Marcia J Rieke

Interests

Research

Distant galaxies, exoplanets, infrared light sensors

Courses

Scholarly Contributions

Journals/Publications

• Rieke, M. J., Schlawin, E. A., Misselt, K. A., Leisenring, J. M., Greene, T. P., Kelly, D., McElwain, M., & Beatty, T. (2021). JWST Noise Floor. II. Systematic Error Sources in JWST NIRCam Time Series. Astronomical journal, 161, 18. doi:10.3847/1538-3881/abd8d4
• Rieke, M. J. (2020). Clustering with JWST: Constraining galaxy host halo masses, satellite quenching efficiencies, and merger rates at z = 4-10. Monthly Notices of the RoyaL Astronomical Society, 493(1), 17. doi:10.1093/mnras/staa324
• Rieke, M. J. (2020). JWST Noise Floor. I. Random Error Sources in JWST NIRCam Time Series. Astronomical Journal, 160(5), 19. doi:10.3847/1538-3881/abb811
• Rieke, M. J. (2020). Simulating JWST/NIRCam Color Selection of High-redshift Galaxies. Astrophysical Journal, 892(2), 22. doi:10.3847/1538-4357/ab7dc3
• Burke, C. J., Peterson, J. R., Egami, E., Leisenring, J. M., Sembroski, G. H., & Rieke, M. J. (2019). PhoSim-NIRCam: photon-by-photon image simulations of the James Webb Space Telescope's near-infrared camera. Journal of Astronomical Telescopes, Instruments, and Systems, 5, 038002.
• Rieke, M. J., Wright, G., Leggett, S. K., Dupuy, T., Morley, C., Marley, M., Best, W., Liu, M., Apai, D., Casewell, S., Geballe, T., Gizis, J., & Pineda, J. S. (2019). 3.8 μm Imaging of 400-600 K Brown Dwarfs and Orbital Constraints for WISEP J045853.90+643452.6AB. Astrophysical Journal, 882(2), 15. doi:10.3847/1538-4357/ab3393
• Wilson, J., Hearty, F., Skrutskie, M., Majewski, S., Holtzman, J., Eisenstein, D., Gunn, J., Blank, B., Henderson, C., Smee, S., Nelson, M., Nidever, D., Arns, J., Barkhouser, R., Barr, J., Beland, S., Bershady, M., Blanton, M., Brunner, S., , Burton, A., et al. (2019). The Apache Point Observatory Galactic Evolution Experiment (APOGEE) Spectrographs. pasp, 131(999), 055001.
• Rieke, M. J., Schlawin, E., Greene, T. P., Line, M., & Fortney, J. (2018). Clear and Cloudy Exoplanet Forecasts for JWST: Maps, Retrieved Composition, and Constraints on Formation with MIRI and NIRCam. Astrophysical Journal, 156, 40 to 51. doi:10.3847/1538-3881/aac774
• Williams, C. C., Curtis-Lake, E., Hainline, K. N., Chevallard, J., Robertson, B. E., Charlot, S., Endsley, R., Stark, D. P., Willmer, C., Alberts, S., Amorin, R., Arribas, S., Baum, S., Bunker, A., Carniani, S., Crandall, S., Egami, E., Eisenstein, D. J., Ferruit, P., , Husemann, B., et al. (2018). The JWST Extragalactic Mock Catalog: Modeling Galaxy Populations from the UV through the Near-IR over 13 Billion Years of Cosmic History. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 236(2).
• Greene, T., Kelly, D., Stansberry, J., Leisenring, J., Egami, E., Schlawin, E., Chu, L., Hodapp, K., & Rieke, M. (2017). $\lambda$ = 2.4 to 5 $\mu$m spectroscopy with the James Webb Space Telescope NIRCam instrument. Journal of Astronomical Telescopes, Instruments, and Systems, 3(3), 035001.
• Schlawin, E., Rieke, M., Leisenring, J., Walker, L., Fraine, J., Kelly, D., Misselt, K., Greene, T., Line, M., Lewis, N., & Stansberry, J. (2017). Two NIRCam Channels are Better than One: How JWST Can Do More Science with NIRCam\rsquos Short-wavelength Dispersed Hartmann Sensor. \pasp, 129(1), 015001.
• Garcia-Marin, M., Willmer, C., Labiano, A., Alberts, S., Rieke, G., Wright, G., & Rieke, M. (2016). Optimizing Parallel Observations for the JWST/MIRI Instrument. OBSERVATORY OPERATIONS: STRATEGIES, PROCESSES, AND SYSTEMS VI, 9910.
• Greene, T. P., Chu, L., Egami, E., Hodapp, K. W., Kelly, D. M., Leisenring, J., Rieke, M., Robberto, M., Schlawin, E., & Stansberry, J. (2016). Slitless spectroscopy with the James Webb Space Telescope Near-Infrared Camera (JWST NIRCam). SPACE TELESCOPES AND INSTRUMENTATION 2016: OPTICAL, INFRARED, AND MILLIMETER WAVE, 9904.
• Leisenring, J. M., Rieke, M., Misselt, K., & Robberto, M. (2016). Characterizing persistence in JWST NIRCam flight detectors. HIGH ENERGY, OPTICAL, AND INFRARED DETECTORS FOR ASTRONOMY VII, 9915.
• Rest, A., Hilbert, B., Leisenring, J. M., Misselt, K., Rieke, M., & Robberto, M. (2016). Gain determination of non-linear IR detectors with the differential photon transfer curve (dPTC) method. SPACE TELESCOPES AND INSTRUMENTATION 2016: OPTICAL, INFRARED, AND MILLIMETER WAVE, 9904.
• Eisner, J. A., Rieke, G. H., Rieke, M. J., Flaherty, K. M., Stone, J. M., Arnold, T. J., Cortes, S. R., Cox, E., Hawkins, C., Cole, A., Zajac, S., & Rudolph, A. L. (2015). Time-monitoring observations of Br gamma emission from young stars. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 447(1), 202-217.
• Thompson, R. I., Eisenstein, D., Fan, X., & Rieke, M. (2015). Constraints on the cosmic near-infrared background excess from NICMOS deep field observations. ASTROPHYSICAL JOURNAL, 657(2), 669-680.
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  NICMOS observations of the resolved object fluxes in the Hubble Deep Field-North and the Hubble Ultra Deep Field are significantly below the fluxes attributed to a 1.4-1.8 mu m near-infrared background excess (NIRBE) from previous low spatial resolution NIRS measurements. Tests placing sources in the NICMOS image with fluxes sufficient to account for the NIRBE indicate that the NIRBE flux must be either flat on scales greater than 100 '' or clumped on scales of several arcminutes to avoid detection in the NICMOS image. A fluctuation analysis of the new NICMOS data shows a fluctuation spectrum consistent with that found at the same wavelength in deep 2MASS calibration images. The fluctuation analysis shows that the majority of the fluctuation power comes from resolved galaxies at redshifts of 1.5 and less and that the fluctuations observed in the earlier deep 2MASS observations can be completely accounted for with normal low-redshift galaxies. Neither the NICMOS direct flux measurements nor the fluctuation analysis require an additional component of near-infrared flux other than the flux from normal resolved galaxies in the redshift range between 0 and 7. The residual fluctuations in the angular range between 1 '' and 10 '' is 1-2 nW m(-2) sr(-1), which is at or above several predictions of fluctuations from high redshift Population III objects, but inconsistent with attributing the entire NIRBE to high-redshift galaxies.
• {Broderick}, A., {Narayan}, R., {Kormendy}, J., {Perlman}, E., {Rieke}, M., , S. (2015). "{The Event Horizon of M87}". apj, 805, 179.
• {Eisner}, J., {Rieke}, G., {Rieke}, M., {Flaherty}, K., {Stone}, J., {Arnold}, T., {Cortes}, S., {Cox}, E., {Hawkins}, C., {Cole}, A., {Zajac}, S., , A. (2015). "{Time-monitoring observations of Br{$gamma$} emission from young stars}". mnras, 447, 202-217.
• Hinz, J. L., Rieke, M. J., Rieke, G. H., Willmer, C. N., Misselt, K., Engelbracht, C. W., & Blaylock, M. (2014). Spitzer observations of low-luminosity isolated and low surface brightness galaxies. ASTROPHYSICAL JOURNAL, 663(2), 895-907.
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  We examine the infrared properties offive low surface brightness galaxies ( LSBGs) and compare them with related but higher surface brightness galaxies, using Spitzer Space Telescope images and spectra. All the LSBGs are detected in the 3.6 and 4.5 mu m bands, representing the stellar population. All but one are detected at 5.8 and 8.0 mu m, revealing emission from hot dust and aromatic molecules, although many are faint or pointlike at these wavelengths. Detections of LSBGs at the far- infrared wavelengths of 24, 70, and 160 mu m are varied in morphology and brightness, with only two detections at 160 mu m, resulting in highly varied spectral energy distributions. Consistent with previous expectations for these galaxies, we find that detectable dust components exist for only some LSBGs, with the strength of dust emission dependent on the existence of bright star- forming regions. However, the far- infrared emission may be relatively weak compared with normal star- forming galaxies.
• Rieke, M. J. (2014). Observations of Transiting Exoplanets with the James Webb Space Telescope (JWST). PASP, 126(946), 40.
• Rieke, M. J. (2014). Tracing Ram-pressure Stripping with Warm Molecular Hydrogen Emission. Astrophysical Journal, 796, 25.
• Dey, A., Bian, C., Soifer, B., Brand, K., Brown, M., Chaffee, F., Le Floc'h, E., Hill, G., Houck, ., Jannuzi, B., Rieke, M., Weedman, D., Brodwin, M., & Eisenhardt, P. (2013). Discovery of a large similar to 200 kpc gaseous nebula at z approximate to 2.7 with the Spitzer Space Telescope. ASTROPHYSICAL JOURNAL, 629(2), 654-666.
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  We report the discovery of a very large, spatially extended Ly alpha-emitting nebula at z=2.656 associated with a luminous mid-infrared source. The bright mid-infrared source (F-24 mu m=0.86 mJy) was first detected in observations made using the Spitzer Space Telescope. Existing broadband imaging data from the NOAO Deep Wide-Field Survey revealed the mid-infrared source to be associated with a diffuse, spatially extended, optical counterpart in the B-W band. Spectroscopy and further imaging of this target reveals that the optical source is an almost purely line-emitting nebula with little, if any, detectable diffuse continuum emission. The Ly alpha nebula has a luminosity of L-Ly alpha approximate to 1.7x10(44) ergs s(-1) and an extent of at least 20" (160 kpc). Its central approximate to 8" shows an ordered, monotonic velocity profile; interpreted as rotation, this region encloses a mass M approximate to 6x10(12) M circle dot. Several sources lie within the nebula. The central region of the nebula shows narrow (approximate to 365 km s(-1)) emission lines of C (IV) and He (II). The mid-infrared source is a compact object lying within the nebula but offset from the center by a projected distance of approximate to 2".5 ( 20 kpc), and likely to be an enshrouded AGN. A young star-forming galaxy lies near the northern end of the nebula. We suggest that the nebula is a site of recent multiple galaxy and AGN formation, with the spatial distribution of galaxies within the nebula perhaps tracking the formation history of the system.
• Beichman, C. A., Rieke, M., Eisenstein, D., Greene, T. P., Krist, J., McCarthy, D., Meyer, M., & Stansberry, J. (2012). Science Opportunities with the Near-IR Camera (NIRCam) on the James Webb Space Telescope (JWST). SPACE TELESCOPES AND INSTRUMENTATION 2012: OPTICAL, INFRARED, AND MILLIMETER WAVE, 8442.
• Beichman, C. A., Rieke, M., Eisenstein, D., Greene, T. P., Krist, J., McCarthy, D., Meyer, M., & Stansberry, J. (2012). Science opportunities with the Near-IR Camera (NIRCam) on the James Webb Space Telescope (JWST). Proceedings of SPIE - The International Society for Optical Engineering, 8442.
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  Abstract: The Near-Infrared Camera (NIRCam) on the James Webb Space Telescope (JWST) offers revolutionary gains in sensitivity throughout the 1-5 μm region. NIRCam will enable great advances in all areas of astrophysics, from the composition of objects in our own Kuiper Belt and the physical properties of planets orbiting nearby stars to the formation of stars and the detection of the youngest galaxies in the Universe. NIRCam also plays an important role in initial alignment of JWST and the long term maintenance of its image quality. NIRCam is presently undergoing instrument Integration and Test in preparation for delivery to the JWST project. Key near-term milestones include the completion of cryogenic testing of the entire instrument; demonstration of scientific and wavefront sensing performance requirements; testing of replacement H2RG detectors arrays; and an analysis of coronagraphic performance in light of (image) measured telescope wavefront characteristics. This paper summarizes the performance of NIRCam, the scientific and education/outreach goals of the science team, and some results of the on-going testing program. © 2012 SPIE.
• Finkelstein, K. D., Papovich, C., Finkelstein, S. L., Willmer, C. N., Rigby, J. R., Rudnick, G., Egami, E., Rieke, M., & Smith, J. -. (2012). PROBING THE STAR FORMATION HISTORY AND INITIAL MASS FUNCTION OF THE z similar to 2.5 LENSED GALAXY SMM J163554.2+661225 WITH HERSCHEL. ASTROPHYSICAL JOURNAL, 742(2).
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  We present the analysis of Herschel Spectral and Photometric Imaging Receiver far-infrared (FIR) observations of the z = 2.515 lensed galaxy SMM J163554.2+661225. Combining new 250, 350, and 500 mu m observations with existing data, we make an improved fit to the FIR spectral energy distribution of this galaxy. We find a total infrared (IR) luminosity of L(8-1000 mu m) = 6.9 +/- 0.6 x 10(11) L-circle dot, a factor of three more precise over previous L-IR estimates for this galaxy, and one of the most accurate measurements for any galaxy at these redshifts. This FIR luminosity implies an unlensed star formation rate (SFR) for this galaxy of 119 +/- 10 M-circle dot yr(-1), which is a factor of 1.9 +/- 0.35 lower than the SFR derived from the nebular Pa alpha emission line (a 2.5 sigma discrepancy). Both SFR indicators assume an identical Salpeter initial mass function (IMF) with slope Gamma = 2.35 over a mass range of 0.1-100 M-circle dot; thus this discrepancy suggests that more ionizing photons may be necessary to account for the higher Pa alpha-derived SFR. We examine a number of scenarios and find that the observations can be explained with a varying star formation history (SFH) due to an increasing SFR, paired with a slight flattening of the IMF. If the SFR is constant in time, then larger changes need to be made to the IMF by either increasing the upper mass cutoff to similar to 200 M-circle dot, or a flattening of the IMF slope to 1.9 +/- 0.15, or a combination of the two. These scenarios result in up to double the number of stars with masses above 20 M-circle dot, which produce the requisite increase in ionizing photons over a Salpeter IMF with a constant SFH.
• Rauscher, B. J., Stahle, C., Hill, R. J., Greenhouse, M., Beletic, J., Babu, S., Blake, P., Cleveland, K., Cofie, E., Eegholm, B., Engelbracht, C. W., Hall, D. N., Hoffman, A., Jeffers, B., Jhabvala, C., Kimble, R. A., Kohn, S., Kopp, R., Lee, D., , Leidecker, H., et al. (2012). Commentary: JWST near-infrared detector degradation-finding the problem, fixing the problem, and moving forward. AIP Advances, 2(2).
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  Abstract: The JamesWebb Space Telescope (JWST) is the successor to the Hubble Space Telescope. JWST will be an infrared-optimized telescope, with an approximately 6.5 m diameter primary mirror, that is located at the Sun-Earth L2 Lagrange point. Three of JWST's four science instruments use Teledyne HgCdTe HAWAII-2RG (H2RG) near infrared detector arrays. During 2010, the JWST Project noticed that a few of its 5 ìm cutoff H2RG detectors were degrading during room temperature storage, and NASA chartered a "Detector Degradation Failure Review Board" (DD-FRB) to investigate. The DD-FRB determined that the root cause was a design flaw that allowed indium to interdiffuse with the gold contacts and migrate into the HgCdTe detector layer. Fortunately, Teledyne already had an improved design that eliminated this degradation mechanism. During early 2012, the improved H2RG design was qualified for flight and JWST began making additional H2RGs. In this article, we present the two public DD-FRB "Executive Summaries" that: (1) determined the root cause of the detector degradation and (2) defined tests to determine whether the existing detectors are qualified for flight.We supplement these with a brief introduction to H2RG detector arrays, some recent measurements showing that the performance of the improved design meets JWST requirements, and a discussion of how the JWST Project is using cryogenic storage to retard the degradation rate of the existing flight spare H2RGs. Copyright © 2012 Author(s).
