_{-0.27}$ for a universe with $w=-1$ and freecurvature. Using toy models mimicking the overall configuration of RXCJ2248, weestimate the impact of the line of sight mass structure on the positional rmsto be $0.3\pm 0.1$.(ABRIDGED)[Journal_ref: A&A 587, A80 (2016)]
• , I. B., , A. M., , B. S., , M. G., , C. G., , M. N., , P. R., , A. B., , S. E., , W. F., , C. J., , A. K., , E. M., , J. M., , G. A., , P. T., , K. U., , E. V., , R. J., , , A. Z., et al. (2016). CLASH-VLT: Dissecting the Frontier Fields Galaxy Cluster MACS J0416.1-2403 with $\sim800$ Spectra of Member Galaxies.
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  We present VIMOS-VLT spectroscopy of the Frontier Fields clusterMACS~J0416.1-2403 (z=0.397). Taken as part of the CLASH-VLT survey, the largespectroscopic campaign provided more than 4000 reliable redshifts, including~800 cluster member galaxies. The unprecedented sample of cluster members atthis redshift allows us to perform a highly detailed dynamical and structuralanalysis of the cluster out to ~2.2$r_{200}$ (~4Mpc). Our analysis ofsubstructures reveals a complex system composed of a main massive cluster($M_{200}$~0.9$\times 10^{15} M_{\odot}$) presenting two major features: i) abimodal velocity distribution, showing two central peaks separated by $\DeltaV_{rf}$~1100 km s$^{-1}$ with comparable galaxy content and velocitydispersion, ii) a projected elongation of the main substructures along theNE-SW direction, with a prominent subclump ~600 kpc SW of the center and anisolated BCG approximately halfway between the center and the SW clump. We alsodetect a low mass structure at z~0.390, ~10' S of the cluster center, projectedat ~3Mpc, with a relative line-of-sight velocity of $\Delta V_{rf}$~-1700 kms$^{-1}$. The cluster mass profile that we obtain through our dynamicalanalysis deviates significantly from the "universal" NFW, being best fit by aSoftened Isothermal Sphere model instead. The mass profile measured from thegalaxy dynamics is found to be in relatively good agreement with those obtainedfrom strong and weak lensing, as well as with that from the X-rays, despite theclearly unrelaxed nature of the cluster. Our results reveal overall a complexdynamical state of this massive cluster and support the hypothesis that the twomain subclusters are being observed in a pre-collisional phase, in line withrecent findings from radio and deep X-ray data. With this article we alsorelease the entire redshift catalog of 4386 sources in the field of thiscluster.[Journal_ref: ]
• , L. P., , B. S., , S. B., , L. A., , K. U., , A. B., , M. G., , P. R., , I. B., , G. B., , B. F., , A. K., , C. G., , M. L., , A. M., & , M. N. (2016). CLASH-VLT: Testing the Nature of Gravity with Galaxy Cluster Mass Profiles.
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  We use high-precision kinematic and lensing measurements of the total massprofile of the dynamically relaxed galaxy cluster MACS J1206.2-0847 at $z=0.44$to estimate the value of the ratio $\eta=\Psi/\Phi$ between the two scalarpotentials in the linear perturbed Friedmann-Lemaitre-Robertson-Walkermetric.[...] Complementary kinematic and lensing mass profiles were derivedfrom exhaustive analyses using the data from the Cluster Lensing And Supernovasurvey with Hubble (CLASH) and the spectroscopic follow-up with the Very LargeTelescope (CLASH-VLT). Whereas the kinematic mass profile tracks only thetime-time part of the perturbed metric (i.e. only $\Phi$), the lensing massprofile reflects the contribution of both time-time and space-space components(i.e. the sum $\Phi+\Psi$). We thus express $\eta$ as a function of the massprofiles and perform our analysis over the radial range $0.5\,Mpc\le r\ler_{200}=1.96\,Mpc$. Using a spherical Navarro-Frenk-White mass profile, whichwell fits the data, we obtain $\eta(r_{200})=1.01\,_{-0.28}^{+0.31}$ at the68\% C.L. We discuss the effect of assuming different functional forms for massprofiles and of the orbit anisotropy in the kinematic reconstruction.Interpreting this result within the well-studied $f(R)$ modified gravity model,the constraint on $\eta$ translates into an upper bound to the interactionlength (inverse of the scalaron mass) smaller than 2 Mpc. This tight constrainton the $f(R)$ interaction range is however substantially relaxed whensystematic uncertainties in the analysis are considered. Our analysishighlights the potential of this method to detect deviations from generalrelativity, while calling for the need of further high-quality data on thetotal mass distribution of clusters and improved control on systematic effects.[Journal_ref: ]
• , M. A., , A. M., , A. B., , M. G., , M. N., , I. B., , P. R., , G. B., , M. B., , R. G., , C. G., , M. L., , B. S., , G. D., , R. D., , B. F., , A. F., , J. M., , M. S., , , U. K., et al. (2016). CLASH-VLT: Environment-driven evolution of galaxies in the z=0.209 cluster Abell 209. A&A.
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  The analysis of galaxy properties and the relations among them and theenvironment, can be used to investigate the physical processes driving galaxyevolution. We study the cluster A209 by using the CLASH-VLT spectroscopic datacombined with Subaru photometry, yielding to 1916 cluster members down to astellar mass of 10^{8.6} Msun. We determine: i) the stellar mass function ofstar-forming and passive galaxies; ii) the intra-cluster light and itsproperties; iii) the orbits of low- and high-mass passive galaxies; and iv) themass-size relation of ETGs. The stellar mass function of the star-forminggalaxies does not depend on the environment, while the slope found for passivegalaxies becomes flatter in the densest region. The color distribution of theintra-cluster light is consistent with the color of passive members. Theanalysis of the dynamical orbits shows that low-mass passive galaxies havetangential orbits, avoiding small pericenters around the BCG. The mass-sizerelation of low-mass passive ETGs is flatter than that of high mass galaxies,and its slope is consistent with that of field star-forming galaxies. Low-massgalaxies are also more compact within the scale radius of 0.65 Mpc. The ratiobetween stellar and number density profiles shows a mass segregation in thecenter. The comparative analysis of the stellar and total density profilesindicates that this effect is due to dynamical friction. Our results areconsistent with a scenario in which the "environmental quenching" of low-massgalaxies is due to mechanisms such as harassment out to R200, starvation andram-pressure stripping at smaller radii, as supported by the analysis of themass function, of the dynamical orbits and of the mass-size relation of passiveearly-types in different regions. Our analyses support the idea that theintra-cluster light is formed through the tidal disruption of subgiantgalaxies.[Journal_ref: A&A 585, A160 (2016)]
• , N. N., , R. K., , R. C., , F. B., , E. F., , B. F., , M. G., , S. K., , G. L., , E. L., , S. M., & , D. S. (2016). Planck's Dusty GEMS. II. Extended [CII] emission and absorption in the Garnet at z=3.4 seen with ALMA.
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  We present spatially resolved ALMA [CII] observations of the bright (fluxdensity S=400 mJy at 350 microns), gravitationally lensed, starburst galaxyPLCK G045.1+61.1 at z=3.427, the "Garnet". This source is part of our set of"Planck's Dusty GEMS", discovered with the Planck's all-sky survey. Twoemission-line clouds with a relative velocity offset of ~600 km/s extendtowards north-east and south-west, respectively, of a small, intenselystar-forming clump with a star-formation intensity of 220 Msun/yr/kpc^2, akinto maximal starbursts. [CII] is also seen in absorption, with a redshift of+350 km/s relative to the brightest CO component. [CII] absorption haspreviously only been found in the Milky Way along sightlines toward brighthigh-mass star-forming regions, and this is the first detection in anothergalaxy. Similar to Galactic environments, the [CII] absorption feature isassociated with [CI] emission, implying that this is diffuse gas shielded fromthe UV radiation of the clump, and likely at large distances from the clump.Since absorption can only be seen in front of a continuum source, the gas inthis structure can definitely be attributed to gas flowing towards the clump.The absorber could be part of a cosmic filament or merger debris being accretedonto the galaxy. We discuss our results also in light of the on-going debate ofthe origin of the [CII] deficit in dusty star-forming galaxies.[Journal_ref: ]
• , Z. C., , X. F., , F. B., , A. Z., , Y. Y., , J. X., , I. M., , Z. Z., , N. K., , R. W., , B. F., , R. G., & , L. J. (2016). MApping the Most Massive Overdensities (MAMMOTH) II -- Discovery of an Extremely Massive Overdensity BOSS1441 at $z=2.32$.
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  Cosmological simulations suggest a strong correlation between highoptical-depth Ly$\alpha$ absorbers, which arise from the intergalactic medium(IGM), and 3-D mass overdensities on scales of $10-30$ $h^{-1}$ comoving Mpc.By examining the absorption spectra of $\sim$ 80,000 QSO sight-lines over avolume of 0.1 Gpc$^3$ in the Sloan Digital Sky Survey III (SDSS-III), we haveidentified an extreme overdensity, BOSS1441, which contains a rare group ofstrong Ly$\alpha$ absorbers at $z=2.32\pm 0.02$. This absorber group isassociated with six QSOs at the same redshift on a 30 comoving Mpc scale. UsingMayall/MOSAIC narrowband and broadband imaging, we detect Ly$\alpha$ emitters(LAEs) down to $0.7\times L_{\rm{Ly\alpha}}^*$, and reveal a large-scalestructure of Ly$\alpha$ emitters (LAEs) in this field. Our follow-up LargeBinocular Telescope (LBT) observations have spectroscopically confirmed 19galaxies in the density peak. We show that BOSS1441 has an LAE overdensity of$10.8\pm 2.6$ on a 15 comoving Mpc scale which could collapse to a massivecluster with $M\gtrsim10^{15}$ M$_\odot$ at $z\sim0$. This overdensity is amongthe most massive large-scale structures at $z\sim2$ discovered to date.[Journal_ref: ]
• , Z. C., , X. F., , S. P., , F. B., , B. F., , I. M., , J. X., , M. W., , N. T., , S. H., & , D. P. (2016). MApping the Most Massive Overdensities Through Hydrogen (MAMMOTH) I: Methodology.
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  Modern cosmology predicts that a galaxy overdensity is associated to a largereservoir of the intergalactic gas, which can be traced by the Ly$\alpha$forest absorption. We have undertaken a systematic study of the relationbetween Coherently Strong intergalactic Ly$\alpha$ Absorption systems (CoSLAs),which have highest optical depth ($\tau$) in $\tau$ distribution, and massoverdensities on the scales of $\sim$ 10 - 20 $h^{-1}$ comoving Mpc. On suchlarge scales, our cosmological simulations show a strong correlation betweenthe effective optical depth ($\tau_{\rm{eff}}$) of the CoSLAs and the 3-D massoverdensities. In moderate signal-to-noise spectra, however, the profiles ofCoSLAs can be confused with high column density absorbers. For $z>2.6$, wherethe corresponding Ly$\beta$ is redshifted to the optical, we have developed thetechnique to differentiate between these two alternatives. We have applied thistechnique to SDSS-III quasar survey at $z = 2.6$ - 3.3, and we present a sampleof five CoSLA candidates with $\tau_{\rm{eff}}$ on 15 $h^{-1}$ Mpc greater than$4.5\times$ the mean optical depth. At lower redshifts of $z < 2.6$, where thebackground quasar density is higher, the overdensity can be traced byintergalactic absorption groups using multiple sight lines. Our overdensitysearches fully utilize the current and next generation of Ly$\alpha$ forestsurveys which cover a survey volume of $> (1\ h^{-1}$ Gpc)$^3$. In addition,systems traced by CoSLAs will build a uniform sample of the most massiveoverdensities at $z > 2$ to constrain the models of structure formation, andoffer a unique laboratory to study the interactions between galaxyoverdensities and the intergalactic medium.[Journal_ref: ]
• Frye, B. L. (2016). The Detection and Statistics of Giant Arcs Behind CLASH Clusters. ApJ, 817, 85.
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  We developed an algorithm to find and characterize gravitationally lensedgalaxies (arcs) to perform a comparison of the observed and simulated arcabundance. Observations are from the Cluster Lensing And Supernova survey withHubble (CLASH). Simulated CLASH images are created using the MOKA package andalso clusters selected from the high resolution, hydrodynamical simulations,MUSIC, over the same mass and redshift range as the CLASH sample. Thealgorithm' s arc elongation accuracy, completeness and false positive rate aredetermined and used to compute an estimate of the true arc abundance. We derivea lensing efficiency of $4 \pm 1$ arcs (with length $\ge 6"$ andlength-to-width ratio $\ge 7$) per cluster for the X-ray selected CLASH sample,$4 \pm 1$ arcs per cluster for the MOKA simulated sample and $3 \pm 1$ arcs percluster for the MUSIC simulated sample. The observed and simulated arcstatistics are in full agreement. We measure the photometric redshifts of alldetected arcs and find a median redshift $z_s = 1.9$ with 33% of the detectedarcs having $z_s > 3$. We find that the arc abundance does not depend stronglyon the source redshift distribution but is sensitive to the mass distributionof the dark matter halos (e.g. the $c-M$ relation). Our results show thatconsistency between the observed and simulated distributions of lensed arcsizes and axial ratios can be achieved by using cluster-lensing simulationsthat are carefully matched to the selection criteria used in the observations.[Journal_ref: ]
• 176 authors, P. C., & Frye, B. (2015). Planck intermediate results: XXVII. High-redshift infrared galaxy overdensity candidates and lensed sources by Planck and confirmed by Herschel-SPIRE. A&A, 582, 30.
• Bian, F., Stark, D., Fan, X., Jiang, L., Clement, B., Egami, E., Frye, B. L., Green, R., McGreer, I., & Cai, Z. (2015). LBT/LUCI Spectroscopic Observations of z≃7 Galaxies. ApJ, 806, 108.
• Canameras, R., Nesvadba, N., Guery, D., McKenzie, T., Koenig, S., Petitpas, G., Dole, H., Frye, B., Flores-Cacho, I., Montier, L., Negrello, M., Beelen, A., Boone, F., Dicken, D., Lagache, G., Le~Floc'h, E., Altieri, B., Bethermin, M., Chary, R., , de~Zotti, G., et al. (2015). Planck's Dusty GEMS: The brightest gravitationally lensed galaxies discovered with the Planck all-sky survey. A&A, 581, 105.
• Grillo, C., Suyu, S. H., Rosati, P., Mercurio, A., Balestra, I., Munari, E., Nonino, M., Caminha, G. B., Lombardi, M., De Lucia, G., Borgani, S., Gobat, R., Biviano, A., Girardi, M., Umetsu, K., Coe, D., Koekemoer, A. M., Postman, M., Zitrin, A., , Halkola, A., et al. (2015). CLASH-VLT: Insights on the mass substructures in the Frontier Fields Cluster MACS J0416.1-2403 through accurate strong lens modeling. ApJ, 800, 38.
• Huang, X., Zheng, W., Wang, J., Ford, H., Lemze, D., Moustakas, J., Shu, X., Wel, A., Zitrin, A., Frye, B. L., Postman, M., Bartelmann, M., Benitez, N., Bradley, L., Broadhurst, T., Coe, D., Donahue, M., Infante, L., Kelson, D., , Koekemoer, A., et al. (2015). CLASH: Extreme Emission Line Galaxies and Their Implication on Selection of High-Redshift Galaxies. ApJ, 801, 12.
• Pirzkal, N., Coe, D., Frye, B., Brammer, G., Moustakas, J., Rothberg, B., Broadhurst, T., Bouwens, R., Bradley, L., Wel, A., Kelson, D., Donahue, M., Zitrin, A., Moustakas, L., & Barker, E. (2015). Not in Our Backyard: Spectroscopic Support for the z=11 CLASH MACSJ0647.7+7015 Candidate. ApJ, 65, 112.
• Zitrin, A., Fabris, A., Merten, J., Melchior, P., Meneghetti, M., Koekemoer, A., Coe, D., Maturi, M., Bartelmann, M., Postman, M., Umetsu, K., Seidel, G., Sendra, I., Broadhurst, T., Balestra, I., Biviano, A., Grillo, C., Mercurio, A., Nonino, M., , Rosati, P., et al. (2015). Hubble Space Telescope Combined Strong and Weak Lensing Analysis of the CLASH Sample: Mass and Magnification Models and Systematic Uncertainties. ApJ, 801(44).
• Canameras, R., Nesvadba, N., Dole, H., McKenzie, T., Koenig, S., Petitpas, G., Frye, B., Guery, D., Flores-Cacho, I., Montier, L., Negrello, M., Beelen, A., Boone, F., Dicken, D., Lagache, G., Le~Floc'h, E., Altieri, B., Chary, R., Bethermin, M., , Giard, M., et al. (2014). Planck's Dusty GEMS: The brightest gravitationally lensed galaxies discovered with the Planck all-sky survey. A&A.
• Dole, H., Gu\'ery, D., Montier, L., Nesvadba, N., Flores-Cacho, I., Altieri, B., Aghanim, N., Beelen, A., B\'ethermin, M., Bonavera, L., Canameras, R., Chary, R., Dassas, K., De Zotti, G., Douspis, M., Frye, B., Giard, M., Gonzalez-Nuevo, J., Hurier, G., , Kneissl, R., et al. (2014). High-redshift infrared galaxy overdensity candidates and lensed sources by Planck and confirmed by Herschel-SPIRE. A&A.