• Cool, R. J., Kochanek, C. S., Eisenstein, D. J., Stern, D., Brand, K., Brown, M. J., Dey, A., Eisenhardt, P. R., Fan, X., Gonzalez, A. H., Green, R. F., Jannuzi, B. T., McKenzie, E. H., Rieke, G. H., Rieke, M., Soifer, B. T., Spinrad, H., & Elston, R. J. (2011). The discovery of three new z > 5 quasars in the AGN and Galaxy Evolution Survey. ASTRONOMICAL JOURNAL, 132(2), 823-830.
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  We present the discovery of three z > 5 quasars in the AGN and Galaxy Evolution Survey spectroscopic observations of the NOAO Deep Wide-Field Survey (NDWFS) Bootes Field. These quasars were selected as part of a larger Spitzer mid-infrared quasar sample, with no selection based on optical colors. The highest redshift object, NDWFS J142516.3+325409, at z 5: 85, is the lowest luminosity z = 5.8 quasar currently known. We compare mid-infrared techniques for identifying z > 5 quasars to more traditional optical techniques and show that mid-infrared colors allow for the selection of high-redshift quasars even at redshifts at which quasars lie near the optical stellar locus and at z > 7, where optical selection is impossible. Using the superb multiwavelength coverage available in the NDWFS Bootes field, we construct the spectral energy distributions (SEDs) of high-redshift quasars from observed BW band to 24 mu m (rest-frame 600 angstrom-3.7 mu m). We show that the three high-redshift quasars have quite similar SEDs, and the rest-frame composite SED of low-redshift quasars from the literature shows little evolution compared to our high-redshift objects. We compare the number of z > 5 quasars we have discovered to the expected number from published quasar luminosity functions. While analyses of the quasar luminosity function are tenuous based on only three objects, we find that a relatively steep luminosity function with Psi alpha L-3.2 provides the best agreement with the number of high-redshift quasars discovered in our survey.
• Finkelstein, K. D., Papovich, C., Finkelstein, S. L., N., C., Rigby, J. R., Rudnick, G., Egami, E., Rieke, M., & Smith, J. -. (2011). Probing the star formation history and initial mass function of the z ∼ 2.5 lensed galaxy SMM J163554.2+661225 with Herschel. Astrophysical Journal, 742(2).
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  Abstract: We present the analysis of Herschel Spectral and Photometric Imaging Receiver far-infrared (FIR) observations of the z = 2.515 lensed galaxy SMM J163554.2+661225. Combining new 250, 350, and 500 μm observations with existing data, we make an improved fit to the FIR spectral energy distribution of this galaxy. We find a total infrared (IR) luminosity of L(8-1000 μm) = 6.9 ± 0.6 × 1011L⊙, a factor of three more precise over previous LIR estimates for this galaxy, and one of the most accurate measurements for any galaxy at these redshifts. This FIR luminosity implies an unlensed star formation rate (SFR) for this galaxy of 119 ± 10M⊙yr-1, which is a factor of 1.9 ± 0.35 lower than the SFR derived from the nebular Paα emission line (a 2.5σ discrepancy). Both SFR indicators assume an identical Salpeter initial mass function (IMF) with slope Γ = 2.35 over a mass range of 0.1-100M⊙; thus this discrepancy suggests that more ionizing photons may be necessary to account for the higher Paα-derived SFR. We examine a number of scenarios and find that the observations can be explained with a varying star formation history (SFH) due to an increasing SFR, paired with a slight flattening of the IMF. If the SFR is constant in time, then larger changes need to be made to the IMF by either increasing the upper mass cutoff to ∼200M⊙, or a flattening of the IMF slope to 1.9 ± 0.15, or a combination of the two. These scenarios result in up to double the number of stars with masses above 20M⊙, which produce the requisite increase in ionizing photons over a Salpeter IMF with a constant SFH. © 2011. The American Astronomical Society. All rights reserved.
• Mao, Y., Andersen, T. B., Kubo, T., Virgen, M., Chan, H., Feller, G., Huff, L. W., Smith, E., Vasudevan, G., Somerstein, S., Jamieson, T., Horner, S., Krist, J., Beichman, C. A., Barone, C., Schmidt, R., Levin, D., Seymour, S., Kelly, D., & Rieke, M. J. (2011). NIRCam coronagraphic Lyot stop: Design, fabrication and testing. Proceedings of SPIE - The International Society for Optical Engineering, 8150.
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  Abstract: The NIRCam instrument on the James Webb Space Telescope (JWST) will provide a coronagraphic imaging capability to search for extrasolar planets in the 2 - 5 microns wavelength range. This capability is realized by a set of Lyot pupil stops with patterns matching the occulting mask located in the JWST intermediate focal plane in the NIRCam optical system. The complex patterns with transparent apertures are made by photolithographic process using a metal coating in the opaque region. The optical density needs to be high for the opaque region, and transmission needs to be high at the aperture. In addition, the Lyot stop needs to operate under cryogenic conditions. We will report on the Lyot stop design, fabrication and testing in this paper. © 2011 SPIE.
• Papovich, C., Rudnick, G., Rigby, J. R., N., C., Smith, J. -., Finkelstein, S., Egami, E., & Rieke, M. (2011). Erratum: Paschen-α Emission in the gravitationally lensed galaxy SMM J163554.2+661225 (Astrophysical Journal (2009) 704 (1506)). Astrophysical Journal, 742(2).
• Scoville, N., Polletta, M., Ewald, S., Stolovy, ., Thompson, R., & Rieke, M. (2011). High-mass, OB star formation in M51: Hubble Space Telescope H alpha and P alpha alpha imaging. ASTRONOMICAL JOURNAL, 122(6), 3017-3045.
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  We have obtained H alpha and P alpha alpha emission-line images covering the central 3'-4' of M51 using the WFPC2 and NICMOS instruments on the Hubble Space Telescope to study the high-mass stellar population. The 0."1-0."2 pixels provide 4.6-9 pc resolution in M51, and the H alpha /P alpha line ratios are used to obtain extinction estimates. A sample of 1373 H Phi emission regions is cataloged using an automated and uniform measurement algorithm. Their sizes are typically 10-100 pc. The luminosity function for the H alpha emission regions is obtained over the range L(H alpha) = 10(36) to 2 x 10(39) ergs s(-1). The luminosity function is fitted well by a power law with dN/d1n L(proportional to) L(-1.01). The power law is significantly truncated, and no regions were found with observed L(H alpha) above 2 x 10(39) ergs s(-1) (uncorrected for extinction). (The maximum seen in ground-based studies is approximately a factor of 5 higher, very likely because of the blending of multiple regions.) The extinctions derived here increase the maximum intrinsic luminosity to above 10(40) ergs s(-1). The logarithmically binned luminosity function is also somewhat steeper (alpha = -1.01) than that found from ground-based imaging (alpha = -0.5 to -0.8)-probably also a result of our resolving regions that were blended in the ground-based images. The two-point correlation function for the H II regions exhibits strong clustering on scales less than or equal to2", or 96 pc.
• Beichman, C. A., Krist, J., Trauger, J. T., Greene, T., Oppenheimer, B., Sivaramakrishnan, A., Doyon, R., Boccaletti, A., Barman, T. S., & Rieke, M. (2010). Imaging young giant planets from ground and space. Publications of the Astronomical Society of the Pacific, 122(888), 162-200.
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  Abstract: High-contrast imaging can find and characterize gas giant planets around nearby young stars and the closest M stars, complementing radial velocity and astrometrie searches by exploring orbital separations inaccessible to indirect methods. Ground-based coronagraphs are already probing within 25 AU of nearby young stars to find objects as small as ∼3 MJup. This paper contrasts near-term and future ground-based capabilities with high-contrast imaging modes of the James Webb Space Telescope (JWST). Monte Carlo modeling reveals that JWST can detect planets with masses as small as 0.2 MJup across a broad range of orbital separations. We present new calculations for planet brightness as a function of mass and age for specific JWSTfilters and extending to 0.1 MJup. © 2010. The Astronomical Society of the Pacific. All rights reserved.
• Brown, M., Brand, K., Dey, A., Jannuzi, B., Cool, R., Le Floc'h, E., Kochanek, C., Armus, L., Bian, C., Higdon, J., Higdon, S., Papovich, C., Rieke, G., Rieke, M., Smith, J., Soifer, B., & Weedman, D. (2010). The 1 < z < 5 infrared luminosity function of type I quasars. ASTROPHYSICAL JOURNAL, 638(1), 88-99.
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  We determine the rest-frame 8 mu m luminosity function of type I quasars over the redshift range 1 < z < 5. Our sample consists of 292 24 mu m sources brighter than 1 mJy selected from 7.17 deg(2) of the Spitzer Space Telescope MIPS survey of the NOAO DeepWide-Field Survey Bootes field. The AGN and Galaxy Evolution Survey (AGES) has measured redshifts for 270 of the R < 21.7 sources, and we estimate that the contamination of the remaining 22 sources by stars and galaxies is low. We are able to select quasars missed by ultraviolet excess quasar surveys, including reddened type I quasars and 2.2 < z < 3.0 quasars with optical colors similar to main-sequence stars. We find that reddened type I quasars comprise similar to 20% of the type I quasar population. Nonetheless, the shape, normalization, and evolution of the rest-frame 8 mu m luminosity function are comparable to those of quasars selected from optical surveys. The 8 mu m luminosity function of type I quasars is well approximated by a power law with index -2.75 +/- 0.14. We directly measure the peak of the quasar space density to be at z = 2.6 +/- 0.3.
• Greene, T., Beichman, C., Gully-Santiago, M., Jaffe, D., Kelly, D., Krist, J., Rieke, M., & Smith, E. H. (2010). NIRCam:Development and testing of the JWST Near-Infrared Camera. Proceedings of SPIE - The International Society for Optical Engineering, 7731.
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  Abstract: The Near Infrared Camera (NIRCam) is one of the four science instruments of the James Webb Space Telescope (JWST). Its high sensitivity, high spatial resolution images over the 0.6 - 5 μxm wavelength region will be essential for making significant findings in many science areas as well as for aligning the JWST primary mirror segments and telescope. The NIRCam engineering test unit was recently assembled and has undergone successful cryogenic testing. The NIRCam collimator and camera optics and their mountings are also progressing, with a brass-board system demonstrating relatively low wavefront error across a wide field of view. The flight model's long-wavelength Si grisms have been fabricated, and its coronagraph masks are now being made. Both the short (0.6 - 2.3 μm) and long (2.4 - 5.0 μm) wavelength flight detectors show good performance and are undergoing final assembly and testing. The flight model subsystems should all be completed later this year through early 2011, and NIRCam will be cryogenically tested in the first half of 2011 before delivery to the JWST integrated science instrument module (ISIM). © 2010 SPIE.
• MINNITI, D., OLSZEWSKI, E., & RIEKE, M. (2010). THE BULGE OF M33. ASTROPHYSICAL JOURNAL, 410(2), L79-L82.
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  H-band imaging of the central region of the Local Group galaxy M33 reveals a bulge with effective radius 0.5 kpc. The brightest bulge stars are resolved. After subtraction of disk contamination, we conclude that the brightest M33 bulge stars are substantially brighter than the brightest stars found in the Milky Way bulge. This fact suggests that the star formation histories of all bulges are not the same; specifically, M33's bulge underwent a star formation episode less than 1 Gyr ago.
• Papovich, C., Momcheva, I., Willmer, C. N., Finkelstein, K. D., Finkelstein, S. L., Tran, K. -., Brodwin, M., Dunlop, J. S., Farrah, D., Khan, S. A., Lotz, J., McCarthy, P., McLure, R. J., Rieke, M., Rudnick, G., Sivanandam, S., Pacaud, F., & Pierre, M. (2010). A spitzer-selected galaxy cluster at z = 1.62. Astrophysical Journal Letters, 716(2), 1503-1513.
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  Abstract: We report the discovery of a galaxy cluster at z = 1.62 located in the Spitzer Wide-Area Infrared Extragalactic survey XMM-LSS field. This structure was selected solely as an overdensity of galaxies with red Spitzer/Infrared Array Camera colors, satisfying ([3.6] - [4.5])AB> - 0.1mag. Photometric redshifts derived from the Subaru XMM Deep Survey (BViz bands), the UKIRT Infrared Deep Survey-Ultra-Deep Survey (UKIDSS-UDS, JK bands), and from the Spitzer Public UDS survey (3.6-8.0 μm) show that this cluster corresponds to a surface density of galaxies at z 1.6 that is >20σ above the mean at this redshift. We obtained optical spectroscopic observations of galaxies in the cluster region using IMACS on the Magellan telescope. We measured redshifts for seven galaxies in the range z = 1.62-1.63 within 2.8arcmin (1.7mag. The photometric-redshift probability distributions for the red galaxies are strongly peaked at z = 1.62, coincident with the spectroscopically confirmed galaxies. The rest-frame (U - B) color and scatter of galaxies on the red sequence are consistent with a mean luminosity-weighted age of 1.2 0.1Gyr, yielding a formation redshift , and corresponding to the last significant star formation period in these galaxies. © 2010. The American Astronomical Society. All rights reserved.
• Schneider, G., Smith, B., Becklin, E., Koerner, D., Meier, R., Hines, D., Lowrance, P., Terrile, R., Thompson, R., & Rieke, M. (2010). NICMOS imaging of the HR 4796A circumstellar disk. ASTROPHYSICAL JOURNAL, 513(2), L127-L130.
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  We report the first near-infrared (NIR) imaging of a circumstellar annular disk around the young (similar to 8 Myr), Vega-like star HR 4796A. NICMOS coronagraph observations at 1.1 and 1.6 mu m reveal a ringlike symmetrical structure that peaks in reflected intensity 1." 05 +/- 0." 02 (similar to 70 AU) from the central AO V star. The ring geometry, with an inclination of 73.degrees 1 +/- 1.degrees 2 and a major axis position angle of 26.degrees 8 +/- 0.degrees 6, is in good agreement with recent 12.5 and 20.8 mu m observations of a truncated disk. The ring is resolved with a characteristic width of less than 0." 26 (17 AU) and appears abruptly truncated at both the inner and outer edges. The region of the disk-plane inward of similar to 60 AU appears to be relatively free of scattering material. The integrated flux density of the part of the disk that is visible (greater than 0." 65 from the star) is found to be 7.6 +/- 0.5 and 7.4 +/- 1.2 mJy at 1.1 and 1.6 mu m, respectively. Correcting for the unseen area of the ring yields total flux densities of 12.8 +/- 1.0 and 12.5 +/- 2.0 mJy, respectively (Vega magnitudes equal to 12.92 +/- 0.08 and 12.35 +/- 0.18). The NIR luminosity ratio is evaluated from these results and ground-based photometry of the star. At these wavelengths, L-disk(lambda)/L-*(lambda) is equal to 1.4 +/- 0.2 x 10(-3) and 2.4 +/- 0.5 x 10(-3), giving reasonable agreement between the stellar flux scattered in the NIR and that which is absorbed in the visible and reradiated in the thermal infrared. The somewhat red reflectance of the disk at these wavelengths implies a mean particle size in excess of several microns, which is larger than typical interstellar grains. The confinement of material to a relatively narrow annular zone implies dynamical constraints on the disk particles by one or more as yet unseen bodies.
• Finkelstein, S. L., Papovich, C., Rudnick, G., Egami, E., Floc'H, E. L., Rieke, M. J., Rigby, J. R., & N., C. (2009). Turning back the clock: Inferring the history of the eight O'clock arc. Astrophysical Journal Letters, 700(1 PART 2), 376-386.
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  Abstract: We present the results from an optical and near-infrared (NIR) spectroscopic study of the ultraviolet-luminous z = 2.73 galaxy, the 8 o'clock arc. Due to gravitational lensing, this galaxy is magnified by a factor of μ > 10, allowing in-depth measurements which are usually unfeasible at such redshifts. In the optical spectra, we measured the systemic redshift of the galaxy, z = 2.7322 ± 0.0012, using stellar photospheric lines. This differs from the redshift of absorption lines in the interstellar medium, z = 2.7302 ± 0.0006, implying gas outflows on the order of 160 km s -1. With H- and K-band NIR spectra, we have measured nebular emission lines of Hα,Hβ,Hλ ,[NII], and [O III], which have a redshift z = 2.7333 ± 0.0001, consistent with the derived systemic redshift. From the Balmer decrement, we measured the dust extinction in this galaxy to be A5500 = 1.17 ± 36 mag. Correcting the Hα line flux for dust extinction as well as the assumed lensing factor, we measure a star formation rate (SFR) of ∼270 M⊙ yr-1, which is higher than ∼85% of star-forming galaxies at z ∼ 2-3. Using combinations of all detected emission lines, we find that the 8 o'clock arc has a gas-phase metallicity of ∼0.8 Z⊙, showing that enrichment at high redshift is not rare, even in blue, star-forming galaxies. Studying spectra from two of the arc components separately, we find that one component dominates both the dust extinction and SFR, although the metallicities between the two components are similar. We derive the mass via stellar population modeling, and find that the arc has a total stellar mass of ∼4.2 x 1011 M⊙, which falls on the mass-metallicity relation at z ∼ 2. Finally, we estimate the total gas mass, and find it to be only ∼12% of the stellar mass, implying that the 8 o'clock arc is likely nearing the end of a starburst. © 2009. The American Astronomical Society. All rights reserved.