• Huang, X., Zheng, W., Wang, J., Ford, H., Lemze, D., Moustakas, J., Shu, X., Wel, A., Zitrin, A., Frye, B. L., Postman, M., Bartelmann, M., Benitez, N., Bradley, L., Broadhurst, T., Coe, D., Donahue, M., Infante, L., Kelson, D., , Koekemoer, A., et al. (2014). CLASH: Extreme Emission Line Galaxies and Their Implication on Selection of High-Redshift Galaxies. ApJ.
• Malhotra, S., Rhoads, J., Finkelstein, K., Carilli, C., Comes, F., Finkelstein, S., Frye, B., Gerin, M., Guillard, P., Nesvadba, N., Rigby, J., Spaans, M., & Strauss, M. (2014). Herschel Extreme Lensing Line Observations: [CII] variation in galaxies at redshifts $z$ = 1-3. ApJ.
• Rhoads, J. E., Malhotra, S., Allam, S., Carilli, C., Combes, F., Finkelstein, K., Finkelstein, S., Frye, B., Gerin, M., Guillard, P., Nesvadba, N., Rigby, J., Spaans, M., & Strauss, M. A. (2014). Herschel Extreme Lensing Line Observations: Dynamics of Two Strongly Lensed Star-forming Galaxies near Redshift z = 2. ApJ, 787, 8.
• Frye, B. L., Hurley, M., Bowen, D. V., Meurer, G., Sharon, K., Straughn, A., Coe, D., Broadhurst, T., & Guhathakurta, P. (2012). Spatially resolved HST grism spectroscopy of a lensed emission line galaxy at z ∼ 1. Astrophysical Journal, 754(1).
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  Abstract: We take advantage of gravitational lensing amplification by A1689 (z = 0.187) to undertake the first space-based census of emission line galaxies (ELGs) in the field of a massive lensing cluster. Forty-three ELGs are identified to a flux of i 775 = 27.3 via slitless grism spectroscopy. One ELG (at z = 0.7895) is very bright owing to lensing magnification by a factor of ≈4.5. Several Balmer emission lines (ELs) detected from ground-based follow-up spectroscopy signal the onset of a major starburst for this low-mass galaxy (M * ≈ 2 × 10 9 M ⊙) with a high specific star formation rate (≈20Gyr -1). From the blue ELs we measure a gas-phase oxygen abundance consistent with solar (12+log(O/H) = 8.8 ± 0.2). We break the continuous line-emitting region of this giant arc into seven ∼1kpc bins (intrinsic size) and measure a variety of metallicity-dependent line ratios. A weak trend of increasing metal fraction is seen toward the dynamical center of the galaxy. Interestingly, the metal line ratios in a region offset from the center by ∼1kpc have a placement on the blue H II region excitation diagram with f ([O III])/f(Hβ) and f ([Ne III])/f(Hβ) that can be fitted by an active galactic nucleus (AGN). This asymmetrical AGN-like behavior is interpreted as a product of shocks in the direction of the galaxy's extended tail, possibly instigated by a recent galaxy interaction. © 2012. The American Astronomical Society. All rights reserved.
• Merten, J., Coe, D., Dupke, R., Massey, R., Zitrin, A., Cypriano, E. S., Okabe, N., Frye, B., Braglia, F. G., Jiménez-Teja, Y., Benítez, N., Broadhurst, T., Rhodes, J., Meneghetti, M., Moustakas, L. A., Sodré Jr, L., Krick, J., & Bregman, J. N. (2011). Creation of cosmic structure in the complex galaxy cluster merger Abell 2744. Monthly Notices of the Royal Astronomical Society, 417(1), 333-347.
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  Abstract: We present a detailed strong-lensing, weak-lensing and X-ray analysis of Abell 2744 (z= 0.308), one of the most actively merging galaxy clusters known. It appears to have unleashed 'dark', 'ghost', 'bullet' and 'stripped' substructures, each ∼1014M⊙. The phenomenology is complex and will present a challenge for numerical simulations to reproduce. With new, multiband Hubble Space Telescope (HST) imaging, we identify 34 strongly lensed images of 11 galaxies around the massive Southern 'core'. Combining this with weak-lensing data from HST, VLT and Subaru, we produce the most detailed mass map of this cluster to date. We also perform an independent analysis of archival Chandra X-ray imaging. Our analyses support a recent claim that the Southern core and Northwestern substructure are post-merger and exhibit morphology similar to the Bullet Cluster viewed from an angle. From the separation between X-ray emitting gas and lensing mass in the Southern core, we derive a new and independent constraint on the self-interaction cross-section of dark matter particles σ/m < 3 ± 1cm2g-1. In the Northwestern substructure, the gas, dark matter and galaxy components have become separated by much larger distances. Most curiously, the 'ghost' clump (primarily gas) leads the 'dark' clump (primarily dark matter) by more than 150kpc. We propose an enhanced 'ram-pressure slingshot' scenario which may have yielded this reversal of components with such a large separation, but needs further confirmation by follow-up observations and numerical simulations. A secondary merger involves a second 'bullet' clump in the North and an extremely 'stripped' clump to the West. The latter appears to exhibit the largest separation between dark matter and X-ray emitting baryons detected to date in our sky. © 2011 Universität Heidelberg Monthly Notices of the Royal Astronomical Society © 2011 RAS.
• Matsuda, Y., Richard, J., Smail, I., Kashikawa, N., Shimasaku, K., Frye, B. L., Yamada, T., Nakamura, Y., Hayasnino, T., & Fujii, T. (2010). A search for galaxies in and around an HI overdense region at z = 5. Monthly Notices of the Royal Astronomical Society: Letters, 403(1), L54-L58.
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  Abstract: We present the discovery of a large-scale structure of emission-line galaxies at redshift z = 4.86 behind a massive cluster of galaxies, A1689. Previous spectroscopic observations of a galaxy, A1689-7.1 at z = 4.87, near this structure, revealed a possible overdense region of intergalactic medium (IGM) around the galaxy, which extends at least ~80 comoving Mpc along the line of sight. In order to investigate whether this z ~ 5 IGM overdense region contains a galaxy overdensity, we undertook narrow- and broad-band imaging observations around A1689-7.1 with Subaru/Suprime-Cam. We detected 51 candidates as Lyα emitters at redshift z = 4.86 ± 0.03 in the 32 × 24 arcmin2 field of view. After correction for lensing by the foreground cluster, we found a large-scale (~20 × 60 comoving Mpc) overdense region of galaxies around A1689-7.1 in the source plane at z = 4.86. The densest peak in this region has an overdensity of δ ~ 4, suggesting that this structure is probably a good candidate for a protocluster which may evolve into a massive cluster of galaxies in the present-day Universe. A1689-7.1 is located at the edge of this region, where the local galaxy density is ~1.6 times the mean density and is close to the density contrast in the IGM along the line of sight to A1689-7.1 estimated from the optical depth. The overdensities of galaxies we have found may suggest that at least some parts of the IGM overdense region have already started to form galaxies and moreover they relate to the formation of a protocluster. Although we lack information on the three-dimensional distributions of both IGM and galaxy overdense regions, the similarity of the scales of both regions may suggest that the two are parts of a single large-scale structure, which would be an large edge-on sheet along the line of sight with a size of ~20 × 60 × 80 comoving Mpc. © 2010 The Authors. Journal compilation © 2010 RAS.
• Zheng, W., Bradley, L. D., Bouwens, R. J., Ford, H. C., Illingworth, G. D., Benítez, N., Broadhurst, T., Frye, B., Infante, L., Jee, M. J., Motta, V., Shu, X. W., & Zitrin, A. (2009). Bright strongly lensed galaxies at redshift z 6-7 behind the clusters abell 1703 and CL0024+16. Astrophysical Journal Letters, 697(2), 1907-1917.
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  Abstract: We report on the discovery of three bright, strongly lensed objects behind Abell 1703 and CL0024+16 from a dropout search over 25 arcmin2 of deep NICMOS data, with deep ACS optical coverage. They are undetected in the deep ACS images below 8500 and have clear detections in the J and H bands. Fits to the ACS, NICMOS, and IRAC data yield robust photometric redshifts in the range z 6-7 and largely rule out the possibility that they are low-redshift interlopers. All three objects are extended, and resolved into a pair of bright knots. The bright i-band dropout in Abell 1703 has an H-band AB magnitude of 23.9, which makes it one of the brightest known galaxy candidates at z > 5.5. Our model fits suggest a young, massive galaxy only 60 million years old with a mass of 1010 M ⊙. The dropout galaxy candidates behind CL0024+16 are separated by 25 (2 kpc in the source plane), and have H-band AB magnitudes of 25.0 and 25.6. Lensing models of CL0024+16 suggest that the objects have comparable intrinsic magnitudes of AB 27.3, approximately one magnitude fainter than L* at z 6.5. Their similar redshifts, spectral energy distribution, and luminosities, coupled with their very close proximity on the sky, suggest that they are spatially associated, and plausibly are physically bound. Combining this sample with two previously reported, similarly magnified galaxy candidates at z 6-8, we find that complex systems with dual nuclei may be a common feature of high-redshift galaxies. © 2009. The American Astronomical Society. All rights reserved..
• Bradley, L. D., Bouwens, R. J., Ford, H. C., Illingworth, G. D., Jee, M. J., Benítez, N., Broadhurst, T. J., Franx, M., Frye, B. L., Infante, L., Motta, V., Rosati, P., White, R. L., & Zheng, W. (2008). Discovery of a very bright strongly lensed galaxy candidate at z ≈ 7.6. Astrophysical Journal, 678(2), 647-654.
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  Abstract: Using Hubble Space Telescope (HST) and Spitzer IRAC imaging, we report the discovery of a very bright strongly lensed Lyman break galaxy (LBG) candidate atz ∼ 7.6 in the field of the massive galaxy cluster Abell 1689 (z = 0.18). The galaxy candidate, which we refer to as A1689-zD1, shows a strong z 850 - J110 break of at least 2.2 mag and is completely undetected ( 7.0 galaxy candidate found to date. © 2008. The American Astronomical Society. All rights reserved.
• Coe, D., Fuselier, E., Benítez, N., Broadhurst, T., Frye, B., & Ford, H. (2008). Lensperfect: Gravitational lens mass map reconstructions yielding exact reproduction of all multiple images. Astrophysical Journal, 681(2), 814-830.
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  Abstract: We present a new approach to gravitational lens mass map reconstruction. Our mass map solutions perfectly reproduce the positions, fluxes, and shears of all multiple images, and each mass map accurately recovers the underlying mass distribution to a resolution limited by the number of multiple images detected. We demonstrate our technique given a mock galaxy cluster similar to Abell 1689, which gravitationally lenses 19 mock background galaxies to produce 93 multiple images. We also explore cases in which as few as four multiple images are observed. Mass map solutions are never unique, and our method makes it possible to explore an extremely flexible range of physical (and unphysical) solutions, all of which perfectly reproduce the data given. Each reconfiguration of the source galaxies produces a new mass map solution. An optimization routine is provided to find those source positions (and redshifts, within uncertainties) that produce the "most physical" mass map solution, according to a new figure of merit developed here. Our method imposes no assumptions about the slope of the radial profile or mass following light. However, unlike "nonparametric" grid-based methods, the number of free parameters that we solve for is only as many as the number of observable constraints (or slightly greater if fluxes are constrained). For each set of source positions and redshifts, mass map solutions are obtained "instantly" via direct matrix inversion by smoothly interpolating the deflection field using a recently developed mathematical technique. Our LensPerfect software is straightforward and easy to use, and is publicly available on our Web site. © 2008. The American Astronomical Society. All rights reserved.
• Frye, B. L., Bowen, D. V., Hurley, M., Tripp, T. M., Fan, X., Holden, B., Guhathakurta, P., Coe, D., Broadhurst, T., Egami, E., & Meylan, G. (2008). Observations of the gas reservoir around a star-forming galaxy in the early universe. Astrophysical Journal, 685(1 PART 2), L5-L8.
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  Abstract: We present a high signal-to-noise spectrum of a bright galaxy at z=4.9 in 14 hr of integration on VLT FORS2. This galaxy is extremely bright, i 850 p 23.10 ± 0.01, and is strongly lensed by the foreground massive galaxy cluster A1689 (z=0.18). Stellar continuum is seen longward of the Lyα emission line at-7100 å, while intergalactic H i produces strong absorption shortward of Lyα. Two transmission spikes at-6800 and-7040 å are also visible, along with other structures at shorter wavelengths. Although this star-forming is galaxy fainter than a QSO, the absence of a strong central ultraviolet flux source in it enables a measurement of the H i flux transmission in the intergalactic medium (IGM) in the vicinity of a high-redshift object. We find that the effective H i optical depth of the IGM is remarkably high within a large 14 Mpc (physical) region surrounding the galaxy compared to that seen toward QSOs at similar redshifts. Evidently, this high-redshift galaxy is located in a region of space where the amount of H i is much larger than that seen at similar epochs in the diffuse IGM. We argue that observations of high-redshift galaxies like this one provide unique insights into the nascent stages of baryonic large-scale structures that evolve into the filamentary cosmic web of galaxies and clusters of galaxies observed in the current universe. © 2008. The American Astronomical Society.
• Kowalski, M., Rubin, D., Aldering, G., Agostinho, R. J., Amadon, A., Amanullah, R., Balland, C., Barbary, K., Blanc, G., Challis, P. J., Conley, A., Connolly, N. V., Covarrubias, R., Dawson, K. S., Deustua, S. E., Ellis, R., Fabbro, S., Fadeyev, V., Fan, X., , Farris, B., et al. (2008). Improved cosmological constraints from new, old, and combined supernova data sets. Astrophysical Journal, 686(2), 749-778.
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  Abstract: We present a new compilation of Type Ia supernovae (SNe Ia), a new data set of low-redshift nearby-Hubble-flow SNe, and new analysis procedures to work with these heterogeneous compilations. This "Union" compilation of 414 SNe Ia, which reduces to 307 SNe after selection cuts, includes the recent large samples of SNe Ia from the Supernova Legacy Survey and ESSENCE Survey, the older data sets, as well as the recently extended data set of distant supernovae observed with the Hubble Space Telescope (HST). A single, consistent, and blind analysis procedure is used for all the various SN Ia subsamples, and a new procedure is implemented that consistently weights the heterogeneous data sets and rejects outliers. We present the latest results from this Union compilation and discuss the cosmological constraints from this new compilation and its combination with other cosmological measurements (CMB and BAO). The constraint we obtain from supernovae on the dark energy density isΩΛ = 0.713-0.029+0.027(stat) -0.039+0.036(sys), for a flat, ACDM universe. Assuming a constant equation of state parameter, w, the combined constraints from SNe, BAO, and CMB give w = -0.969-0.063+0.059(stat) -0.066+0.063(sys). While our results are consistent with a cosmological constant, we obtain only relatively weak constraints on a w that varies with redshift. In particular, the current SN data do not yet significantly constrain w at z > 1. With the addition of our new nearby Hubble-flow SNe Ia, these resulting cosmological constraints are currently the tightest available. © 2008. The American Astronomical Society. All rights reserved.
• Frye, B. L., Coe, D., Bowen, D. V., Benítez, N., Broadhurst, T., Guhathakurta, P., Illingworth, G., Menanteau, F., Sharon, K., Lupton, R., Meylan, G., Zekser, K., Meurer, G., & Hurley, M. (2007). The sextet arcs: A strongly lensed lyman break galaxy in the acs spectroscopic galaxy survey toward abell 1689. Astrophysical Journal, 665(2 I), 921-935.
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  Abstract: We present results of the HST Advanced Camera for Surveys spectroscopic ground-based redshift survey in the field of A1689. We measure 98 redshifts, increasing the number of spectroscopically confirmed objects sixfold. We present two spectra from this catalog of the Sextet Arcs, images that arise from a strongly lensed Lyman break galaxy (LBG) at a redshift of z = 3.038. Gravitational lensing by the cluster magnifies its flux by a factor of ∼ 16 and produces six separate images with a total r-band magnitude of r 625 = 21.7. The two spectra, each of which represents emission from different regions of the LBG, show H I and interstellar metal absorption lines at the systemic redshift. Significant variations are seen in the Lyα profile across a single galaxy, ranging from strong absorption to a combination of emission plus absorption. A spectrum of a third image close to the brightest arc shows Lyα emission at the same redshift as the LBG, arising from either another spatially distinct region of the galaxy or from a companion galaxy close to the LBG. Taken as a group, the Lyα equivalent width in these three spectra decreases with increasing equivalent width of the strongest interstellar absorption lines. We discuss how these variations can be used to understand the physical conditions in the LBG. Intrinsically, this LBG is faint, ∼0. 1L*, and is forming stars at a modest rate, ∼4 M ⊙ yr-1. We also detect absorption-line systems toward the Sextet Arcs at z = 2.873 and z = 2.534. The latter system is seen across two of our spectra. © 2007. The American Astronomical Society. All rights reserved.