• Krist, J. E., Balasubramanian, K., Beichman, C. A., Echternach, P. M., Green, J. J., Liewer, K. M., Muller, R. E., Serabyn, E., Shaklan, S. B., Trauger, J. T., Wilson, D. W., Horner, S. D., Mao, Y., Somerstein, S. F., Vasudevan, G., Kelly, D. M., & Rieke, M. J. (2009). The JWST/NIRCam coronagraph: Mask design and fabrication. Proceedings of SPIE - The International Society for Optical Engineering, 7440.
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  Abstract: The NIRCam instrument on the James Webb Space Telescope will provide coronagraphic imaging from λ =1-5 μm of high contrast sources such as extrasolar planets and circumstellar disks. A Lyot coronagraph with a variety of circular and wedge-shaped occulting masks and matching Lyot pupil stops will be implemented. The occulters approximate grayscale transmission profiles using halftone binary patterns comprising wavelength-sized metal dots on anti-reflection coated sapphire substrates. The mask patterns are being created in the Micro Devices Laboratory at the Jet Propulsion Laboratory using electron beam lithography. Samples of these occulters have been successfully evaluated in a coronagraphic testbed. In a separate process, the complex apertures that form the Lyot stops will be deposited onto optical wedges. The NIRCam coronagraph flight components are expected to be completed this year. © 2009 Copyright SPIE - The International Society for Optical Engineering.
• Mao, Y., Harrison, D., Richardson, T., Schulz, B., Taylor, D., Huff, L. W., Horner, S., Kelly, D., & Rieke, M. J. (2009). Cryogenic spectral performance of bandpass filters for NIRCam instruments. Proceedings of SPIE - The International Society for Optical Engineering, 7439.
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  Abstract: The Bandpass Filters in the NIRCam instrument are required to have high throughput in bandpass spectral region and excellent out-of-band blocking over the entire region of detector spectral response. The high throughput is needed for the instrument to have high sensitivity for detecting distant galaxies, and the out-ofband blocking is needed for accurate calibration on James Webb Space Telescope. The operating temperature of the instrument is at cryogenic temperature from 32 Kelvin to 39.5 Kelvin. We have performed spectral measurement of NIRCam bandpass filters at cryogenic temperature after three cryo-to-ambient cycles. We will report the experiment and results in this paper. This work was performed and funded by NASA Goddard Space Flight Center under Prime Contract NAS5-02105. © 2009 SPIE.
• Papovich, C., Rudnick, G., Rigby, J. R., N., C., Smith, J. -., Finkelstein, S. L., Egami, E., & Rieke, M. (2009). Paschen-α emission in the gravitationally lensed galaxy SMM. Astrophysical Journal Letters, 704(2), 1506-1518.
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  Abstract: We report the detection of the Paα emission line in the z = 2.515 galaxy SMM J163554.2+661225 using Spitzer spectroscopy. SMM J163554.2+661225 is a submillimeter-selected infrared-luminous galaxy maintaining a high star formation rate (SFR), with no evidence of an active galactic nucleus from optical or infrared spectroscopy, nor X-ray emission. This galaxy is lensed gravitationally by the cluster Abell 2218, making it accessible to Spitzer spectroscopy. We measure a line luminosity, L(Paα) = (2.05 0.33) × 1042 erg s-1, corrected for gravitational lensing. Comparing the Hα and Paα luminosities, we derive a nebular extinction, A(V) = 3.6 0.4mag. The dust-corrected luminosity, L(Paα) = (2.57 0.43) × 1042 erg s-1, corresponds to an ionization rate, Q 0 = (1.6 0.3) × 1055 γs-1. The instantaneous SFR is ψ = 171 28 M ȯ yr-1, assuming a Salpeter-like initial mass function from 0.1 to 100 M ȯyr-1. The total IR luminosity derived using 70, 450, and 850μm data is LIR = (5-10) × 1011 L ⊙, corrected for gravitational lensing. This corresponds to ψ = 90-180 M ⊙ yr-1, where the upper range is consistent with that derived from the Paα luminosity. While the L(8 μm)/L(Paα) ratio is consistent with the extrapolated relation observed in local galaxies and star-forming regions, the rest-frame 24μm luminosity is significantly lower with respect to local galaxies of comparable Paα luminosity. Thus, SMM J163554.2+661225 arguably lacks a warmer dust component (TD ∼ 70 K), which is associated with deeply embedded star formation, and which contrasts with local galaxies with comparable SFRs. Rather, the starburst in SMM J163554.2+661225 is consistent with star-forming local galaxies with intrinsic luminosities, L IR 1010 L ⊙, but "scaled up" by a factor of 10-100. © 2009. The American Astronomical Society. All rights reserved.
• ZARITSKY, D., RIEKE, M., RIX, H., Dejonghe, H., & Habing, H. (2009). IR IMAGING OF SPIRAL GALAXY BULGES. GALACTIC BULGES, 441-442.
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  Imaging in the infrared (2.2 mu) minimizes the impact of dust obscuration and allows reliable mapping of the mass-tracing stellar population in spiral galaxies. We find dramatic differences compared to photometry at shorter wavelengths (e.g. 0.8 mu). As an example, the observations of the mini-bar and inner spiral arms of M 51 are discussed.
• Beichman, C. A., Krist, J., Trauger, J. T., Greene, T., Oppenheimer, B., Sivaramakrishnan, A., Doyon, R., Boccaletti, A., Barman, T. S., & Rieke, M. (2008). Imaging Young Giant Planets From Ground and Space. PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC, 122(888), 162-200.
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  High-contrast imaging can find and characterize gas giant planets around nearby young stars and the closest M stars, complementing radial velocity and astrometric searches by exploring orbital separations inaccessible to indirect methods. Ground-based coronagraphs are already probing within 25 AU of nearby young stars to find objects as small as similar to 3 M(Jup). This paper contrasts near-term and future ground-based capabilities with high-contrast imaging modes of the James Webb Space Telescope (JWST). Monte Carlo modeling reveals that JWST can detect planets with masses as small as 0.2 M(Jup) across a broad range of orbital separations. We present new calculations for planet brightness as a function of mass and age for specific JWST filters and extending to 0.1 M(Jup).
• Thompson, R., Rieke, M., Schneider, G., Hines, D., & Corbin, M. (2008). Initial on-orbit performance of NICMOS. ASTROPHYSICAL JOURNAL, 492(2), L95-+.
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  On 1997 February 13, Space Shuttle astronauts placed the Near-Infrared Camera and Multiobject Spectrometer (NICMOS) into the Hubble Space Telescope. Following installation, the servicing mission orbital verification program (SMOV) performed extensive testing of the instrument to verify that it can be operated and calibrated effectively. This program is essentially completed, and routine science observations have begun in most of the NICMOS modes of operation. This Letter describes the performance levels of NICMOS at this time.
• Brown, M., Brand, K., Dey, A., Jannuzi, B. T., Cool, R., Le, F. E., Kochanek, C. S., Armus, L., Bian, C., Higdon, J., Higdon, S., Papovich, C., Rieke, G., Rieke, M., Smith, J. D., Soifer, B. T., & Weedman, D. (2007). The 1 < z < 5 infrared luminosity function of type I quasars (vol 638, pg 88, 2006). ASTROPHYSICAL JOURNAL, 657(1), 641-641.
• Dinshaw, N., Evans, A., Epps, H., Scoville, N., & Rieke, M. (2007). NICMOS observations of interaction-triggered star formation in the luminous infrared galaxy NGC 6090. ASTROPHYSICAL JOURNAL, 525(2), 702-708.
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  High-resolution 1.1, 1.6, and 2.2 mu m imaging of the luminous infrared galaxy NGC 6090 obtained with NICMOS on the Hubble Space Telescope is presented. These new observations are centered on the two nuclei of the merger and reveal the spiral structure of the eastern galaxy and the amorphous nature of the western galaxy. The nuclear separation of 3.2 kpc (H-0 = 75 km s(-1) Mpc(-1)) indicates that NGC 6090 is at an intermediate stage of merging. Bright knots/clusters are also visible in the region overlapping the merging galaxies; four of these knots appear bluer than the underlying galaxies and have colors consistent with young (less than or equal to 10(7) yr) star clusters. The spatial coincidence of the knots with the molecular gas in NGC 6090 indicates that much of the present star formation is occurring outside the nuclear region of merging galaxies, consistent with recent studies of other double nucleus luminous infrared galaxies.
• Greene, T., Beichman, C., Eisenstein, D., Horner, S., Kelly, D., Mao, Y., Meyer, M., Rieke, M., & Shi, F. (2007). Observing exoplanets with the JWST NIRCam grisms. Proceedings of SPIE - The International Society for Optical Engineering, 6693.
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  Abstract: The near-infrared camera (NIRCam) on the James Webb Space Telescope (JWST) will incorporate 2 identical grisms in each of its 2 long wavelength channels. These transmission gratings have been added to assist with the coarse phasing of the JWST telescope, but they will also be used for slitless wide-field scientific observations over selectable regions of the A = 2.4 - 5.0 μm. wavelength range at spectroscopic resolution R ≡ λ/δλX ≃ 2000. We describe the grism design details and their expected performance in NIRCam. The grisms will provide pointsource continuum sensitivity of approximately AB = 23 mag in 10,000 s exposures with S/N = 5 when binned to R = 1000. This is approximately a factor of 3 worse than expected for the JWST NIRSpec instrument, but the NIRCam grisms provide better spatial resolution, better spectrophotometric precision, and complete field coverage. The grisms will be especially useful for high precision spectrophotometric observations of transiting exoplanets. We expect that R = 500 spectra of the primary transits and secondary eclipses of Jupiter-sized exoplanets can be acquired at moderate or high signal-to-noise for stars as faint as M = 10 - 12 mag in 1000 s of integration time, and even bright stars (V = 5 mag) should be observable without saturation. We also discuss briefly how these observations will open up new areas of exoplanet science and suggest other unique scientific applications of the grisms.
• Krist, J. E., Beichman, C. A., Trauger, J. T., Rieke, M. J., Somerstein, S., Green, J. J., Horner, S. D., Stansberry, J. A., Shi, F., Meyer, M. R., Stapelfeldt, K. R., & Roellig, T. L. (2007). Hunting planets and observing disks with the JWST NIRCam coronagraph. Proceedings of SPIE - The International Society for Optical Engineering, 6693.
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  Abstract: The expected stable point spread function, wide field of view, and sensitivity of the NIRCam instrument on the James Webb Space Telescope (JWST) will allow a simple, classical Lyot coronagraph to detect warm Jovian-mass companions orbiting young stars within 150 pc as well as cool Jupiters around the nearest low-mass stars. The coronagraph can also be used to study protostellar and debris disks. At λ = 4.5 μm, where young planets are particularly bright relative to their stars, and at separations beyond ∼0.5 arcseconds, the low space background gives JWST significant advantages over ground-based telescopes equipped with adaptive optics. We discuss the scientific capabilities of the NIRCam coronagraph, describe the technical features of the instrument, and present end-to-end simulations of coronagraphic observations of planets and circumstellar disks.
• Murray, S., Kenter, A., Forman, W., Jones, C., Green, P., Kochanek, C., Vikhlinin, A., Fabricant, D., Fazio, G., Brand, K., Brown, M., Dey, A., Jannuzi, B., Najita, J., McNamara, B., Shields, J., & Rieke, M. (2007). XBootes: An X-ray survey of the NDWFS Bootes field. I. Overview and initial results. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 161(1), 1-8.
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  We obtained a 5 ks deep Chandra X-ray Observatory ACIS-I map of the 9.3 deg(2) Bootes field of the NOAO Deep Wide-Field Survey. Here we describe the data acquisition and analysis strategies leading to a catalog of 4642 ( 3293) point sources with 2 or more ( 4 or more) counts, corresponding to a limiting flux of roughly 4(8) x 10(-15) ergs cm(-2) s(-1) in the 0.5 - 7 keV band. These Chandra XBootes data are unique in that they constitute the widest contiguous X-ray field yet observed to such a faint flux limit. Because of the extraordinarily low background of the ACIS, we expect only 14% (0.7%) of the sources to be spurious. We also detected 43 extended sources in this survey. The distribution of the point sources among the 126 pointings (ACIS-I has a 16' x 16' field of view) is consistent with Poisson fluctuations about the mean of 36.8 sources per pointing. While a smoothed image of the point source distribution is clumpy, there is no statistically significant evidence of large-scale filamentary structure. We do find however, that for theta > 1', the angular correlation function of these sources is consistent with previous measurements, following a power law in angle with slope similar to - 0.7. In a 1.4 deg(2) sample of the survey, approximately 87% of the sources with 4 or more counts have an optical counterpart to R similar to 26 mag. As part of a larger program of optical spectroscopy of the NDWFS Bootes area, spectra have been obtained for similar to 900 of the X-ray sources, most of which are quasars or active galactic nuclei.
• TEGLER, S., CAMPINS, H., LARSON, S., KLEINE, M., KELLY, D., & RIEKE, M. (2007). SIMULTANEOUS VISIBLE AND NEAR-INFRARED SPECTROPHOTOMETRY OF COMET AUSTIN 1989C(1). ASTROPHYSICAL JOURNAL, 396(2), 711-716.
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  Simultaneous visible and near-infrared spectra of comet Austin were obtained with the 1.5 m and 2.3 m telescopes of the University of Arizona Observatories on 1990 May 16. The visible spectrum obtained with the IHW spectrograph covers the 3126-9490 angstrom wavelength interval, while the near-infrared spectrum obtained with the germanium spectrometer covers the 9036-12794 angstrom wavelength interval. For the first time, we present simultaneous measurements of integrated band fluxes for the CN B 2-SIGMA+-X 2-SIGMA+ (violet) and A 2-PI+-X 2-SIGMA+ (red) systems. We also present a CN spectrum and CN band flux ratios calculated from a fluoresence equilibrium model. From a comparison between the observed and calculated CN spectra and band flux ratios, we find that red system oscillator strengths determined from recent ab initio calculations appropriately describe the radiative properties of CN molecules.
• ZARITSKY, D., RIX, H., & RIEKE, M. (2007). INNER SPIRAL STRUCTURE OF THE GALAXY M51. NATURE, 364(6435), 313-315.
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  MODELLING the structure and kinematics of spiral galaxies requires accurate maps of the mass-tracing stellar population. But this has hitherto been difficult because of dust obscuration and the presence of luminous young stars. To minimize the effects of dust and maximize sensitivity to the dominant stellar population, we have obtained K-band (2.2-mum) images of the nearby 'grand-design' spiral galaxy NGC5194 (M51). Our observations reveal remarkable dynamical structures not visible in conventional optical images. We find that the spiral arms extend significantly further towards the galaxy's centre than previously observed and can be traced continuously through almost three revolutions - roughly twice as far as with optical images. The coherence of the arms over this large radial range challenges current theories of spiral structure. We suggest that a combination of several mechanisms, such as the interaction of M51 with the neighbouring galaxy NGC5195, forcing by the central 'bar', or distortions from density waves, is required to generate the observed structure.
• Lowrance, P., McCarthy, C., Becklin, E., Zuckerman, B., Schneider, G., Webb, R., Hines, D., Kirkpatrick, J., Koerner, D., Low, F., Meier, R., Rieke, M., Smith, B., Terrile, R., & Thompson, R. (2006). A candidate substellar companion to CD -33 degrees 7795 (TWA 5). ASTROPHYSICAL JOURNAL, 512(1), L69-L72.
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  We present the discovery of a candidate substellar object in a survey of young stars in the solar vicinity using the sensitivity and spatial resolution afforded by the NICMOS coronagraph on the Hubble Space Telescope. The H = 12.1 mag object was discovered approximately 2" from the TW Hydrae association member CD -33 degrees 7795 (TWA 5), and the photometry implies a spectral type M8-M8.5, with a temperature of similar to 2600 K. We estimate that the probability of a chance alignment with a background object of this nature is less than 2 x 10(-5) and therefore postulate that the object (TWA 5B) is physically associated at a projected separation of 100 AU, Given the likely youth of the primary (similar to 10 Myr), current brown dwarf cooling models predict a mass of approximate to 20M(Jup) for TWA 5B.
• Papovich, C., Momcheva, I., Willmer, C. N., Finkelstein, K. D., Finkelstein, S. L., Tran, K. -., Brodwin, M., Dunlop, J. S., Farrah, D., Khan, S. A., Lotz, J., McCarthy, P., McLure, R. J., Rieke, M., Rudnick, G., Sivanandam, S., Pacaud, F., & Pierre, M. (2006). A SPITZER-SELECTED GALAXY CLUSTER AT z=1.62. ASTROPHYSICAL JOURNAL, 716(2), 1503-1513.