• Aracil, B., Tripp, T. M., Bowen, D. V., Prochaska, J. X., Chen, H., & Frye, B. L. (2006). Erratum: High-metallicity, photoionized gas in intergalactic large-scale filaments (Monthly Notices of the Royal Astronomical Society (2006) 367 (139-155) DOI: 10.1111/j.1365-2966.2005.09962.x). Monthly Notices of the Royal Astronomical Society, 372(2), 959-960.
• Aracil, B., Tripp, T. M., Bowen, D. V., Prochaska, J. X., Chen, H., & Frye, B. L. (2006). High-metallicity, photoionized gas in intergalactic large-scale filaments. Monthly Notices of the Royal Astronomical Society, 367(1), 139-155.
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  Abstract: ABSTRACT We present high-resolution ultraviolet spectra of absorption-line systems towards the low-z quasi-stellar object (QSO) HS 0624+6907 (z QSO= 0.3700). Coupled with ground-based imaging and spectroscopic galaxy redshifts, we find evidence that many of these absorbers do not arise in galaxy haloes but rather are truly intergalactic gas clouds distributed within large-scale structures, and moreover, the gas is cool (T < 10 5 K) and has relatively high metallicity (Z > 0.9 Z ⊙). Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS) data reveal a dramatic cluster of 13 H i Lyman α (Lyα) lines within a 1000 km s -1 interval at z abs= 0.0635. We find 10 galaxies at this redshift with impact parameters ranging from ρ= 135 h -170 kpc to 1.37 h -170 Mpc. The velocities and velocity spread of the Lyα lines in this complex are unlikely to arise in the individual haloes of the nearby galaxies; instead, we attribute the absorption to intragroup medium gas, possibly from a large-scale filament viewed along its long axis. Contrary to theoretical expectations, this gas is not the shock-heated warm-hot intergalactic medium (WHIM); the width of the Lyα lines all indicate a gas temperature T≪ 10 5 K, and metal lines detected in the Lyα complex also favour photoionized, cool gas. No O vi absorption lines are evident, which is consistent with photoionization models. Remarkably, the metallicity is near-solar, [M/H]=-0.05 ± 0.4 (2σ uncertainty), yet the nearest galaxy which might pollute the intergalactic medium is at least 135 h -170 kpc away. Tidal stripping from nearby galaxies appears to be the most likely origin of this highly enriched, cool gas. More than six Abell galaxy clusters are found within 4°of the sight line suggesting that the QSO line of sight passes near a node in the cosmic web. At z≈ 0.077, we find absorption systems as well as galaxies at the redshift of the nearby clusters Abell 564 and Abell 559. We conclude that the sight line pierces a filament of gas and galaxies feeding into these clusters. The absorber at z abs= 0.075 73 associated with Abell 564/559 also has a high metallicity with [C/H] > -0.6, but again the closest galaxy is relatively far from the sight line (ρ= 293 h -170 kpc). The Doppler parameters and H i column densities of the Lyα lines observed along the entire sight line are consistent with those measured towards other low-z QSOs, including a number of broad (b > 40 km s -1) Lyα lines. © 2006 RAS.
• Garavini, G., Aldering, G., Amadon, A., Amanullah, R., Astier, P., Ballanc, G., Blanc, G., Conley, A., Dahlén, T., Deustua, S. E., Ellis, R., Fabbro, S., Fadeyev, V., Fan, X., Folatelli, G., Frye, B., Gates, E. L., Gibbons, R., Goldhaber, G., , Goldman, B., et al. (2005). Spectroscopic observations and analysis of the unusual Type Ia SN 1999ac. Astronomical Journal, 130(5), 2278-2292.
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  Abstract: We present optical spectra of the peculiar Type la supernova (SN Ia) 1999ac. The data extend from -15 to +42 days with respect to B-band maximum and reveal an event that is unusual in several respects. Prior to B-band maximum, the spectra resemble those of SN 1999aa, a slowly declining event, but possess stronger Si II and Ca II signatures (more characteristic of a spectroscopically normal SN). Spectra after the B-band maximum appear more normal. The expansion velocities inferred from the iron lines appear to be lower than average, whereas the expansion velocity inferred from calcium H and K are higher than average. The expansion velocities inferred from Si II are among the slowest ever observed, although SN 1999ac is not particularly dim. The analysis of the parameters v 10(Si II), R(Si II), v̇, and Δm 15 further underlines the unique characteristics of SN 1999ac. We find convincing evidence of C II λ6580 in the day - 15 spectrum with ejection velocity v > 16,000 km s -1, but this signature disappears by day - 9. This rapid evolution at early times highlights the importance of extremely early-time spectroscopy. © 2005. The American Astronomical Society. All rights reserved.
• Menanteau, F., Martel, A. R., Tozzi, P., Frye, B., Ford, H. C., Infante, L., Benítez, N., Galaz, G., Coe, D., Illingworth, G. D., Hartig, G. F., & Clampin, M. (2005). The nature of blue cores in spheroids: A possible connection with active galactic nuclei and star formation. Astrophysical Journal Letters, 620(2 I), 697-702.
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  Abstract: We investigate the physical nature of blue cores in early-type galaxies through the first multiwavelength analysis of a serendipitously discovered field blue-nucleated spheroid in the background of the deep Hubble Space Telescope ACS/WFC griz multicolor observations of the cluster A1689. The resolved g-r, r-i, and i-z color maps reveal a prominent blue core identifying this galaxy as a "typical" case study, exhibiting variations of 0.5-1.0 mag in color between the center and the outer regions, opposite to the expectations of reddened metallicity-induced gradients in passively evolved elliptical galaxies. From a Magellan-Clay telescope spectrum we secure the galaxy redshift at z = 0.624. We find a strong X-ray source coincident with the spheroid galaxy. Spectral features and a high X-ray luminosity indicate the presence of an active galactic nucleus (AGN) in the galaxy. However, a comparison of the X-ray luminosity to a sample derived from the Chandra Deep Field-South displays L X to be comparable to type 1/QSO galaxies while the optical flux is consistent with a normal star-forming galaxy. We conclude that the galaxy's nonthermal component dominates at high-energy wavelengths, while we associate the spheroid blue light with the stellar spectrum of normal star-forming galaxies. We argue for a probable association between the presence of blue cores in spheroids and AGN activity. © 2005. The American Astronomical Society. All rights reserved.
• Garavini, G., Folatelli, G., Goobar, A., Nobili, S., Aldering, G., Amadon, A., Amanullah, R., Astier, P., Balland, C., Blanc, G., Burns, M. S., Conley, A., Dahlén, T., Deustua, S. E., Ellis, R., Fabbro, S., Fan, X., Frye, B., Gates, E. L., , Gibbons, R., et al. (2004). Spectroscopic observations and analysis of the peculiar SN 1999aa. Astronomical Journal, 128(1 1783), 387-404.
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  Abstract: We present an extensive new time series of spectroscopic data of the peculiar SN 1999aa in NGC 2595. Our data set includes 25 optical spectra between -11 and +58 days with respect to B-band maximum light, providing an unusually complete time history. The early spectra resemble those of an SN 1991T-like object but with a relatively strong Ca H and K absorption feature. The first clear sign of Si II λ6355, characteristic of Type Ia supernovae, is found at day -7, and its velocity remains constant up to at least the first month after B-band maximum light. The transition to normal-looking spectra is found to occur earlier than in SN 1991T, suggesting SN 1999aa as a possible link between SN 1991T-like and Branch-normal supernovae. Comparing the observations with synthetic spectra, doubly ionized Fe, Si, and Ni are identified at early epochs. These are characteristic of SN 1991T-like objects. Furthermore, in the day -11 spectrum, evidence is found for an absorption feature that could be identified as high velocity C II λ6580 or Hα. At the same epoch C II λ4648.8 at photospheric velocity is probably responsible for the absorption feature at 4500 Å. High-velocity Ca is found around maximum light together with Si II and Fe II confined in a narrow velocity window. Implied constraints on supernovae progenitor systems and explosion hydrodynamic models are briefly discussed.
• Hall, P. B., Hoversten, E. A., Tremonti, C. A., E., D., Schneider, D. P., Strauss, M. A., Knapp, G. R., York, D. G., Hutemékers, D., Newman, P. R., Brinkmann, J., Frye, B., Fukugita, M., Glazebrook, K., Harvanek, M., Heckman, T. M., Ivezić, Ž., Kleinman, S., Krzesinski, J., , Long, D. C., et al. (2004). A Lyα-only active galactic nucleus from the Sloan Digital Sky Survey. Astronomical Journal, 127(6 1782), 3146-3154.