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  We report the discovery of a galaxy cluster at z = 1.62 located in the Spitzer Wide-Area Infrared Extragalactic survey XMM-LSS field. This structure was selected solely as an overdensity of galaxies with red Spitzer/Infrared Array Camera colors, satisfying ([3.6] - [4.5]) AB > -0.1 mag. Photometric redshifts derived from the Subaru XMM Deep Survey (BV iz bands), the UKIRT Infrared Deep Survey-Ultra-Deep Survey (UKIDSS-UDS, JK bands), and from the Spitzer Public UDS survey (3.6-8.0 mu m) show that this cluster corresponds to a surface density of galaxies at z approximate to 1.6 that is >20 sigma above the mean at this redshift. We obtained optical spectroscopic observations of galaxies in the cluster region using IMACS on the Magellan telescope. We measured redshifts for seven galaxies in the range z = 1.62-1.63 within 2.8 arcmin ( 1.7 mag. The photometric-redshift probability distributions for the red galaxies are strongly peaked at z = 1.62, coincident with the spectroscopically confirmed galaxies. The rest-frame (U - B) color and scatter of galaxies on the red sequence are consistent with a mean luminosity-weighted age of 1.2 +/- 0.1 Gyr, yielding a formation redshift (z(f)) over bar = 2.35 +/- 0.10, and corresponding to the last significant star formation period in these galaxies.
• Rothberg, B., Whitmore, B., Schweizer, F., Chandar, R., Van, R., Rossa, J., Blair, W., Mengel, S., & Rieke, M. (2006). The formation of young clusters in three ongoing galaxy mergers. Proceedings of the International Astronomical Union, 2(S235), 240-.
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  Abstract: High-resolution, multi-wavelength (UV through NIR) imaging from the Hubble Space Telescope has been obtained for three mergers in the Toomre Sequence, NGC 520, NGC 2623, & NGC 3256, to identify and measure the properties of young Globular Cluster (GC) candidates. Unlike previous merger studies, this work focuses on objects that lie in the middle of the Toomre Sequence. This age range represents a critical dynamical transition in the merging sequence between ongoing mergers and advanced remnants with properties more akin to elliptical galaxies. The early results of our investigation include luminosity functions and age-dating of the GC candidates. These results also address the impact of the dynamical state of the merger on the current young cluster population as compared with earlier studies that have dealt with the very oldest and very youngest mergers in the Toomre Sequence. © 2007 International Astronomical Union.
• Thompson, R., Eisenstein, D., Fan, X., Rieke, M., & Kennicutt, R. (2006). NICMOS measurements of the near-infrared background. NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA B-GENERAL PHYSICS RELATIVITY ASTRONOMY AND MATHEMATICAL PHYSICS AND METHODS, 122(9-11), 941-946.
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  This paper addresses the nature of the near-infrared background. We investigate whether there is an excess background at 1.4 microns; what is the source of the near-infrared background and whether that background after the subtraction of all known sources contains the signature of high-redshift objects (Z > 10). Based oil NICMOS observations in the Hubble Ultra Deep Field and the Northern Hubble Deep Field we find that there is no excess in the background at 1.4 microns and that the claimed excess is elite to inaccurate models of the zodiacal background. We find that the near-infrared background is now spatially resolved amid is dominated by galaxies in the redshift range between 0.5 and 1.5. We find no signature than can be attributed to high-redshift sources after subtraction of all known sources either ill the residual background or in the fluctuations of the residual background. We show that the color of the fluctuations from both NICMOS and Spitzer observations are consistent with low-redshift objects and inconsistent with objects at redshifts greater than 10. It is most likely that the residual fluctuation power after source subtraction is due to the outer regions of low-redshift galaxies that are below the source detection limit and therefore not removed during the source subtraction.
• BECHTOLD, J., ELVIS, M., FIORE, F., KUHN, O., CUTRI, R., MCDOWELL, J., RIEKE, M., SIEMIGINOWSKA, A., & WILKES, B. (2005). X-RAY SPECTRAL EVOLUTION OF HIGH-REDSHIFT QUASARS. ASTRONOMICAL JOURNAL, 108(3), 759-765.
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  At z approximate to 3, the x-ray spectra of radio-loud and radio-quiet quasars are different. High-redshift radio-quiet quasars either have large absorbing columns, N-H, and steeper power law spectral indices, alpha(E), than low redshift quasars, or no absorption and similar alpha(E)'s. In contrast, the radio-loud quasars at high redshift have substantial absorption and similar alpha(E)'s to low redshift quasars. Implications for the interpretation of the evolution of the luminosity function of quasars are discussed. If the absorption arises outside the central engine for both radio-loud and radio-quiet quasars, then radio-quiet quasars differ from the radio-loud quasars in that their emitted power law spectrum has evolved with redshift. We argue that this favors models where quasars are numerous and short-lived, rather than rare and long-lived.
• Green, J. J., Beichman, C., Basinger, S. A., Horner, S., Meyer, M., Redding, D. C., Rieke, M., & Trauger, J. T. (2005). High contrast imaging with the JWST NIRCAM coronagraph. Proceedings of SPIE - The International Society for Optical Engineering, 5905, 1-11.
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  Abstract: Relative to ground-based telescopes, the James Webb Space Telescope (JWST) will have a substantial sensitivity advantage in the 2.2-5μm wavelength range where brown dwarfs and hot Jupiters are thought to have significant brightness enhancements. To facilitate high contrast imaging within this band, the Near-Infrared Camera (NIRCAM) will employ a Lyot coronagraph with an array of band-limited image-plane occulting spots. In this paper, we provide the science motivation for high contrast imaging with NIRCAM, comparing its expected performance to that of the Keck, Gemini and 30 m (TMT) telescopes equipped with Adaptive Optics systems of different capabilities. We then describe our design for the NIRCAM coronagraph that enables imaging over the entire sensitivity range of the instrument while providing significant operational flexibility. We describe the various design tradeoffs that were made in consideration of alignment and aberration sensitivities and present contrast performance in the presence of JWST's expected optical aberrations. Finally we show an example of a two-color image subtraction that can provide 10-5 companion sensitivity at sub-arcsecond separations.
• Loose, M., Beletic, J., Blackwell, J., Garnett, J., Wong, S., Hall, D., Jacobson, S., Rieke, M., & Winters, G. (2005). The SIDECAR ASIC - Focal plane electronics on a single chip. Proceedings of SPIE - The International Society for Optical Engineering, 5904, 1-10.
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  Abstract: Traditionally, focal plane arrays require extensive external focal plane electronics (FPE) to provide clocks and biases as well as to digitize the analog output signals. The FPE has to be well-designed and is typically large, heavy and powerhungry. Most importantly, the FPE has to be placed some distance away from the FPA, which complicates maintaining low noise performance throughout the complete system. To offer an alternative to the discrete electronics, Rockwell Scientific has developed a new approach known as the SIDECAR application-specific integrated circuit (ASIC). This single chip provides all the functionality necessary to operate an infrared array with the convenience of a pure digital interface to the outside world. This paper will present performance data on the latest generation of the SIDECAR ASIC operating the JWST H2RG detector arrays at cryogenic temperature. The test results demonstrate that an ASIC based FPA system will meet or exceed all performance requirements for the JWST mission. The SIDECAR ASIC has been selected by NASA to become the FPA drive electronics for all shortwave infrared instruments on JWST.
• McCaughrean, M., Chen, H., Bally, J., Erickson, E., Thompson, R., Rieke, M., Schneider, G., Stolovy, S., & Young, E. (2005). High-resolution near-infrared imaging of the Orion 114-426 silhouette disk. ASTROPHYSICAL JOURNAL, 492(2), L157-+.
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  We present the first high-resolution near-infrared images of the edge-on silhouette circumstellar disk, Orion 114-426, made using NICMOS on the Hubble Space Telescope. Images taken against the bright nebular background of the ionized hydrogen Pa alpha line at 1.87 mu m show the major axis of the disk to be approximately 20% smaller than at 0.6 mu m, from which we deduce the structure of the edge of the disk. Continuum images of diffuse polar lobes above and below the plane of the disk show a morphology and evolution with wavelength consistent with predictions for reflection nebulae in a diffuse envelope with large polar cavities, surrounding a thin, massless, Keplerian disk, centered on an otherwise hidden central star. We make use of our observations and reasonable assumptions about the underlying disk structure to show that the disk mass is at least 10 M+ and plausibly greater than or equal to 5 x 10(-4) M-..
• Rieke, M. J., Kelly, D., & Horner, S. (2005). Overview of James Webb Space Telescope and NIRCam's role. Proceedings of SPIE - The International Society for Optical Engineering, 5904, 1-8.
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  Abstract: The James Webb Space Telescope (JWST) is the scientific successor to both the Hubble Space Telescope and the Spitzer Space Telescope. It is envisioned as a facility-class mission. The instrument suite provides broad wavelength coverage and capabilities aimed at four key science themes: 1)The End of the Dark Ages: First Light and Reionization; 2) The Assembly of Galaxies; 3) The Birth of Stars and Protoplanetary Systems; and 4) Planetary Systems and the Origins of Life. NIRCam is the 0.6 to 5 micron imager for JWST, and it is also the facility wavefront sensor used to keep the primary mirror in alignment.
• Scoville, N., Stolovy, ., Rieke, M., Christopher, M., & Yusef-Zadeh, F. (2005). Hubble Space Telescope Pa alpha and 1.9 micron imaging of Sagittarius A West. ASTROPHYSICAL JOURNAL, 594(1), 294-311.
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  We present Hubble Space Telescope/NICMOS images at 0."2 resolution (Nyquist-sampled in the central 19") of the H I Paalpha emission line in a 70"(alpha) x 90"(delta) region of the Galactic center centered on the nonthermal radio source Sgr A*. The majority of the emission arises from ionized gas in the minispiral in the central parsec. Paalpha emission is also seen from 26 stellar sources, presumably early-type stars with mass-loss winds. The new data reveal significant small-scale structure (less than or equal to 1" similar to 1.2 x 10(17) cm) in the ionized gas of the mini-spiral; low surface brightness emission features are also seen for the first time. The ratio of observed Paalpha emission to 6 cm radio continuum emission is used to derive an extinction map for the ionized gas over the central parsec. A(V) varies from 20 to 50 mag with a median value of A(V) = 31.1 mag, in excellent agreement with earlier estimates derived for the stellar sources. Extinctions, independently derived using H92alpha recombination-line data, were in excellent agreement with those derived from the 6 cm continuum. A broad minimum in the extinction extends similar to30" northeast-southwest over the area of the IRS 16 cluster, including the area of peak flux in Paalpha and radio continuum. Large increases in extinction are seen along the periphery of the ionized gas, particularly in the direction of the western arm, suggesting that the ionized gas is partially extincted by dust in the molecular clouds at the outside of the ionized region; however, the H II cannot be entirely behind the molecular clouds since the extinctions would then be much greater. The minimum Lyman continuum emission rate within 40" radius of Sgr A* is 3.9 x 10(50) s(-1) or L(LyC) similar or equal to 2.7 x 10(6) L(.), half of this within 20" radius. The small-scale, filamentary structures in the ionized gas have a free thermal expansion time of only similar to3000 yr; either magnetic fields or mass-loss winds from the hot emission line stars may contain the ionized. laments. (Eight new emission-line stars were also detected in Paalpha.) For both the ionized gas and stellar continuum, the centroids of the emission (corrected for extinction) remain within similar to+/-1" from a radius of 2" out to 40". This provides further evidence that Sgr A* (the putative central black hole) is indeed at or extremely close (less than or equal to0.04 pc or 1.2 x 10(17) cm) to the center of the Galactic nucleus stellar distribution and presumably the dynamical center of the Galaxy. The 1.9 mum surface brightness increases inwards to 0."9 radius and exhibits a decrease or leveling off closer to Sgr A*, possibly indicating the core radius of the central stellar distribution or depletion of the late-type stars by stellar collisions near the central black hole.
• Weedman, D. W., Soifer, B. T., Hao, L., Higdon, J. L., Higdon, S. J., Houck, J. R., Le Floc'h, E., Brown, M. J., Dey, A., Jannuzi, B. T., Rieke, M., Desai, V., Bian, C., Thompson, D., Armus, L., Teplitz, H., Eisenhardt, P., & Willner, S. P. (2005). Spitzer IRS spectra of optically faint infrared sources with weak spectral features. ASTROPHYSICAL JOURNAL, 651(1), 101-112.
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  Spectra have been obtained with the low-resolution modules of the Infrared Spectrograph (IRS) on the Spitzer Space Telescope (Spitzer) for 58 sources having f(v)(24 mu m) > 0.75 mJy. Sources were chosen from a survey of 8.2 deg(2) within the NOAO Deep Wide-Field Survey region in Bootes (NDWFS) using the Multiband Imaging Photometer (MIPS) on Spitzer. Most sources are optically very faint (I > 24 mag). Redshifts have previously been determined for 34 sources, based primarily on the presence of a deep 9.7 mu m silicate absorption feature, with a median z of 2.2. Spectra are presented for the remaining 24 sources for which we were previously unable to determine a confident redshift because the IRS spectra show no strong features. Optical photometry from the NDWFS and infrared photometry with MIPS and the Infrared Array Camera on Spitzer (IRAC) are given, with K photometry from the Keck I telescope for some objects. The sources without strong spectral features have overall spectral energy distributions (SEDs) and distributions among optical and infrared fluxes that are similar to those for the sources with strong absorption features. Nine of the 24 sources are found to have feasible redshift determinations based on fits of a weak silicate absorption feature. Results confirm that the "1 mJy" population of 24 mu m Spitzer sources that are optically faint is dominated by dusty sources with spectroscopic indicators of an obscured AGN rather than a star-burst. There remain 14 of the 58 sources observed in Bootes for which no redshift could be estimated, and 5 of these sources are invisible at all optical wavelengths.
• Chen, H., Bally, J., O'Dell, C., McCaughrean, M., Thompson, R., Rieke, M., Schneider, G., & Young, E. (2004). 2.12 Micron molecular hydrogen emission from circumstellar disks embedded in the Orion Nebula. ASTROPHYSICAL JOURNAL, 492(2), L173-+.
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  We present narrowband images of two externally illuminated circumstellar disks embedded in the Orion Nebula. The images were taken with camera 2 of the Near-Infrared Camera and Multiobject Spectrometer (NICMOS) as part of the Hubble Space Telescope Early Release Observations program. Molecular hydrogen emission is confined to the silhouettes embedded in the objects HST 10 (182-413) and HST 17 (183-419). This emission appears to trace the surfaces of nearly edge-on circumstellar disks and is likely to be excited by the intense far-ultraviolet (FUV) radiation field produced by nearby O stars. The presence of this emission confirms that FUV radiation penetrates to the disk surface. The absence of H-2 emission in the region between the ionization front and the disk surface provides evidence that this medium is predominantly atomic. Our observations constitute the first demonstration that the dense circumstellar disks embedded in the proplyds are predominately molecular. While the central star is marginally detected at 2.15 mu m in HST 10, the central star of HST 17 is clearly detected.
• Davila, P., Bos, B., Contreras, J., Evans, C., Greenhouse, M., Hobbs, G., Holota, W., Huff, L. W., Hutchings, J., Jamieson, T. H., Lightsey, P., Morbey, C., Murowinski, R., Rieke, M., Rowlands, N., Steakley, B., Wells, M., Plate, M. T., & Wright, G. (2004). The James Webb Space Telescope science instrument suite: An overview of optical designs. Proceedings of SPIE - The International Society for Optical Engineering, 5487(PART 2), 611-627.
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  Abstract: The James Webb Space Telescope (JWST) Observatory, the follow-on mission to the Hubble Space Telescope and to the Spitzer Space Facility, will yield astounding breakthroughs in the realms of infrared space science. The science instrument suite for this Observatory will consist of a Near-Infrared Camera, a Near-Infrared Spectrograph, a Mid-Infrared Instrument with imager, coronagraph and integral field spectroscopy modes, and a Fine Guider System Instrument with both a Guider module and a Tunable Filter Module. In this paper we present an overview of the optical designs of the telescope and instruments.
• Horner, S., & Rieke, M. (2004). The near infrared camera (NIRCam) for the James Webb Space Telescope (JWST). Proceedings of SPIE - The International Society for Optical Engineering, 5487(PART 2), 628-634.
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  Abstract: The NIRCam science objectives are the detection and identification of "first light" objects, the study of star and brown dwarf formation, and the detection and characterization of planetary systems and their formation. These three science programs are also the key objectives of the JWST program as a whole. The NIRCam instrument design is optimized for these objectives within the mission constraints. NIRCam consists of two optics modules, each with a field of view of 2.2 arcmin square. The modules are identical except for the mechanical layout. Each module consists of two channels divided by a dichroic beamsplitter. The short wavelength channel has a band pass of 0.6 - 2. 3 microns, with pixels sized for Nyquist sampling of the PSF at 2.0 microns. The long wavelength channel has a band pass of 2.4 - 5.0 microns, with pixels sized for Nyquist sampling at 4.0 microns. Selections of wide (R~4), intermediate (R~10), and narrow (R~100) bandwidth filters are provided in each of the four channels, along with coronagraphic occulting masks and pupil stops. A refractive optical design results in a smaller instrument volume and mass, provides good images at the pupils for wavefront sensing and coronagraphy, allows good access to the pupils and focal planes, and relaxes the alignment requirements compared to a reflective design.