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  Abstract: The Sloan Digital Sky Survey has discovered a z = 2.4917 radio-loud active galactic nucleus (AGN) with a luminous, variable, low-polarization UV continuum, H I two-photon emission, and a moderately broad Lyα line (FWHM ≃ 1430 km s-1) but without obvious metal-line emission. SDSS J113658.36+024220.1 does have associated metal-line absorption in three distinct, narrow systems spanning a velocity range of 2710 km s-1. Despite certain spectral similarities, SDSS J1136+0242 is not a Lyman break galaxy. Instead, the Lyα and two-photon emission can be attributed to an extended, low-metallicity narrow-line region. The unpolarized continuum argues that we see SDSS 11136+0242 very close to the axis of any ionization cone present. We can conceive of two plausible explanations for why we see a strong UV continuum but no broad-line emission in this "face-on radio galaxy" model for SDSS J1136+0242: the continuum could be relativistically beamed synchrotron emission that swamps the broad-line emission, or more likely, SDSS J1136+0242 could be similar to PG1407+265, a quasar in which for some unknown reason the high-ionization emission lines are very broad, very weak, and highly blueshifted.
• Winn, J. N., Suto, Y., Turner, E. L., Narita, N., Frye, B. L., Aoki, W., Sato, B., & Yamada, T. (2004). A search for Hα absorption in the exosphere of the transiting extrasolar planet HD 209458b. Publications of the Astronomical Society of Japan, 56(4), 655-662.
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  Abstract: There is evidence that the transiting planet HD 209458h has a large exosphere of neutral hydrogen, based on a 15% decrement in Lyman-α flux that was observed by Vidal-Madjar et al. during transits. Here we report upper limits on Hα absorption by the exosphere. The results are based on optical spectra of the parent star obtained with the Subaru High Dispersion Spectrograph. Comparison of the spectra taken inside and outside of transit reveals no exospheric Hα signal greater than 0.1% within a 5.1 Å band (chosen to have the same Δλ/λ as the 15% Lyα absorption). The corresponding limit on the column density of n = 2 neutral hydrogen is N2 ≲ 109cm-2. This limit constrains proposed models involving a hot (∼ 104K) and hydrodynamically escaping exosphere.
• Frye, B., Broadhurst, T., & Benítez, N. (2002). Spectral evidence for widespread galaxy outflows at z > 4. Astrophysical Journal Letters, 568(2 I), 558-575.
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  Abstract: We present discovery spectra of a sample of eight lensed galaxies at high redshift, 3.7 < z < 5.2, selected by their red colors in the fields of four massive clusters: A1689, A2219, A2390, and AC 114. Metal absorption lines are detected and observed to be blueshifted by 300-800 km s-1 with respect to the centroid of Lyα emission. A correlation is found between this blueshift and the equivalent width of the metal lines, which we interpret as a broadening of saturated absorption lines caused by a dispersion in the outflow velocity of interstellar gas. Local starburst galaxies show similar behavior, associated with obvious gas outflows. We also find a trend of increasing equivalent width of Lyα emission with redshift, which may be a genuine evolutionary effect toward younger stellar populations at high redshift with less developed stellar continua. No obvious emission is detected below the Lyman limit in any of our spectra or in deep U- or B-band images. The UV continua are reproduced well by early B stars, although some dust absorption would allow a fit to hotter stars. If B stars dominate, then their relatively prominent stellar absorption lines should separate in wavelength from those of the outflowing gas, requiring more detailed spectroscopy. After correcting for the lensing, we derive small physical sizes for our objects, ∼0.5-5 kpc h-1 for a flat cosmology with Ωm = 0.3, Ω Λ = 0.7. The lensed images are only marginally resolved in good seeing despite their close proximity to the critical curve, where large arcs are visible and hence high magnifications of up to ∼20 times are inferred. Two objects show a clear spatial extension of the Lyα emission relative to the continuum starlight, indicating a "breakout" of the gas. The sizes of our galaxies together with their large gas motion suggests that outflows of gas are common at high redshift and associated with galaxy formation.
• Smith, G. P., Treu, T., Ellis, R., Smail, I., Kneib, J. -., & Frye, B. L. (2001). Near-infrared spectroscopy and Hubble Space Telescope imaging of a dusty starburst extremely red object. Astrophysical Journal Letters, 562(2 PART II), 635-640.
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  Abstract: We present near-infrared spectroscopy and Hubble Space Telescope (HST) imaging of ERO J164023+ 4644, an Extremely Red Object (ERO) with (R - K) = 5.9 at z = 1.05 that has been detected by Infrared Space Observatory (ISO) at 15 μm. ERO J164023 resembles a disk galaxy, with an optical/infrared spectral energy distribution that is strongly reddened by dust (LFIR/LB ≲ 200; AV ∼ 5). The combination of the narrow width of the emission lines in our spectra (∼ 300 km s-1) and the relatively high [N II]/Hα line ratio indicate that this is a "composite" starburst-Seyfert galaxy. Assuming that star formation dominates the energy output, we constrain the star formation rate to lie in the broad range ∼ 10-700 M⊙ yr-1 from a variety of star formation indicators. We compare ERO J164023 with the only other spectroscopically identified dusty EROs: HR10 (z = 1.44) and ISO J1324-2016 (z = 1.50). ERO J164023 and HR10 have similar disklike morphologies in the rest-frame UV, and both exhibit a variation in the apparent dust obscuration depending upon the diagnostic used, which suggests that there is a complex spatial mix of stellar populations and dust in these galaxies. In contrast, the compact morphology and spectral properties of ISO J1324-2016 indicate that it is a dusty quasar. Overall, our results demonstrate that the population of dusty galaxies identified using photometric ERO criteria includes systems ranging from pure starbursts through transition systems, such as ERO J164023, to dusty quasars. We suggest that the classification of EROs into these subclasses, necessary for the detailed modeling of the population, cannot be reliably achieved from optical/near-infrared photometry and instead requires mid/far-infrared or submillimeter photometry and near-infrared spectroscopy. The advent of efficient multiobject spectrographs working in the near-infrared, as well as the imminent launch of SIRTF, therefore promises the opportunity of rapid progress in our understanding of the elusive ERO population. © 2001. The american astronomical society. All rights reserved.
• Swift, J. J., Welch, W. J., & Frye, B. L. (2001). Spatially resolved millimeter spectroscopy of the gravitational lens PKS 1830-211. Astrophysical Journal Letters, 549(1 PART 2), L29-L32.
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  Abstract: This paper presents data from the BIMA interferometer showing spatially resolved absorption spectra of the gravitationally lensed quasar PKS 1830-211. High-resolution (1.2 km s-1) spectra were taken in two spectral windows centered on the redshifted frequencies of the HCO+(2 ← 1) and HCN(2 ← 1) molecular transitions. There is no molecular absorption in the northeast image, but the southwest image reveals optically thick absorbing gas at these transition frequencies. Further analyses conclude that the spectra are consistent with completely saturated absorption in the southwest image, and the line profiles suggest that the absorbing medium is complex, perhaps containing multiple components and small-scale structure. The absorption occurs along a pencil beam through the lensing galaxy which is thought to be a late-type spiral oriented almost face-on. However, the spectra show absorption spanning more than 60 km s-1, which is difficult to explain for this scenario.
• Broadhurst, T., Huang, X., Frye, B., & Ellis, R. (2000). A spectroscopic redshift for the CL 0024+16 multiple arc system: Implications for the central mass distribution. Astrophysical Journal Letters, 534(1 PART 2), L15-L18.
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  Abstract: We present a spectroscopic redshift of z = 1.675 for the well-known multiply lensed system of arcs seen in the z = 0.39 cluster Cl 0024+16. In contrast to earlier work, we find that the lensed images are accurately reproduced by a projected mass distribution which traces the locations of the brightest cluster elliptical galaxies, suggesting that the most significant minima of the cluster potential are not dynamically erased. The averaged mass profile is shallow and consistent with predictions of recent numerical simulations. The source redshift enables us to determine an enclosed cluster mass of M(
• Lidman, C., Courbin, F., Meylan, G., Broadhurst, T., Frye, B., & Welch, W. J. (1999). The redshift of the gravitationally lensed radio source PKS 1830-211. Astrophysical Journal Letters, 514(2 PART 2), L57-L60.
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  Abstract: We report on the spectroscopic identification and the long-awaited redshift measurement of the heavily obscured, gravitationally lensed radio source PKS 1830-211, which was first observed as a radio Einstein ring. The northeast component of the doubly imaged core is identified, in our infrared spectrum covering the wavelength range 1.5-2.5 μm, as an impressively reddened quasar at z = 2.507 ± 0.002. The mass contained within the Einstein ring radius is M(r < 2.1 h-1 kpc) = 6.3 × 1010 h-1 M⊙ for ΩM = 1 or M(r < 2.4 h-1 kpc) = 7.4 × 1010 h-1 M⊙ for ΩM = 0.3. Our redshift measurement, together with the recently measured time delay (Lovell et al.), means that we are a step closer to determining H0 from this lens. Converting the time delay into H0 by using existing models leads to high values of the Hubble parameter, H0 = 65+15-9 for ΩM = 1 and H0 = 7618-10, for ΩM = 0.3. Since the lensing galaxy lies very close to the center of the lensed ring, improving the error bars on H0 will require not only a more precise time delay measurement but also very precise astrometry of the whole system.