• Kaaret, P., Alonso-Herrero, A., III, J. G., Fabbiano, G., Zezas, A., & Rieke, M. J. (2004). Displacement of X-ray sources from star clusters in starburst galaxies. Monthly Notices of the Royal Astronomical Society, 348(2), L28-L32.
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  Abstract: We examine the spatial offsets between X-ray point sources and star clusters in three starburst galaxies. We find that the X-ray sources are preferentially located near the star clusters. Because the star clusters are very good tracers of the star formation activity in the galaxies, this indicates that the X-ray sources are young objects associated with current star formation. We find significant displacements of the X-ray sources from the clusters. These displacements are likely due to motion of the X-ray sources and indicates that they are X-ray binaries. We find that brighter X-ray sources preferentially occur closer to clusters. The absence of very bright sources at large displacements from clusters may help constrain models of the sources.
• Kern, S., McCarthy, D., Buie, M., Brown, R., Campins, H., & Rieke, M. (2004). Compositional variation on the surface of Centaur 8405 Asbolus. ASTROPHYSICAL JOURNAL, 542(2), L155-L159.
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  Near-infrared 1-2 mum spectra of the Centaur 8405 Asbolus (1995 GO) have been obtained using the Hubble Space Telescope near-infrared camera and multiobject spectrometer. Strong and variable absorption features indicate a significantly inhomogeneous surface characterized by water ice mixed with additional unknown constituents. Over a 1.7 hr interval, the observed spectra varied from a nearly featureless spectrum to a very complicated absorption spectrum, and the integrated flux varied in a manner consistent with previous light-curve observations. The accepted rotation period of 8.9351 hr assumes a shape-dominated light curve. Our observations indicate that the light curve may in fact be dominated by a relatively bright spot with a period of 4.47 hr, i.e., half the previous value.
• Papovich, C., Dickinson, M., Ferguson, H. C., Giavalisco, M., Lotz, J., Madau, P., Idzi, R., Kretchmer, C., Moustakas, L. A., F., D., Gardner, J. P., Rieke, M. J., Somerville, R. S., & Stern, D. (2004). Evolution in the colors of lyman break galaxies from z ∼ 4 to z ∼ 3. Astrophysical Journal Letters, 600(2 II), L111-L114.
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  Abstract: The integrated colors of distant galaxies provide a means for interpreting the properties of their stellar content. Here we use rest-frame UV-to-optical colors to constrain the spectral energy distributions and stellar populations of color-selected, B-dropout galaxies at z ∼ 4 in the Great Observatories Origins Deep Survey (GOODS). We combine the Advanced Camera for Surveys data with ground-based near-infrared images, which extend the coverage of galaxies at z ∼ 4 to the rest-frame B band. We observe a color-magnitude trend in the rest-frame m(UV)-B versus B diagram for the z ∼ 4 galaxies that has a fairly well-defined "blue envelope," and is strikingly similar to that of color-selected, U-dropout galaxies at z ∼ 3. We also find that although the co-moving luminosity density at rest-frame UV wavelengths (1600 Å) is roughly comparable at z ∼ 3 and ∼4, the luminosity density at rest-frame optical wavelengths increases by about one-third from z ∼ 4 to ∼3. Although the star formation histories of individual galaxies may involve complex and stochastic events, the evolution in the global luminosity density of the UV-bright galaxy population corresponds to an average star formation history with a star formation rate that is constant or increasing over these redshifts. This suggests that the evolution in the luminosity density corresponds to an increase in the stellar mass density of ≳33%.
• Sivaramakrishnan, A., Morse, E. C., Makidon, R. B., Bergeron, L. E., Casertano, S., Figer, D. F., Acton, D. S., Atcheson, P. D., & Rieke, M. J. (2004). Limits on routine wavefront sensing with NIRCam on JWST. Proceedings of SPIE - The International Society for Optical Engineering, 5487(PART 2), 909-917.
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  Abstract: The James Webb Space Telescope (JWST) will be a segmented, deployable, infrared-optimized 6.5m space telescope. Its active primary segments will be aligned, co-phased, and then fine-tuned in order to deliver image quality sufficient for the telescope's intended scientific goals. Wavefront sensing used to drive this fine tuning will come from the analysis of defocussed phase diverse images taken with its near-IR science camera, NIRCam. Here we concentrate on routine maintenance of the JWST primary, as might be expected to occur on a more or less monthly timescale after the telescope is commissioned. We carry out an end-to-end optical and wavefront sensing simulation, starting from the primary mirror figure, calculating a noiseless point-spread function as it would appear on the detector, inject noise sources due to photon statistics, as well as detector and electronics characteristics (as measured in Rockwell HAWAII-2RG detectors in the lab), and reduce the data with a simple scheme to create one realization of a full wavefront sensing operation. We generate JWST point-spread functions for a given OPD map on a JWST pupil with -6, -3, 3, and 6 waves of focus, and simulate three realizations of the same exposure. We start with a mirror figure that provides a point-spread function (PSF) that is just under the acceptable specification for JWST's Strehl ratio, which is 80% at 2 microns in NIRCam. We do not include zodiacal light, diffuse sources, or contamination by other stars in our simulation. Our up-the-ramp exposures include a model of cosmic ray contamination of the data. We calibrate the image to account for dark current and flat field variation, and process the images with an implementation of the Misell-Gerchberg-Saxton algorithm assuming a known pupil support function. Our entire process is described here, to document a tool that helps to verify our intended method of maintaining the JWST PSF within specificatiuons during routine science operations.
• Watson, C. R., Kochanek, C. S., Forman, W. R., Hickox, R. C., Jones, C. J., Brown, M. J., Brand, K., Dey, A., Jannuzi, B. T., Kenter, A. T., Murray, S. S., Vikhlinin, A., Eisenstein, D. J., Fazio, G. G., Green, P. J., McNamara, B. R., Rieke, M., & Shields, J. C. (2004). THE STAR FORMATION AND NUCLEAR ACCRETION HISTORIES OF NORMAL GALAXIES IN THE AGES SURVEY. ASTROPHYSICAL JOURNAL, 696(2), 2206-2219.
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  We combine IR, optical, and X-ray data from the overlapping, 9.3 deg(2) NOAO Deep Wide-Field Survey, AGN and Galaxy Evolution Survey (AGES), and XBootes Survey to measure the X-ray evolution of 6146 normal galaxies as a function of absolute optical luminosity, redshift, and spectral type over the largely unexplored redshift range 0.1 less than or similar to z less than or similar to 0.5. Because only the closest or brightest of the galaxies are individually detected in X-rays, we use a stacking analysis to determine the mean properties of the sample. Our results suggest that X-ray emission from spectroscopically late-type galaxies is dominated by star formation, while that from early-type galaxies is dominated by a combination of hot gas and active galactic nucleus (AGN) emission. We find that the mean star formation and supermassive black hole accretion rate densities evolve like similar to (1 + z)(3 +/- 1), in agreement with the trends found for samples of bright, individually detectable starburst galaxies and AGN. Our work also corroborates the results of many previous stacking analyses of faint source populations, with improved statistics.
• Evans, A. S., Becklin, E. E., Scoville, N. Z., Neugebauer, G., Soifer, B. T., Matthews, K., Ressler, M., Werner, M., & Rieke, M. (2003). The compact nucleus of the deep silicate absorption galaxy NGC 4418. Astronomical Journal, 125(5 1769), 2341-2347.
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  Abstract: High-resolution Hubble Space Telescope (HST) near-infrared and Keck mid-infrared images of the heavily extinguished infrared-luminous galaxy NGC 4418 are presented. These data make it possible to observe the imbedded near-infrared structure on scales of 10-20 pc and to constrain the size of the mid-infrared-emitting region. The 1.1-2.2 μm data of NGC 4418 show no clear evidence of nuclear star clusters or of a reddened active galactic nucleus. Instead, the nucleus of the galaxy consists of a ∼100-200 pc linear structure with fainter structures extending radially outward. The near-infrared colors of the linear feature are consistent with a 10-300 Myr starburst suffering moderate levels (a few magnitudes) of visual extinction. At 7.9-24.5 μm NGC 4418 has estimated size upper limits in the range of 30-80 pc. These dimensions are consistent with the highest-resolution radio observations obtained to date of NGC 4418, as well as the size of 50-70 pc expected for a blackbody with a temperature derived from the 25, 60, and 100 μm flux densities of the galaxy. Further, a spectral energy distribution constructed from the multiwavelength mid-infrared observations shows the strong silicate absorption feature at 10 μm, consistent with previous mid-infrared observations of NGC 4418. An infrared surface brightness of ∼2.1 × 1013 L⊙ kpc-2 is derived for NGC 4418. Such a value, though consistent with the surface brightness of warm ultraluminous infrared galaxies [LIR (8-1000 μm) ≥ 10 12 L⊙], such as IRAS 05189-2524 and IRAS 08572+3915, is not large enough to distinguish NGC 4418 as a galaxy powered by an active galactic nucleus, as opposed to a lower surface brightness starburst.
• Grauer, A. D., Rieke, M. J., & Quillen, A. C. (2003). Infrared observations of galaxies in the local universe. II. 391 Calibrated images with photometric and structural measurements. Astrophysical Journal, Supplement Series, 149(2), 327-342.
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  Abstract: This paper presents empirical results from a deep imaging survey of galaxies in the local universe at the J and K s wavelengths. Three hundred ninety-one images have been obtained and calibrated using the same camera and filter set with the Steward Observatory 1.6 m Kuiper Telescope on Mount Bigelow and the 2.3 m Bok Telescope on Kitt Peak. The limiting magnitude is typically 22 mag arcsec -1 at J and 21 mag arcsec -1 at K s. The central surface brightness, apparent magnitudes, sizes, scale lengths, and inclinations are tabulated from measurements made using these data. The purpose of this paper is to provide basic near-infrared data on a variety of galaxy types.
• Kenter, A., Murray, S., Forman, W., Jones, C., Green, P., Kochanek, C., Vikhlinin, A., Fabricant, D., Fazio, G., Brand, K., Brown, M., Dey, A., Jannuzi, B., Najita, J., McNamara, B., Shields, J., & Rieke, M. (2003). XBootes: An X-ray survey of the NDWFS Bootes field. II. The X-ray source catalog. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 161(1), 9-20.
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  We present results from a Chandra survey of the 9 deg(2) Bootes field of the NOAO Deep Wide-Field Survey (NDWFS). This XBootes survey consists of 126 separate contiguous ACIS-I observations each of approximately 5000 s in duration. These unique Chandra observations allow us to search for large-scale structure and to calculate X-ray source statistics over a wide, contiguous field of view with arcsecond angular resolution and uniform coverage. Optical spectroscopic follow-up observations and the rich NDWFS data set will allow us to identify and classify these X- ray - selected sources. Using wavelet decomposition, we detect 4642 point sources with n >= 2 counts. In order to keep our detections similar to 99% reliable, we limit our list to sources with n >= 4 counts. For a 5000 s observation and assuming a canonical unabsorbed active galactic nucleus (AGN) type X-ray spectrum, a 4 count on-axis source corresponds to a flux of 4.7 x 10(-15) ergs cm(-2) s(-1) in the soft (0.5 - 2 keV) band, 1.5 x 10(-14) ergs cm(-2) s(-1) in the hard (2 - 7 keV) band, and 7.8 x 10(-15) ergs cm(2) s(-1) in the full (0.5 - 7 keV) band. The full 0.5 - 7 keV band n >= 4 count list has 3293 point sources. In addition to the point sources, 43 extended sources have been detected, consistent with the depth of these observations and the number counts of clusters. We present here the X- ray catalog for the XBootes survey, including source positions, X- ray fluxes, hardness ratios, and their uncertainties. We calculate and present the differential number of sources per flux density interval, N(S), for the point sources. In the soft (0.5 - 2 keV) band, N(S) is well fitted by a broken power law with slope of 2.60(-0.12)(+0.11) at bright fluxes and 1.74(-0.22)(+0.28) for faint fluxes. The hard source N(S) is well described by a single power law with an index of -2.93(-0.09)(+0.09).
• Scoville, N. Z., Stolovy, S. R., Rieke, M., Christopher, M., & Yusef-Zadeh, F. (2003). Hubble Space Telescope Paα and 1.9 Micron Imaging of Sagittarius a West. Astrophysical Journal Letters, 594(1 I), 294-311.
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  Abstract: We present Hubble Space Telescope/NICMOS images at 0″2 resolution (Nyquist-sampled in the central 19″) of the H I Paα emission line in a 70″ (a) × 90″ (δ) region of the Galactic center centered on the nonthermal radio source Sgr A*. The majority of the emission arises from ionized gas in the minispiral in the central parsec. Paα emission is also seen from 26 stellar sources, presumably early-type stars with mass-loss winds. The new data reveal significant small-scale structure (≤1″ ∼ 1.2 × 1017 cm) in the ionized gas of the minispiral; low surface brightness emission features are also seen for the first time. The ratio of observed Paa emission to 6 cm radio continuum emission is used to derive an extinction map for the ionized gas over the central parsec. AV varies from 20 to 50 mag with a median value of AV = 31.1 mag, in excellent agreement with earlier estimates derived for the stellar sources. Extinctions, independently derived using H92α recombination-line data, were in excellent agreement with those derived from the 6 cm continuum. A broad minimum in the extinction extends ∼30″ northeast-southwest over the area of the 1RS 16 cluster, including the area of peak flux in Paa and radio continuum. Large increases in extinction are seen along the periphery of the ionized gas, particularly in the direction of the western arm, suggesting that the ionized gas is partially extincted by dust in the molecular clouds at the outside of the ionized region; however, the H II cannot be entirely behind the molecular clouds since the extinctions would then be much greater. The minimum Lyman continuum emission rate within 40″ radius of Sgr A*is 3.9 × 1050 s-1 or L Lyc ≃ 2.7 × 106 L⊙, half of this within 20″ radius. The small-scale, filamentary structures in the ionized gas have a free thermal expansion time of only ∼3000 yr; either magnetic fields or mass-loss winds from the hot emission line stars may contain the ionized filaments. (Eight new emission-line stars were also detected in Paα.) For both the ionized gas and stellar continuum, the centroids of the emission (corrected for extinction) remain within ∼±1″ from a radius of 2″ out to 40″. This provides further evidence that Sgr A*(the putative central black hole) is indeed at or extremely close (≤0.04 pc or 1. 2 × 1017 cm) to the center of the Galactic nucleus stellar distribution and presumably the dynamical center of the Galaxy. The 1.9 μm surface brightness increases inwards to 0″.9 radius and exhibits a decrease or leveling off closer to Sgr A*, possibly indicating the core radius of the central stellar distribution or depletion of the late-type stars by stellar collisions near the central black hole.
• Scoville, N., Evans, A., Dinshaw, N., Thompson, R., Rieke, M., Schneider, G., Low, F., Hines, D., Stobie, B., Becklin, E., & Epps, H. (2003). NICMOS imaging of the nuclei of ARP 220. ASTROPHYSICAL JOURNAL, 492(2), L107-+.
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  We report high-resolution imaging of the ultraluminous infrared galaxy Arp 220 at 1.1, 1.6, and 2.22 mu m with the Near-Infrared Camera and Multiobject Spectrometer on the Hubble Space Telescope. The diffraction-limited images at 0".1-0".2 resolution clearly resolve both nuclei of the merging galaxy system and reveal for the first time a number of luminous star clusters in the circumnuclear envelope. The morphologies of both nuclei are strongly affected by dust obscuration, even at 2.2 mu m: the primary nucleus (west) presents a crescent shape, concave to the south, and the secondary (eastern) nucleus is bifurcated by a dust lane with the southern component being very reddened. In the western nucleus, the morphology of the 2.2 mu m emission is most likely the result of obscuration by an opaque disk embedded in the nuclear star cluster. The morphology of the central starburst cluster in the western nucleus is consistent with either a circumnuclear ring of star formation or a spherical cluster with the bottom half obscured by the embedded dust disk. Comparison of centimeter-wave radio continuum maps with the near-infrared images suggests that the radio nuclei lie in the dust disk on the west and near the highly reddened southern component of the eastern complex. The radio nuclei are separated by 0".98 (corresponding to 364 pc at 77 Mpc), and the half-widths of the infrared nuclei are similar to 0".2-0".5. At least eight unresolved infrared sources--probably globular clusters--are also seen in the circumnuclear envelope at radii of 2"-7". Their near-infrared colors do not significantly constrain their ages.
• Corbin, M. R., O'Neil, E., & Rieke, M. J. (2002). Hubble space telescope NICMOS imaging of the core of M87. Astronomical Journal, 124(1 1759), 183-190.
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  Abstract: We present broadband 1.1, 1.6, and 2.2 μm images and a 2.37 μm narrowband image of the inner 19″ of the nearby radio galaxy M87, obtained with the Near Infrared Camera and Multi-Object Spectrometer of the Hubble Space Telescope (HST). The isophotes of the broadband images are almost perfectly circular to within approximately 0″.5 (∼50 pc) of the active nucleus, and an r1/4 law provides a good fit to the galaxy brightness profile at these wavelengths to within the same distance. This result agrees with predictions that the nuclear supermassive black hole will produce a nearly spherical distribution of the surrounding stars within a galaxy crossing time. A difference image formed from the 1.6 μm image and a V-band image obtained with the HST Wide Field Planetary Camera 2 does not show any clear evidence of a physically thick dusty torus around the nucleus, consistent with its lack of strong thermal mid-infrared emission. If such a torus is present, our data indicate its outer radius to be less than 50 pc. The infrared broadband colors and 2.37 μm image (which is sensitive to the strength of the stellar CO absorption) show no gradients to a distance of approximately 5″ (∼400 pc) from the nucleus and are consistent with a population dominated by late M giants, with no evidence of recent star formation. However, the globular clusters in this region are confirmed to consist of stars bluer than the underlying galaxy, indicating a different formation history. The images and associated colors also confirm that the regions beyond the nucleus do not contain strongly concentrated dust, in contrast to many other radio galaxies. In combination with other recent observations, these results indicate that M87 represents the dynamically evolved product of past galaxy mergers and suggest that its nucleus is in the final stages of activity.
• BECHTOLD, J., ELVIS, M., FIORE, F., KUHN, O., CUTRI, R., MCDOWELL, J., RIEKE, M., SIEMIGINOWSKA, A., & WILKES, B. (2001). INFRARED TO X-RAY SPECTRAL ENERGY-DISTRIBUTIONS OF HIGH-REDSHIFT QUASARS. ASTRONOMICAL JOURNAL, 108(2), 374-394.
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  We have observed 14 quasars with z>2.8 with the ROSAT-PSPC, and detected 12 of them, including the z=4.11 quasar 0000-263. We present the first x-ray spectrum of a radio quiet quasar with z>3, 1946+768. Its x-ray spectrum is consistent with a power law with spectral index alpha(E) = 1.8(+2.1/-1.4) and no evidence for absorption in excess of the galactic column [alpha(E) = 1.00(+0.28/-0.32) assuming N(H) = N(H)(Gal)]. A PSPC hardness ratio is used to constrain the x-ray spectral properties of the quasars for which there were less than 100 photons detected. For the radio quiet quasars, [alpha(E)] almost-equal-to 1.2, if one assumes that there is no absorption in excess of the galactic column. We combine the x-ray data with new ground based optical and near-IR obtained at the Steward 2.3 m and Multiple Mirror Telescope, and data from the literature. The energy distributions are compared to those of low redshift objects. For the radio quiet quasars with z>2.5, the mean (alpha(ox)] approximately 1.8. This is larger than the mean for quasars, with z
• Corbin, M. R., O'Neil, E., & Rieke, M. J. (2001). Hubble space telescope NICMOS imaging of the cores of M31 and M32. Astronomical Journal, 121(5), 2549-2556.
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  Abstract: We present 1.1, 1.6, and 2.2 μm images of the cores of the Local Group galaxies M31 and M32 obtained with the Near Infrared Camera and Multi-Object Spectrometer of the Hubble Space Telescope (HST). These images are also compared with optical images of the galaxies obtained with the HST Wide Field Planetary Camera 2 (WFPC2). In M31, the nucleus remains distinctly asymmetric in all of the infrared bands, with no evidence of concentrated dust, although the distinction between the two nuclei, P1 and P2, is not as strong as in the WFPC2 and earlier WF/PC-1 images. This result is nonetheless consistent with the model of the nucleus as an eccentric stellar disk produced by the dynamical influence of a central supermassive black hole. Several individual M giant stars are detected within ∼3″ of the nuclei and may represent stars that have escaped from the disk and phase-mixed around the nuclear center of mass. In M32 we also do not find strong evidence of dust, and the brightness profiles within the central ∼1″ of the infrared images can be fitted by a power law of the same form as that fitted to the optical images. The infrared color profiles of the central few arcseconds of M32 show no strong gradients and indicate a population dominated by K giant stars. This is consistent with recent ground-based spectroscopy and photometry of the core region, which similarly show no strong gradients in age or metallicity within its stellar population.
• Helou, G., Roussel, H., Appleton, P., Frayer, D., Stolovy, S., Storrie-Lombardi, L., Hurt, R., Lowrance, P., Makovoz, D., Masci, F., Surace, J., Gordon, K., Alonso-Herrero, A., Engelbracht, C., Misselt, K., Rieke, G., Rieke, M., Willner, S., Pahre, M., , Ashby, M., et al. (2001). The anatomy of star formation in NGC 300. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 154(1), 253-258.
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  The Spitzer Space Telescope was used to study the mid-to far-infrared properties of NGC 300 and to compare dust emission to Halpha to elucidate the heating of the interstellar medium (ISM) and the star formation cycle at scales smaller than 100 pc. The new data allow us to discern clear differences in the spatial distribution of 8 mum dust emission with respect to 24 mum dust and to H II regions traced by Halpha light. The 8 mum emission highlights the rims of H II regions, and the 24 mum emission is more strongly peaked in star-forming regions than 8 mum. We confirm the existence and approximate amplitude of interstellar dust emission at 4.5 mum, detected statistically in Infrared Space Observatory (ISO) data, and conclude it arises in star-forming regions. When averaging over regions larger than similar to1 kpc, the ratio of Halpha to aromatic feature emission in NGC 300 is consistent with the values observed in disks of spiral galaxies. The mid-to far-infrared spectral energy distribution of dust emission is generally consistent with pre-Spitzer models.
• YUN, J., CLEMENS, D., MCCAUGHREAN, M., & RIEKE, M. (2001). NEAR-INFRARED DISCOVERY OF THE L810 NEBULA ILLUMINATOR. ASTROPHYSICAL JOURNAL, 408(2), L101-L103.
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  As part of a deep near-infrared imaging survey for infrared point sources in Bok globules, we have discovered the illuminator of the optical reflection nebula seen toward the Bok globule L810. The illuminator (L810 IRS) is located at the position predicted by Scarrott, Rolph, & Tadhunter from analysis of their optical polarimetry. This source is very red (J-K approximately 3.9) and bright (m(K) = 10.7), and has an estimated bolometric luminosity of 890 L.. Additionally, we found a near-infrared nebula which extends 20'' symmetrically to the north and to the south of L810 IRS, exhibiting an hourglass shape. Both the morphology and the orientation of the near-infrared nebula are in good agreement with the morphology and orientation of the high-velocity molecular outflow associated with L810. Finally, we found a near-infrared jetlike structure whose axis is collinear with L810 IRS. Together, these findings indicate that L810 IRS is likely to be a deeply embedded, very active intermediate-mass young stellar object within the L810 cloud.
• Kern, S. D., Mccarthy, D. W., Buie, M. W., Brown, R. H., Campins, H., & Rieke, M. (2000). Compositional variation on the surface of Centaur 8405 Asbolus. Astrophysical Journal Letters, 542(2 PART 2), L155-L159.
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  Abstract: Near-infrared 1-2 μm spectra of the Centaur 8405 Asbolus (1995 GO) have been obtained using the Hubble Space Telescope near-infrared camera and multiobject spectrometer. Strong and variable absorption features indicate a significantly inhomogeneous surface characterized by water ice mixed with additional unknown constituents. Over a 1.7 hr interval, the observed spectra varied from a nearly featureless spectrum to a very complicated absorption spectrum, and the integrated flux varied in a manner consistent with previous light-curve observations. The accepted rotation period of 8.9351 hr assumes a shape-dominated light curve. Our observations indicate that the light curve may in fact be dominated by a relatively bright spot with a period of 4.47 hr, i.e., half the previous value.
• Beichman, C., Benneke, B., Knutson, H., Smith, R., Lagage, P., Dressing, C., Latham, D., Lunine, J., Birkmann, S., Ferruit, P., Giardino, G., Kempton, E., Carey, S., Krick, J., Deroo, P. D., Mandell, A., Ressler, M. E., Shporer, A., Swain, M., , Vasisht, G., et al. (1999). Observations of Transiting Exoplanets with the James Webb Space Telescope (JWST). PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC, 126(946), 1134-1173.
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  This article summarizes a workshop held on March, 2014, on the potential of the James Webb Space Telescope (JWST) to revolutionize our knowledge of the physical properties of exoplanets through transit observations. JWSTs unique combination of high sensitivity and broad wavelength coverage will enable the accurate measurement of transits with high signal-to-noise ratio (S/N). Most importantly, JWST spectroscopy will investigate planetary atmospheres to determine atomic and molecular compositions, to probe vertical and horizontal structure, and to follow dynamical evolution, i.e., exoplanet weather. JWST will sample a diverse population of planets of varying masses and densities in a wide variety of environments characterized by a range of host star masses and metallicities, orbital semi-major axes, and eccentricities. A broad program of exoplanet science could
• Brand, K., Brown, M., Dey, A., Jannuzi, B., Kochanek, C., Kenter, A., Fabricant, D., Fazio, G., Forman, W., Green, P., Jones, C., McNamara, B., Murray, S., Najita, ., Rieke, M., Shields, J., & Vikhlinin, A. (1999). The Chandra XBootes survey. III. Optical and near-infrared counterparts. ASTROPHYSICAL JOURNAL, 641(1), 140-157.
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  The XBootes Survey is a 5 ks Chandra survey of the Bootes Field of the NOAO Deep Wide-Field Survey (NDWFS). This survey is unique in that it is the largest (9.3 deg(2)) contiguous region imaged in X-ray with complementary deep optical and near-infrared (near-IR) observations. We present a catalog of the optical counterparts to the 3213 X-ray point sources detected in the XBootes survey. Using a Bayesian identification scheme, we successfully identified optical counterparts for 98% of the X-ray point sources. The optical colors suggest that the optically detected galaxies are a combination of z < 1 massive early-type galaxies and bluer star-forming galaxies whose optical AGN emission is faint or obscured, whereas the majority of the optically detected point sources are likely quasars over a large redshift range. Our large-area, X-ray-bright, optically deep survey enables us to select a large subsample of sources (773) with high X-ray-to-optical flux ratios (fx/fo > 10). These objects are likely high-redshift and/or dust-obscured AGNs. These sources have generally harder X-ray spectra than sources with 0.1 < fx/fo < 10. Of the 73 X-ray sources with no optical counterpart in the NDWFS catalog, 47 are truly optically blank down to R similar to 25.5 ( the average 50% completeness limit of the NDWFS R-band catalogs). These sources are also likely to be high-redshift and/or dust-obscured AGNs.
• Brand, K., Dey, A., Brown, M., Watson, C., Jannuzi, B., Najita, ., Kochanek, C., Shields, J., Fazio, G., Forman, W., Green, P., Jones, C., Kenter, A., McNamara, B., Murray, S., Rieke, M., & Vikhlinin, A. (1999). Tracing the nuclear accretion history of the red galaxy population. ASTROPHYSICAL JOURNAL, 626(2), 723-732.
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  We investigate the evolution of the hard X-ray luminosity of the red galaxy population using a large sample of 3316 red galaxies selected over a wide range in redshift (0.3 < z < 0.9) from a 1.4 deg(2) region in the Bootes field of the NOAO Deep Wide-Field Survey (NDWFS). The red galaxies are early-type, bulge-dominated galaxies and are selected to have the same evolution-corrected, absolute R-band magnitude distribution as a function of redshift to ensure that we are tracing the evolution in the X-ray properties of a comparable optical population. Using a stacking analysis of 5 ks Chandra/ACIS observations within this field to study the X-ray emission from these red galaxies in three redshift bins, we find that the mean X-ray luminosity increases as a function of redshift. The large mean X-ray luminosity and the hardness of the mean X-ray spectrum suggest that the X-ray emission is largely dominated by active galactic nuclei (AGNs) rather than stellar sources. The hardness ratio can be reproduced by either an absorbed (N-H approximate to 2 x 10(22) cm(-2)) Gamma = 1.7 power-law source, consistent with that of a population of moderately obscured Seyfert-like AGNs, or an unabsorbed Gamma = 0: 7 source, suggesting a radiatively inefficient accretion flow ( e. g., an advection-dominated accretion flow). We also find that the emission from this sample of red galaxies constitutes at least 5% of the hard X-ray background. These results suggest a global decline in the mean AGN activity of normal early-type galaxies from z similar to 1 to the present, which indicates that we are witnessing the tailing off of the accretion activity onto supermassive black holes in early-type galaxies since the quasar epoch.
• Dinshaw, N., Evans, A. S., Epps, H., Scoville, N. Z., & Rieke, M. (1999). NICMOS observations of interaction-triggered star formation in the luminous infrared galaxy NGC 6090. Astrophysical Journal Letters, 525(2 PART 1), 702-708.
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  Abstract: High-resolution 1.1, 1.6, and 2.2 μm imaging of the luminous infrared galaxy NGC 6090 obtained with NICMOS on the Hubble Space Telescope is presented. These new observations are centered on the two nuclei of the merger and reveal the spiral structure of the eastern galaxy and the amorphous nature of the western galaxy. The nuclear separation of 3.2 kpc (H0 = 75 km s-1 Mpc-1) indicates that NGC 6090 is at an intermediate stage of merging. Bright knots/clusters are also visible in the region overlapping the merging galaxies ; four of these knots appear bluer than the underlying galaxies and have colors consistent with young (
• Evans, A. S., Scoville, N. Z., Dinshaw, N., Armus, L., Soifer, B. T., Neugebauer, G., & Rieke, M. (1999). Hubble space telescope nicmos observations of rest-frame optical continuum and Hα + [N I] emission in FSC 10214+4724. Astrophysical Journal Letters, 518(1 PART 1), 145-152.
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  Abstract: High-resolution 1.10, 2.05, 2.12, and 2.15 μm imaging of the gravitationally lensed system FSC 10214+4724 are presented. These data extend Bubble Space Telescope (HST) observations of the lens system to redder wavelengths, thus providing the highest resolution images to date of the rest-frame optical and narrow-line (i.e., Hα + [N II]) regions of the background quasar. The length of the arc in the wide-band continuum images increases with increasing wavelength, and the Hα + [N H] emission has a length in between that of the 1.10 and 2.05 μnd emission. The structure of the arc changes from having an eastern and western peak at 1.10 μm to having a single peak in the center at 2.05 μm. The changing structure and length of the arc can be understood in terms of a model in which the background quasar consists of a region of scattered active galactic nucleus (AGN) light that dominates at 1.10 μm (rest frame 3300 Å), surrounded by a more extended narrow-line region. An even more extended red stellar population would thus contribute light at 2.05 μm (rest frame 6200 Å). In addition, the Hα + [N II] emission has structural features similar to the 1.10 μm emission normalized by the (predominantly stellar) 2.05 μm emission, possibly confirming that the 1.10 μm emission is a superposition of the sources associated with the line emission (AGNs/massive stars) and the red stellar component that dominates the 2.05 μm emission. The counterimage of the lensed quasar is detected in the 1.10 and 2.05 μm images, and the rest frame 3300 and 6200 Å magnifications of the lensed quasar are calculated to be 50 ± 11 and 25 ± 6, respectively, which translates into a rest-frame optical luminosity for the quasar of ∼6 × 109 L⊙. These magnification values are lower than the previously measured magnification of ∼100 at rest frame 2400 Å. If the dust in the primary lensing galaxy is not affecting the measurement of the counterimage flux at 2400 and 3300 Å, the magnification of the quasar appears to decrease with increasing wavelength. Flux measurements of the primary lensing galaxy fit the spectral energy distribution of an unevolving elliptical galaxy at a redshift of 0.9, consistent with previous determinations of the redshift.
• Huang, J., Barmby, P., Fazio, G., Willner, S., Wilson, G., Rigopoulou, D., Alonso-Herrero, A., Dole, H., Egami, E., Le Floc'h, E., Papovich, C., Perez-Gonzalez, P., Rigby, J., Engelbracht, C., Gordon, K., Hines, D., Rieke, M., Rieke, G., Meisenheimer, K., & Miyazaki, S. (1999). Infrared array camera (IRAC) imaging of the Lockman Hole. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 154(1), 44-47.
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  IRAC imaging of a 4.7 x 4.'7 area in the Lockman Hole detected over 400 galaxies in the IRAC 3.6 and 4.5 mum bands, 120 in the 5.8 mum band, and 80 in the 8.0 mum band in 30 minutes of observing time. Color-color diagrams suggest that about half of these galaxies are at redshifts 0.6 < z < 1.3 with about a quarter at higher redshifts ( z > 1.3). We also detect IRAC counterparts for six of the seven SCUBA sources and all nine XMM-Newton sources in this area. The detection of the counterparts of the SCUBA sources and galaxies at z > 1: 3 demonstrates the ability of IRAC to probe the universe at very high redshifts.