• Courbin, F., Lidman, C., Frye, B. L., Magain, P., Broadhurst, T. J., Pahre, M. A., & Djorgovski, S. G. (1998). Image deconvolution of the radio ring pks 1830-211. Astrophysical Journal Letters, 499(2 PART II), L119-L123.
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  Abstract: New high-quality Keck and ESO images of PKS 1830-211 are presented. By applying a powerful new deconvolution algorithm to these optical and infrared data, both images of the flat spectrum core of the radio source have been identified. An extended source is also detected in the optical images which is consistent with the expected location of the lensing galaxy. The source counterparts are very red at I - K ∼ 7, which suggests strong Galactic absorption with additional absorption by the lensing galaxy at z = 0.885 and is consistent with the detection of high-redshift molecules in the lens. © 1998. The American Astronomical Society. All rights reserved.
• Frye, B., & Broadhurst, T. (1998). Discovery of red-selected arcs at z = 4.04 behind abell 2390. Astrophysical Journal Letters, 499(2 PART II), L115-L118.
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  Abstract: We describe the properties of three red arcs discovered at z = 4.04 behind the cluster A2390 (z = 0.23). We demonstrate that these arcs are images of a single galaxy where lensing is compounded by an elliptical cluster member near the critical curve of the cluster. The combined magnification is estimated to be ∼20 using Hubble Space Telescope images, depending on the gradient of the model potentials, implying an unlensed magnitude for the source of IAB = 25.5. Keck spectroscopy reveals a continuum that is well fitted by B stars and attenuated by the Lyman series forest with an opacity consistent with z ∼ 4 QSO spectra, making the arcs relatively red. Damped Lyα absorption is observed at the source redshift corresponding to a high column density NHI = 3 × 1021. Lyα emission is found to be spatially separated (∼0.5 kpc) from the bright stellar continuum and lies ∼300 km s-1 redward of interstellar absorption lines at z = 4.04. Similar redward shifts are found in all high-redshift galaxies with good spectroscopy, indicating that outward flows of enriched gas are typical of young galaxies. Finally, we briefly comment on the notorious "straight arc" in A2390, which is resolved into two unrelated galaxies at z = 0.913 and z = 1.033. © 1998. The American Astronomical Society. All rights reserved.
• Frye, B., Welch, W. J., & Broadhurst, T. (1997). Resolving redshifted molecular absorption toward the gravitational lens PKS 1830-211. Astrophysical Journal Letters, 478(1 PART II), L25-L28.
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  Abstract: Using the high-resolution configuration of the BIMA array, we have spatially resolved molecular absorption at z = 0.89 toward the gravitational lens PKS 1830-211. Two continuum sources are detected at λ3 mm separated by 0″.98 at the known positions of the doubly lensed radio core. Broad molecular absorption of width 40 km s-1 is found toward the southwest component only, where surprisingly it does not reach the base of the continuum, despite the large optical depth inferred from the molecular transitions (Wiklind & Combes). This implies incomplete coverage of the southwest component, ∼70%, by the molecular gas, despite the small projected size of the source, less than 8 h-1 pc at the absorption redshift. Similar saturated but unfilled columns of low-density molecular gas are found in absorption through the spiral arms of the Milky Way, with large variations in column depth on parsec scales, indicating that the southwest component of PKS 1830-211 may be occulted by an ordinary spiral arm. At spectral resolution better than 5 km s-1, we might expect the broad molecular absorption of PKS 1830-211 to resolve into multiple narrow lines. © 1997. The American Astronomical Society. All rights reserved.
• Gerin, M., Phillips, T. G., Benford, D. J., Young, K. H., Menten, K. M., & Frye, B. (1997). Redshifted molecular absorption systems toward PKS 1830-211 and B0218+357: Submillimeter CO, C I, and H₂O data. Astrophysical Journal Letters, 488(1 PART II), L31-L34.
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  Abstract: We have detected the J = 4 ← 3 rotational transition of 12CO in absorption at z = 0.89 toward the quasar PKS 1830-211, but not the 12CO (5 ← 4) or the 3/1 ← 3/P0 fine-structure line of neutral carbon. The intervening molecular medium thus has a total 12CO column density of 1018 cm-2 ≤ N(CO) ≤ 5 × 1018 cm-2 with a most likely value of N(CO) ≃ 2 × 10-8 cm-2, which corresponds to the large column density of molecular hydrogen of N(H2) = 2.5 × 1022 cm-2 and a reddening of Aν. = 25 mag. The 12CO excitation temperature is low, below 15 K. Comparison with existing molecular absorption results shows that the absorbing material has molecular abundances similar to Galactic dark clouds. We find an upper limit for atomic carbon of N(C I) ≤ 1018 cm-2, which again would be the case for most Galactic dark clouds. We also report new observations of the absorbing system toward B0218+357 at z = 0.68. We have tentatively detected the 13CO (4 ← 3) line, but for H2O, although a feature is seen at the correct velocity, because of the inadequate signal-to-noise ratio we report only an upper limit for the fundamental line of ortho-water vapor. The tentative detection of the 13CO J = 4 ← 3 line implies that the 13CO excitation temperature is lower than 20 K and the column density is fairly large, 4 × 1016 cm-2 ≤ N (CO13) ≤ 2.2 × 1017 cm-2, with a likely value of N(CO13) ≃ 1017 cm-2, giving rise to saturated absorption in the J = 2 ← 1 transition. The total column density of molecular gas is again large in this source, N(H2) ≥ 2 × 1022 cm-2, which corresponds to a reddening larger than 20 mag. © 1997. The American Astronomical Society. All rights reserved.

Proceedings Publications

• Coe}, D., Salmon, B., Bradac, M., Bradley, L., Sharon, K., Zitrin, A., Acebron, A., Cerny, C., Nathalia, C., Strait, V., Paterno-Mahler, R. .., Mahler, G., Avila, R., Ogaz, S., Huang, K., Pelliccia, D., Stark, D., Mainali, R., Oesch, P., , Trenti, M., et al. (2020, jan). "Results from the HST Treasury Program RELICS: Reionization Lensing Cluster Survey". In American Astronomical Society Meeting Abstracts #235, 235.
• Cooper, O., Lowenthal, J., Yun, M., Kamieneski, P., Frye, B., Harrington, K., Wang, D., & Berman, D. (2020, jan). "Lensing Masses of 8 Planck-selected Gravitationally Lensed Sub-millimeter Galaxies". In American Astronomical Society Meeting Abstracts #235, 235.
• Jansen}, R., Grogin, N., Windhorst, R., Ashcraft, T., Brisken, W., Cohen, S., Conselice, C., Driver, S., Finkelstein, S., Frye, B., Hathi, N., Jones, V., Joshi, B., Kim, D., Koekemoer, A., Maksym, W., Riess, A., Rodney, S., Royle, P., , Ryan, R., et al. (2020, jan). "UV-Visible observations with HST in the JWST North Ecliptic Pole Time-Domain Field". In American Astronomical Society Meeting Abstracts #235, 235.
• Fogarty, K., Postman, M., Donahue, M., Li, Y., Liu, H. B., Dannerbauer, H., Balestra, I., Frye, B., Koekemoer, A., Umetsu, K., & Ziegler, B. (2019, jan). Molecular Gas and Dust in the Brightest Cluster Galaxy of MACS 1931.8-2635. In American Astronomical Society Meeting Abstracts #233, 233.
• Jansen, R. A., Grogin, N., Ashcraft, T., Brisken, W., Cohen, S., Conselice, C., Driver, S., Finkelstein, S., Frye, B., Hathi, N., Jones, V., Joshi, B., Kim, D., Koekemoer, A., Maksym, W., Riess, A., Rodney, S., Royle, P., Ryan, R., , Smith, B., et al. (2019, jan). UV-Visible observations with HST in the JWST North Ecliptic Pole Time-Domain Field. In American Astronomical Society Meeting Abstracts #233, 233.
• Kamieneski, P., Yun, M., Lowenthal, J. D., Harrington, K., Wang, D., & Frye, B. (2019, jan). Multi-wavelength source reconstruction of gravitationally-lensed Planck-selected sub-mm galaxies. In American Astronomical Society Meeting Abstracts #233, 233.