• Ivanov, V. D., Alonso-Herrero, A., Rieke, M. J., & McCarthy, D. (1999). An infrared determination of the reddening and distance to dwingeloo 1. Astronomical Journal, 118(2), 826-830.
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  Abstract: We present the first published infrared observations of the nearby, highly obscured galaxy Dwingeloo 1 (Dw 1), including deep H-band imaging covering a total of 4′.9 × 4′.9, together with J and Ks imaging of the central 2′.5 × 2′.5. We used the small dispersion of the intrinsic infrared colors of spiral galaxies to determine an infrared H-band extinction of AH = 0.47 ± 0.11 mag toward Dw 1. Using infrared colors reduces the uncertainties in the reddening and distance by a factor of 3. The H-band magnitude, corrected for extinction, and the infrared Tully-Fisher relation are then used to estimate a distance modulus of (m - M)0 = 28.62 ± 0.27 and, thus, a distance of d = 5.3+0.7-0.6 Mpc, which places Dw 1 at the far end of the IC 342/Maffei 1-2 group of galaxies. Our result is largely independent of the nature of the reddening law because we estimated both the reddening and the distance at the same wavelength range.
• McIntosh, D. H., Rieke, M. J., Rix, H. -., Foltz, C. B., & Weymann, R. J. (1999). A statistical study of rest-frame optical emission properties in luminous quasars at 2.0 ≤ z ≤ 2.5. Astrophysical Journal Letters, 514(1 PART 1), 40-67.
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  Abstract: We have obtained H-band spectra of 32 luminous quasars at 2.0 ≤ z < 2.5 with the Multiple Mirror Telescope. The sample contains 15 radio-loud quasars (RLQs) and 17 radio-quiet quasars (RQQs). We have measured emission line properties from the rest-frame wavelength range of approximately λλ4500-5500 by fitting the data with composite model spectra. Our analysis includes comparison of RLQs versus RQQs, as well as comparison between the broad-absorption-line quasar (BALQSO) and non-broad-absorption-line quasar (nonBALQSO) subsets of the RQQ sample. In addition, we calculated the complete correlation matrix of the measured properties. We combined our high-redshift sample with the sample of 87 low-redshift quasars from Boroson & Green to determine the luminosity and redshift dependences of the measured emission properties. Our main results are the following: (1) The RLQ sample has significantly (at more than 97.2% confidence) stronger [O III] λ5007 emission than the RQQ sample, which favors scenarios including two populations of quasars that are intrinsically different. We are not aware of a unified model based upon orientation that can explain enhanced [O III] emission with increased radio power. (2) The RLQ sample has significantly narrower (in full width at half-maximum) Hβ broad component line profiles than the RQQ sample. (3) At the sensitivity of our observations, there are no statistically significant (> 95%) differences between the rest-frame optical emission line properties of the BALQSO and nonBALQSO subsamples. This result is consistent with the view that all RQQs have broad-absorption-line clouds with a small (∼ 10%-20%) covering factor and that differences between the two types are merely a function of viewing angle and covering factor. (4) The significant [O III]-Fe II anticorrelation found in lower redshift quasars holds at this higher redshift range; however, it is the [O III] emission in this relationship that appears to be related to the physical distinction between the RLQ and RQQ classes instead of the Fe II emission that distinguishes at low redshifts and luminosities. We also find significant relationships between (i) the [O III] emission strength and the radio power, the broad-emission-line widths, and the X-ray continuum shape; (ii) positive correlations relating the strength of optical Fe II emission to broad-emission-line widths and the shape of the ionizing continuum; and (iii) similar relations for the strength and width of the Hβ emission. Many of these correlations have been found in lower redshift and luminosity studies. (5) We report a previously unknown luminosity and/or redshift dependence of the narrow-line region velocity width over the range O < z < 2.5, such that emission line widths increase with increasing luminosity. We confirm a similar dependence for the Hβ broad-line width. These findings may be evidence for a physical connection between the continuum and line-emitting regions at similar energies. Furthermore, we find a "Baldwin Effect" for the [O III] λ5007 line in the RQQ-only sample over this same range in redshifts.
• McIntosh, D. H., Rix, H. -., Rieke, M. J., & Foltz, C. B. (1999). Redshifted and blueshifted broad lines in luminous quasars. Astrophysical Journal Letters, 517(2 PART 2), L73-L76.
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  Abstract: We have observed a sample of 22 luminous quasars, in the range 2.0 ≲ z ≲ 2.5, at 1.6 μm with the near-infrared (NIR) spectrograph FSPEC on the Multiple Mirror Telescope. Our sample contains 13 radio-loud and nine radio-quiet objects. We have measured the systemic redshifts zsys directly from the strong [O III] λ5007 line emitted from the narrow-line region. From the same spectra, we have found that the nonresonance broad Hβ lines have a systematic mean redward shift of 520 ± 80 km s-1 with respect to systemic. Such a shift was not found in our identical analysis of the low-redshift sample of Boroson & Green. The amplitude of this redshift is comparable to half the expected gravitational redshift and transverse Doppler effects and is consistent with a correlation between redshift differences and quasar luminosity. From data in the literature, we confirm that the high-ionization rest-frame ultraviolet broad lines are blueshifted ∼550-1050 km s-1 from systemic and that these velocity shifts systematically increase with ionization potential. Our results allow us to quantify the known bias in estimating the ionizing flux from the intergalactic medium J1GMv via the proximity effect. Using redshift measurements commonly determined from strong broad-line species, like Lyα or C IV λ1549, results in an overestimation of J1GMv by factors of ∼1.9-2.3. Similarly, corresponding lower limits on the density of baryons Ωb, will be overestimated by factors of ∼1.4-1.5. However, the low-ionization Mg II λ2798 broad line is within ∼50 km s-1 of systemic and thus would be the line of choice for determining the true redshift of 1.0 < z < 2.2 quasars without NIR spectroscopy and z > 3.1 objects using NIR spectroscopy.
• Papovich, C., Rudnick, G., Rigby, J. R., Willmer, C. N., Smith, J. -., Finkelstein, S. L., Egami, E., & Rieke, M. (1999). PASCHEN-alpha EMISSION IN THE GRAVITATIONALLY LENSED GALAXY SMM J163554.2+661225. ASTROPHYSICAL JOURNAL, 704(2), 1506-1518.
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  We report the detection of the Pa alpha emission line in the z = 2.515 galaxy SMM J163554.2+661225 using Spitzer spectroscopy. SMM J163554.2+661225 is a submillimeter-selected infrared-luminous galaxy maintaining a high star formation rate (SFR), with no evidence of an active galactic nucleus from optical or infrared spectroscopy, nor X-ray emission. This galaxy is lensed gravitationally by the cluster Abell 2218, making it accessible to Spitzer spectroscopy. We measure a line luminosity, L(Pa alpha) = (2.05 +/- 0.33) x 10(42) erg s(-1), corrected for gravitational lensing. Comparing the H alpha and Pa alpha luminosities, we derive a nebular extinction, A(V) = 3.6 +/- 0.4 mag. The dust-corrected luminosity, L(Pa alpha) = (2.57 +/- 0.43) x 10(42) erg s(-1), corresponds to an ionization rate, Q(0) = (1.6 +/- 0.3) x 10(55) gamma s(-1). The instantaneous SFR is psi = 171 +/- 28M(circle dot) yr(-1), assuming a Salpeter-like initial mass function from 0.1 to 100 M(circle dot) yr(-1). The total IR luminosity derived using 70, 450, and 850 mu m data is L(IR) = (5-10) x 10(11) L(circle dot), corrected for gravitational lensing. This corresponds to psi = 90-180 M(circle dot) yr(-1), where the upper range is consistent with that derived from the Pa alpha luminosity. While the L(8 mu m)/L(Pa alpha) ratio is consistent with the extrapolated relation observed in local galaxies and star-forming regions, the rest-frame 24 mu m luminosity is significantly lower with respect to local galaxies of comparable Pa alpha luminosity. Thus, SMM J163554.2+661225 arguably lacks a warmer dust component (T(D) similar to 70 K), which is associated with deeply embedded star formation, and which contrasts with local galaxies with comparable SFRs. Rather, the starburst in SMM J163554.2+ 661225 is consistent with star-forming local galaxies with intrinsic luminosities, L(IR) approximate to 10(10) L(circle dot), but "scaled up" by a factor of similar to 10-100.
• Whitmore, B. C., Chandar, R., Schweizer, F., Rothberg, B., Leitherer, C., Rieke, M., Rieke, G., Blair, W. P., Mengel, S., & Alonso-Herrero, A. (1999). THE ANTENNAE GALAXIES (NGC 4038/4039) REVISITED: ADVANCED CAMERA FOR SURVEYS AND NICMOS OBSERVATIONS OF A PROTOTYPICAL MERGER. ASTRONOMICAL JOURNAL, 140(1), 75-109.
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  The Advanced Camera for Surveys and the Near Infrared Camera and Multi-Object Spectrometer (NICMOS) have been used to obtain new Hubble Space Telescope images of NGC 4038/4039 ("The Antennae"). These new observations allow us to better differentiate compact star clusters from individual stars, based on both size and color. We use this ability to extend the cluster luminosity function (LF) by approximately 2 mag over our previous WFPC2 results, and find that it continues as a single power law, dN/dL proportional to L(alpha) with alpha = -2.13 +/- 0.07, down to the observational limit of M(V) approximate to -7. Similarly, the mass function (MF) is a single power law dN/dM proportional to M beta with beta = -2.10 +/- 0.20 for clusters with ages 3 mag.
• Evans, A., Becklin, E., Scoville, N., Neugebauer, G., Soifer, B., Matthews, K., Ressler, M., Werner, M., & Rieke, M. (1998). The compact nucleus of the deep silicate absorption galaxy NGC 4418. ASTRONOMICAL JOURNAL, 125(5), 2341-2347.
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  High-resolution Hubble Space Telescope (HST) near-infrared and Keck mid-infrared images of the heavily extinguished infrared-luminous galaxy NGC 4418 are presented. These data make it possible to observe the imbedded near-infrared structure on scales of 10-20 pc and to constrain the size of the mid-infrared-emitting region. The 1.1-2.2 mum data of NGC 4418 show no clear evidence of nuclear star clusters or of a reddened active galactic nucleus. Instead, the nucleus of the galaxy consists of a similar to100-200 pc linear structure with fainter structures extending radially outward. The near-infrared colors of the linear feature are consistent with a 10-300 Myr starburst suffering moderate levels (a few magnitudes) of visual extinction. At 7.9-24.5 mum NGC 4418 has estimated size upper limits in the range of 30-80 pc. These dimensions are consistent with the highest-resolution radio observations obtained to date of NGC 4418, as well as the size of 50-70 pc expected for a blackbody with a temperature derived from the 25, 60, and 100 mum flux densities of the galaxy. Further, a spectral energy distribution constructed from the multiwavelength mid-infrared observations shows the strong silicate absorption feature at 10 mum, consistent with previous mid-infrared observations of NGC 4418. An infrared surface brightness of similar to2.1 x 10(13) L-. kpc(-2) is derived for NGC 4418. Such a value, though consistent with the surface brightness of warm ultraluminous infrared galaxies [L-IR(8-1000 mum) greater than or equal to 10(12) L-.], such as IRAS 05189-2524 and IRAS 08572+3915, is not large enough to distinguish NGC 4418 as a galaxy powered by an active galactic nucleus, as opposed to a lower surface brightness starburst.
• Evans, A., Scoville, N., Dinshaw, N., Armus, L., Soifer, B., Neugebauer, G., & Rieke, M. (1998). Hubble Space Telescope NICMOS observations of rest-frame optical continuum and H alpha+[N I] emission in FSC 10214+4724. ASTROPHYSICAL JOURNAL, 518(1), 145-152.
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  High-resolution 1.10, 2.05, 2.12, and 2.15 mu m imaging of the gravitationally lensed system FSC 10214+4724 are presented. These data extend Hubble Space Telescope (HST) observations of the lens system to redder wavelengths, thus providing the highest resolution images to date of the rest-frame optical and narrow-line (i.e., H alpha + [N II]) regions of the background quasar. The length of the are in the wide-band continuum images increases with increasing wavelength, and the H alpha + [N II] emission has a length in between that of the 1.10 and 2.05 mu m emission. The structure of the are changes from having an eastern and western peak at 1.10 mu m to having a single peak in the center at 2.05 mu m. The changing structure and length of the are can be understood in terms of a model in which the background quasar consists of a region of scattered active galactic nucleus (AGN) light that dominates at 1.10 mu m (rest frame 3300 Angstrom), surrounded by a more extended narrow-line region. An even more extended red stellar population would thus contribute light at 2.05 mu m (rest frame 6200 Angstrom). In addition, the H alpha + [N II] emission has structural features similar to the 1.10 mu m emission normalized by the (predominantly stellar) 2.05 mu m emission, possibly confirming that the 1.10 mu m emission is a superposition of the sources associated with the line emission (AGNs/massive stars) and the red stellar component that dominates the 2.05 mu m emission. The counterimage of the lensed quasar is detected in the 1.10 and 2.05 mu m images, and the rest frame 3300 and 6200 Angstrom magnifications of the lensed quasar are calculated to be 50 +/- 11 and 25 +/- 6, respectively, which translates into a rest-frame optical luminosity for the quasar of similar to 6 x 10(9) L.. These magnification values are lower than the previously measured magnification of similar to 100 at rest frame 2400 Angstrom. If the dust in the primary lensing galaxy is not affecting the measurement of the counterimage flux at 2400 and 3300 Angstrom, the magnification of the quasar appears to decrease with increasing wavelength. Flux measurements of the primary lensing galaxy fit the spectral energy distribution of an unevolving elliptical galaxy at a redshift of 0.9, consistent with previous determinations of the redshift.
• Grauer, A. D., & Rieke, M. J. (1998). Infrared observations of galaxies in the local universe. I. The survey and some representative results. Astrophysical Journal, Supplement Series, 116(1), 29-45.
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  Abstract: This paper introduces a continuing survey of galaxies in the local universe. Consistent deep images are being acquired for a representative sample of 321 galaxies in the Uppsala General Catalogue down to 21.7 mag arcsec-2 at Ks (2.16 μm) and 22.4 mag arcsec-2 at J (1.25 μm) using a NICMOS camera with a 3′.8 × 3′.8 field of view attached to the 61 inch (1.5 m) telescope on Mount Bigelow. We provide some examples of the results being obtained by employing 64 deep images of a subset of 44 galaxies. Bulge-to-disk ratios are tabulated for 30 galaxies. The brightness of the central region of 44 galaxies declines approximately 5 mag from Hubble type S0 to Sm. An exponential vertical scale height at Ks is found to be 500 pc for the disk of UGC 5173. Arm amplitudes of four nearly face-on spiral galaxies are found to range between 11% and 88% compared to the interarm region. There is some evidence that the arm amplitude is larger at Ks than it is at J. Color gradients are measured for 15 galaxies with only one showing a significant nonzero result. A measurement of galactic symmetry applied to 64 deep images reveals an average asymmetry of 7.6% (σ = 4.6%) for these galaxies.
• McLeod, B. A., Bernstein, G. M., Rieke, M. J., & Weedman, D. W. (1998). The gravitational lens MG 0414+0534: A link between red galaxies and dust. Astronomical Journal, 115(4), 1377-1382.
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  Abstract: We present near-IR observations of the red gravitational lens system MG 0414+0534. Our images are of sufficient quality to allow photometry of all four QSO images and the lens galaxy. The observations show that the K-band brightnesses of the components are more similar to the radio brightnesses than to the optical and thus support the notion that the system is highly reddened. The differing brightnesses at visible wavelengths are interpreted as variable amounts of extinction in the lens galaxy. The lens galaxy is detected in the K band and is as red as any other known galaxy of comparable apparent magnitude. An estimate of the redshift of the lens galaxy of 0.45 < z < 0.6 is determined from the Faber-Jackson relation and photometric considerations. By extension, we argue that other very red field galaxies may contain large amounts of dust. K-band spectra of the individual components show no difference in the Hα equivalent widths among the components. This is evidence against significant microlensing.
• Persson, S. E., Murphy, D. C., Krzeminski, W., Roth, M., & Rieke, M. J. (1998). A new system of faint near-infrared standard stars. Astronomical Journal, 116(5), 2475-2488.
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  Abstract: A new grid of 65 faint near-infrared standard stars is presented. They are spread around the sky, lie between 10th and 12th magnitude at K, and are measured in most cases to precisions better than 0.001 mag in the J, H, K, and Ks bands; the latter is a medium-band modified K. A secondary list of red stars suitable for determining color transformations between photometric systems is also presented.
• Ponder, J. M., Burstein, D., O'Connell, R. W., Rose, J. A., Frogel, J. A., Wu, C., Crenshaw, D. M., Rieke, M. J., & Tripicco, M. (1998). Integrated ultraviolet spectra and line indices of M31 globular clusters and the cores of elliptical galaxies. Astronomical Journal, 116(5), 2297-2314.