• Pascale, M., Frye, B., Zitrin, A., Diego, J., Coe, D., Cohen, S., Jansen, R. A., & Windhorst, R. (2019, jan). New HST Imaging and Strong Gravitational Lensing Models of Galaxy-overdense Fields Selected by Color Using Planck and Herschel. In American Astronomical Society Meeting Abstracts #233, 233.
• Coe, D., Bradley, L., Salmon, B., Avila, R., Ogaz, S., Bradac, M., Huang, K., Strait, V., Hoag, A., Frye, B. L., & (total of 43 coauthors), e. a. (2018, January). RELICS: Reionization Lensing Cluster Survey - Discovering Brightly Lensed Distant Galaxies for JWST. In AAS, 231.
• Conselice, C., Griffiths, A., Alpaslan, M., Frye, B. L., Zitrin, A., Diego, J., Yan, H., Ma, Z., Barone-Nugent, R., Bhatawdekar, R., Driver, S., Robotham, A., Windhorst, R., & Wyithe, S. (2018, January). The Discovery and Properties of a Newly Discovered Compact Lensing Cluster CLIO at z=0.42: A unique JWST target. In AAS, 231.
• Jansen, R., Windhorst, R., Grogin, N., Koekemoer, A., Royle, P., Hathi, N., Jones, V., Cohen, S., Ashcraft, T., Willmer, C. N., Conselice, C., White, C., & Frye, B. L. (2018, January). UV--Visible observations with HST in the JWST North Ecliptic Pole Time-Domain Field. In AAS, 231.
• Salmon, B., Coe, D., Bradley, L., Bradac, M., Huang, K., Oesch, P., Brammer, G., Stark, D., Sharon, K., Frye, B. L., & (total of 28 authors), e. a. (2018, January). RELICS: A Candidate Galaxy Arc at z~10 and Other Brightly Lensed z>6 Galaxies. In AAS, 231.
• Frye, B. L., Frye, B. L., Rieke, M. J., Rieke, M. J., Willmer, C. N., Willmer, C. N., Egami, E., Egami, E., Ferruit, P., Ferruit, P., Alberts, S., Alberts, S., Bunker, A., Bunker, A., Charlot, S., Charlot, S., Chevallard, J., Chevallard, J., Dressler, A., , Dressler, A., et al. (2017, June). NIRcam-NIRSpec GTO Observations of Galaxy Evolution. In AAS, 230.
• Cai, Z., Fan, X., Bian, F., McGreer, I. D., Frye, B. L., Yang, Y., Zabludoff, A. I., & Zheng, Z. (2014, jan). MApping the Most Massive Overdensity Through Hydrogen (MAMMOTH). In American Astronomical Society Meeting Abstracts, 223, #358.21.

Presentations

• Frye, B. L. (2021, February 18). Planck-Herschel Detection (PHD) of Galaxy Overdensities from z = 3 to the Present. Colloquium, University of Massachusetts at Amherst. This was a virtual colloquium delivered to the audience at UMass Amherst.: IAS Princeton.
• Frye, B. L. (2020, April). New Views of Galaxy Cluster Laboratories. Astronomy Seminar. Waterloo, Canada (Virtual talk): University of Waterloo.
• Frye, B. L. (2020, October). Hubble Views of Overdense Structures and Giant Arcs Discovered Using Planck. Astrophysics Seminar Series. Institute for Advanced Study, Princeton, in PERSON: Institue for Advanced Study.
• Frye, B. L., & Liviatan, O. (2019, February). Opening Outer Space. St. Joseph's Bridges Lecture Series. St. Joseph's campus, Waterloo, Canada: St. Joseph's campus, Waterloo, Canada.
• Frye, B. L., & Liviatan, O. (2020, February). Opening Outer Space. St. Joseph's Bridges Lecture Series. St. Joseph's campus, Waterloo, Canada: St. Joseph's campus, Waterloo, Canada.
• Frye, B. L. (2019, April). Planck's View of Galaxy Clusters. Invited Astrophysics Seminar. University of Urbana-Champaign: University of Urbana-Champaign.
• Frye, B. L., Norman, D., Bauer, A., & Stobie, B. (2018, July/Summer). Gemini Observations from QSOs to Starbursts. Science and Evolution of Gemini Conference. San Francisco, CA: NOAO.
• Frye, B. L., Qin, Y., Pascale, M., & Bauer, A. (2018, November/Fall). A Rare View of Galaxy Cluster Laboratories. Informal Astrophysics Seminar. Institute for Advanced Study (IAS), Princeton, NJ: IAS.
• Frye, B. L. (2016, 10/2016). The Best ‘Optics’ for JWST: the Planck Connection. NOAO FLASH Talk. NOAO, Tucson.
• Frye, B. L. (2016, February/Spring). Rare Views of Submillimeter Galaxies using Planck/Herschel. Invited Talk: Reionization Lensing Cluster Survey (RELICS) Conference. Steward Observatory, University of Arizona: RELICS.
• Frye, B. L. (2016, October, 2016). Exploring the Universe with JWST - II. Invited Conference Talk. Montreal, Canada.
• Frye, B. L. (2015, August). High Redshift Galaxies in the Fields of Massive Lensing Clusters. Seminar at Institute of Astronomy, Cambridge University, England. IoA, Cambridge, England.
• Frye, B. L. (2015, June). Strongly Lensed Star Forming Galaxies from z=1 to 10.8. Institute for Theory and Computation (ITC) Seminar, Harvard University. ITC, Harvard University: Harvard University (Avi Loeb).
• Frye, B. L. (2015, June). The Sightline to PG1543+489: from sub-DLAs to the QSO Host. Cosmology Seminar, Princeton University. Department of Astrophysical Sciences, Princeton University.
• Frye, B. L. (2015, September, 2015). CLASH-N: a Faint Galaxy Survey in the Field of MACSJ0647+7015. Invited Talk: CLASH-VLT. Florence, Italy.
• Frye, B. L. (2014, April 25). Lensed Views of Ordinary and Extraordinary Star Forming Galaxies. Invited Talk. SESE, Arizona State University.
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  I gave a seminar at SESE, and had discussions with most of the faculty and graduate students on topics of mutual interest.
• Frye, B. L. (2014, June 11). The QSO Host of PG1543+489. Invited Talk. Laboratoire d'Astrophysique de Marseille, Marseille, France.
• Frye, B. L. (2014, June 13). The Sightline to PG1543+489: evidence for accreting cool halo gas. Invited talk. Meudon Observatory, France.
• Frye, B. L. (2014, June). Rare Views of Giant Arcs at z=1-5. EWASS 2014: European Week of Astronomy and Space Science Special Session on Cluster Lensing and Distant Sources. Geneva, Switzerland.
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  I gave a talk at the Special Session on Cluster Lensing and Distant Sources, on the invitation of the conference organizer Jean-Paul Kneib.
• Frye, B. L. (2014, October). Faint Galaxy Redshift Galaxies in the Fields of Massive Lensing Clusters. CLASH-VLT: New Frontiers for Galaxy Clusters. INAF - Astronomical Observatory of Capodimonte, Napoli, Italy.

Poster Presentations

• Frye, B. L., Jansen, R., Alpaslan, M., Ashby, M., Ashcraft, T., Cohen, S., Condon, J., Conselice, C., Ferrara, A., Grogin, N., & coauthors, p. 1. (2017, January). The JWST North Ecliptic Pole Survey Field for Time-domain Studies. AASAAS.

Creative Performances

• Frye, B. L. (2021. Discovery of a Galaxy Shipyard. NPR Interview with Tony Perkins. Tucson, AZ.
• Frye, B. L. (2021. The Institute of Useless Knowledge. NPR interview with Davis Duncan for the "Off the Beaten Path" radio series. IAS, Princeton: IAS.
• Frye, B. L. (2021. The Shipyard Galaxy. KVOA News Channel 4 Interview with Angelique Lizarde. Tucson, AZ.

Case Studies

• Foley, R., Koekemoer, A., Spergel, D., Bianco, F., Capak, P., Dai, L., Dore, O., Fazio, G., Ferguson, H., Filippenko, A., Frye, B. L., & (total of 41 authors), e. a. (2018. White Paper: LSST Observing Strategy White Paper: LSST Observations of WFIRST Deep Fields(pp arXiv: 1812.00514).
• Frye, B. L. (2018. WFIRST/LSST Deep Fields Workshop: Breakout Leader on strong lensing and deep fields(pp 30 min talk plus discussion).

Others

• Xu, B., Meneghetti, M., Zitrin, A., Merten, J., Maoz, D., Frye, B. L., Umetsu, K., Zheng, W., Bradley, L., Vega, J., & Koekemoer, A. (2018, January). Properties of giant arcs behind CLASH clusters (Xu+, 2016). VizieR Online Data Catalog.