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  Abstract: We present observations of the integrated light of four M31 globular clusters (MIV, MII, K280, and K58) and of the cores of six elliptical galaxies (NGC 3605, 3608, 5018, 5831, 6127, and 7619) made with the Faint Object Spectrograph on the Hubble Space Telescope. The spectra cover the range 2200-4800 Å at a resolution of 8 Å with signal-to-noise ratio of more than 20 and flux accuracy of ∼ 5%. To these data we add from the literature IUE observations of the dwarf elliptical galaxy M32, Galactic globular clusters, and Galactic stars. The stellar populations in these systems are analyzed with the aid of mid-UV and near-UV colors and absorption line strengths. Included in the measured indices is the key NH feature at 3360 Å. We compare these line index measures with the 2600 - 3000 colors of these stars and stellar populations. We find that the M31 globular clusters, Galactic globular clusters/Galactic stars, and elliptical galaxies represent three distinct stellar populations, based on their behavior in color-line strength correlations involving Mg II, NH, CN, and several UV metallic blends. In particular, the M31 globular cluster MIV, as metal-poor as the Galactic globular M92, shows a strong NH 3360 Å feature. Other line indices, including the 3096 Å blend that is dominated by lines of Mg I and Al I, show intrinsic differences as well. We also find that the broadband line indices often employed to measure stellar population differences in faint objects, such as the 4000 Å and the Mg 2800 breaks, are disappointingly insensitive to these stellar population differences. We find that the hot (T > 20,000 K) stellar component responsible for the "UV upturn" at shorter wavelengths can have an important influence on the mid-UV spectral range (2400-3200 Å) as well. The hot component can contribute over 50% of the flux at 2600 Å in some cases and affects both continuum colors and line strengths. Mid-UV spectra of galaxies must be corrected for this effect before they can be used as age and abundance diagnostics. Of the three stellar populations studied here, M31 globular clusters and elliptical galaxies are more similar to each other than either is to the Galactic stellar populations defined by globular clusters and nearby stars. Similarities between the abundance-pattern differences currently identified among these stellar populations and those among globular cluster stars; (N, Al enhancements) present a curious coincidence that deserves future investigation.
• Thompson, R. I., Eisenstein, D., Fan, X., Rieke, M., & Kennicutt, R. C. (1998). Evidence for a z < 8 origin of the source-subtracted near-infrared background. ASTROPHYSICAL JOURNAL, 666(2), 658-662.
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  This paper extends our previous fluctuation analysis of the near-infrared background at 1.6 mu m tothe1.1 mu m( F110W) image of the Hubble Ultra Deep Field. When all detectable sources are removed, the ratio of fluctuation power in the two images is consistent with the ratio expected for faint, z < 8, sources, and is inconsistent with the expected ratio for galaxies with z > 8. We also use numerically redshifted model galaxy spectral energy distributions for 50 and 10 Myr old galaxies to predict the expected fluctuation power at 3.6 and 4.5 mu m to compare with recent Spitzer observations. The predicted fluctuation power for galaxies at z 0 12 matches the observed Spitzer fluctuation power, while the predicted power for z > 13 galaxies is much higher than the observed values. As was found in the 1.6 mu m ( F160W) analysis, the fluctuation power in the source- subtracted F110Wimage is 2 orders of magnitude below the power in the image with all sources present. This leads to the conclusion that the 0.8 - 1.8 mu m near- infrared background is due to resolved galaxies in the redshift range z < 8, with the majority of power in the redshift range of 0.5 - 1.5.
• Werner, M., Reach, W., Rieke, M., Harwit, M., & Hauser, M. (1998). Studies of the cosmic infrared background with the space infrared telescope facility (SIRTF). EXTRAGALACTIC INFRARED BACKGROUND AND ITS COSMOLOGICAL IMPLICATIONS, 439-453.
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  IRAS, COBE, and ISO have demonstrated the unique importance of a cryogenic infrared telescope in space for studying diffuse infrared backgrounds and for teasing out the individual point sources which contribute to them. This importance results from the extremely high infrared sensitivity of such telescopes, particularly to diffuse radiation. The next cryogenic infrared telescope will be NASA's Space Infrared Telescope Facility (SIRTF), which is currently in the final stages of construction leading to launch in 2002. SIRTF will be the first infrared space observatory to make extensive use - both for imaging and spectroscopy of large format infrared detector arrays. The sensitivity and spatial and spectral coverage of SIRTF's array-based instruments endow SIRTF with great power for the study of the cosmic infrared background (CIRB) and related scientific issues. This paper reviews the SIRTF mission design and measurement functionality and describes SIRTF's potential studies of the CIRB, drawing examples from the programs planned by the SIRTF Guaranteed Time Observers (GTO's). We also summarize the opportunities for community participation in SIRTF.
• Werner, M., Roellig, T., Low, F., Rieke, G., Rieke, M., Hoffmann, W., Young, E., Houck, ., Brandl, B., Fazio, G., Hora, J., Gehrz, R., Helou, G., Soifer, B., Stauffer, J., Keene, J., Eisenhardt, P., Gallagher, D., Gautier, T., , Irace, W., et al. (1998). The Spitzer Space Telescope mission. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 154(1), 1-9.
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  The Spitzer Space Telescope, NASA's Great Observatory for infrared astronomy, was launched 2003 August 25 and is returning excellent scientific data from its Earth-trailing solar orbit. Spitzer combines the intrinsic sensitivity achievable with a cryogenic telescope in space with the great imaging and spectroscopic power of modern detector arrays to provide the user community with huge gains in capability for exploration of the cosmos in the infrared. The observatory systems are largely performing as expected, and the projected cryogenic lifetime is in excess of 5 years. This paper summarizes the on-orbit scientific, technical, and operational performance of Spitzer. Subsequent papers in this special issue describe the Spitzer instruments in detail and highlight many of the exciting scientific results obtained during the first 6 months of the Spitzer mission.
• Friedli, D., Wozniak, H., Rieke, M., Martinet, L., & Bratschi, P. (1996). Disc galaxies with multiple triaxial structures. * II. JHK surface photometry and numerical simulations. Astronomy and Astrophysics Supplement Series, 118(3), 461-479.
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  Abstract: We present detailed JHK surface photometry with ellipse fits of 13 galaxies selected from previous optical observations as likely candidates for having a secondary bar or a triaxial bulge within the primary bar. We have found 7 double-barred galaxies, 3 double-barred galaxies with an additional intermediate structure with twisted isophotes, and 3 galaxies with a bar and central twisted isophotes. A global analysis of the structural parameter characteristics in the I- and K-bands is presented. Various numerical models of galaxies with bars within bars are also analysed using the ellipse fitting technique and compared to the observations. A thorough review of the possible hypotheses able to explain this phenomenon is given with emphasis on the most likely ones.
• Hanson, M. M., Conti, P. S., & Rieke, M. J. (1996). A spectral atlas of hot, luminous stars at 2 microns. Astrophysical Journal, Supplement Series, 107(1), 281-311.
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  Abstract: We present 2 μm (K band) spectra of 180 well-studied, optically visible, luminous stars. Most of the stars are of OB spectral type, but we have also included a number of Oe and Be stars, OBN and OBC stars, cool hypergiant stars, and high-mass X-ray binary stars. Our aim in studying normal OB stars is to develop an empirical relationship between 2 μm spectral features of these massive stars and their stellar temperature and luminosity. We find the system of lines between 2.0 and 2.2 μm is particularly good for differentiating the early- and mid-O type stars. In the late-O and early-B stars, differentiation becomes more difficult, as the features show only moderate changes. We have developed a spectral classification system for the K band to be used to estimate effective temperatures of O and early-B stars. We demonstrate that K-band spectroscopy is superior in estimating the temperature of hot, luminous stars than the traditional methods of using infrared or even optical photometric colors alone. The only requirements are that adequate resolution (R > 1000) and signal-to-noise (S/N ∼ 70) be achieved. With our classification system, stars behind large amounts of visible extinction, such as in young, heavily reddened H II regions throughout our Galaxy, may be identified and studied for the first time through 2 μm spectroscopy. Emission lines are commonly seen in the K-band spectra of supergiant stars, however, the OBN super- giants, which have a higher ratio of some processed materials at their surface, may be more likely to show line emission, especially the He I singlet transition at 2.058 μm. This has led us to propose an evolutionary scenario for some of the Galactic center He I emission-line stars, which evokes rotational mixing (Maeder 1987; Langer 1992) to explain both the strong line emission and high luminosity of these mysterious sources. We have compared our spectroscopic database with the most recent stellar atmosphere models. We are encouraged by the good match between the model line profiles at 2 μm of Schaerer et al. (1996b) and those observed in OB stars. Finally, we include a thorough discussion of the observational and reduction methods employed to obtain the spectra shown in this atlas for the benefit of those wishing to obtain similar, classification-quality, near-infrared spectra.
• MINNITI, D., OLSZEWSKI, E., & RIEKE, M. (1996). IR COLOR-MAGNITUDE DIAGRAMS OF 20 GALACTIC GLOBULAR-CLUSTERS AND BULGE FIELDS. ASTRONOMICAL JOURNAL, 110(4), 1686-1698.
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  We present K vs J-K color-magnitude diagrams for 20 Galactic globular clusters projected onto the bulge. These color-magnitude diagrams reach similar to 2 mag below the horizontal branch at the distance of the bulge. Some of these clusters (HP 1, ESO45-SC11, NGC 6284, NGC 6401, NGC 6642, Pal 6, and UKS 1) have no previously published CMDs. The candidate clusters TJ 5, TJ 15, and TJ 16 are not detected in our deep IR images, it is likely that these are not real globulars. We compare the position of the giant branches with respect to the standard globular clusters M92, M4, and M22, and put all the dusters on a uniform scale using the best available reddenings and metallicities. Reddenings are derived for the less studied clusters, based on the position of the red giant branches in the near-IR color-magnitude diagrams. A comparative study is made between the clusters and the bulge stellar population, using photometry in selected fields located a few arcminutes away from the cluster cores. Our major conclusion is that the bulge giants have the same near-IR colors in the mean as the most metal-rich globulars, From existing models acid observations, we adopt the calibration law [Fe/H]=5.0(J-K)-5.60 based on the color of the red giant branch at K-0=-5.5, valid between [Fe/H]=-2.3 and 0.5. On the basis of differential colors of the cluster giant branch against the field giant branch, we find a metallicity gradient in the bulge fields that supports previously published results from optical photometry. (C) 1995 American Astronomical Society.
• ELSTON, R., BECHTOLD, J., LOWENTHAL, J., & RIEKE, M. (1995). EMISSION FROM THE Z = 2 DAMPED LY-ALPHA ABSORBER TOWARD Q1215+333. ASTROPHYSICAL JOURNAL, 373(2), L39-L42.
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  We have detected narrow emission lines at 1.118-mu-m and 1.456-mu-m in the spectrum of the z = 2.606 quasar Q1215 + 333, corresponding to [O II] lambda-3727 and H-beta at z = 1.9984, the redshift of a damped Ly-alpha absorber toward this quasar. The intensity of the H-beta line is 7.6 +/- 2 x 10(-16) ergs cm-2 s-1, which corresponds to a line luminosity of 5 x 10(42) ergs s-1 h100(-2) (q0 = 0.5). If we assume that the photoionization producing the emission is due purely to massive star formation with a Salpeter initial mass function, we find a total star formation rate of 100 M. yr-1 h100(-2). Given the uncertainty in the initial mass function and cosmological parameters, this star formation rate is very uncertain. However, the star formation rate is well above those inferred from Ly-alpha emission-line searches of similar systems, implying effective destruction of Ly-alpha photons. The intensity of the [O II] lambda-3727 line is 1.6 +/- 0.3 x 10(-15) ergs cm-2 s-1. The ratio [O II]/H-beta-almost-equal-to 2 and the weakness of the ratio [O II] lambda-5007/H-beta < 0.5 is typical of star formation regions with gas at nearly solar metallicity.
• Kuhn, O., Bechtold, J., Cutri, R., Elvis, M., & Rieke, M. (1995). The spectral energy distribution of the z = 3 quasar: HS 1946+7658. Astrophysical Journal Letters, 438(2), 643-649.
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  Abstract: For the bright z = 3.02 radio-quiet quasar, HS 1946+7658, we have obtained radio to X-ray data within the past year: 5 GHz and 1415 MHz data from the VLA; IR photometry at J, H, K, L′ (3.4 μm) and N; IR spectroscopy; UBVRI photometry; optical spectrophotometry and high-resolution spectra; and an X-ray spectrum from the ROSAT PSPC. The spectral energy distribution (SED) constructed from these data is compared to the mean SED for a set of low-redshift quasars, and while.they appear generally similar, there are several differences. In relation to the low-redshift mean, the SED of HS 1946+7658 shows (1) only an upper limit at 10 μm (a rest wavelength of 2.5 μm), indicating that HS 1946+7658 does not have a strong near-IR excess such as hot dust would produce; (2) relatively weak Fe II and Balmer continuum emission at ∼3000 Å; and (3) a steeper turndown shortward of Lyα, even after correction for the Lyα forest absorption lines.
• McLeod, B. A., & Rieke, M. J. (1995). The effects of starbursts and low surface brightness galaxies on faint galaxy models. Astrophysical Journal Letters, 454(2), 611-622.
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  Abstract: We present models predicting the magnitude, redshift, and color distributions of field galaxies. We explore whether a fading starburst scenario can account for the observations of faint blue galaxies. We marginally rule out a starburst scenario with a local initial mass function (IMF) because the models predict too many nearby faint galaxies that are not observed. A burst model with a truncated IMF reproduces the counts and redshift distributions well but produces too blue a population. We show that surface brightness selection has a significant effect on the distributions. In particular, adding a population of low-surface brightness galaxies, known to exist locally, can explain the counts for BJ < 23. They do not, however, account for the steepness of the counts at fainter magnitudes. Finally, we show that the colors of galaxies in a K-band-selected sample are too blue to be consistent with a constant star formation rate, passive-evolution model.
• Mcleod, B. A., Bernstein, G. M., Rieke, M. J., Tollestrup, E. V., & Fazio, G. G. (1995). K-band galaxy counts. Astrophysical Journal, Supplement Series, 96(1), 117-121.
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  Abstract: We present new counts of field galaxies from more than 20 arcmin2 to a limiting magnitude of K = 20 and from 2 arcmin2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples. galaxies: general - infrared: galaxies.
• Minniti, D., Olszewski, E. W., & Rieke, M. (1995). IR color-magnitude diagrams of 20 galactic globular clusters and bulge fields. Astronomical Journal, 110(4), 1686-1698.
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  Abstract: We present K vs J-K color-magnitude diagrams for 20 Galactic globular clusters projected onto the bulge. These color-magnitude diagrams reach ∼2 mag below the horizontal branch at the distance of the bulge. Some of these clusters (HP 1, ESO45-SC11, NGC 6284, NGC 6401, NGC 6642, Pal 6, and UKS 1) have no previously published CMDs. The candidate clusters TJ 5, TJ 15, and TJ 16 are not detected in our deep IR images, it is likely that these are not real globulars. We compare the position of the giant branches with respect to the standard globular clusters M92, M4, and M22, and put all the clusters on a uniform scale using the best available reddenings and metallicities. Reddenings are derived for the less studied clusters, based on the position of the red giant branches in the near-IR color-magnitude diagrams. A comparative study is made between the clusters and the bulge stellar population, using photometry in selected fields located a few arcminutes away from the cluster cores. Our major conclusion is that the bulge giants have the same near-IR colors in the mean as the most metal-rich globulars. From existing models and observations, we adopt the calibration law [Fe/H]=5.0(J-K)-5.60 based on the color of the red giant branch at K0=-5.5, valid between [Fe/H]=-2.3 and 0.5. On the basis of differential colors of the cluster giant branch against the field giant branch, we find a metallicity gradient in the bulge fields that supports previously published results from optical photometry. © 1995 American Astronomical Society.
• Bechtold, J., Elvis, M., Fiore, F., Kuhn, O., Cutri, R. M., Mcdowell, J. C., Rieke, M., Siemiginowska, A., & Wilkes, B. J. (1994). Infrared to x-ray spectral energy distributions of high redshift quasars. Astronomical Journal, 108(2), 374-394.
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  Abstract: We have observed 14 quasars with z>2.8 with the ROSAT-PSPC, and detected 12 of them, including the z=4.11 quasar 0000-263. We present the first x-ray spectrum of a radio quiet quasar with z>3, 1946+768. Its x-ray spectrum is consistent with a power law with spectral index αE = 1.8+2.1-1.4 and no evidence for absorption in excess of the galactic column [αE=1.00+0.28-0.32 assuming NH=NH(Gal)]. A PSPC hardness ratio is used to constrain the x-ray spectral properties of the quasars for which there were less than 100 photons detected. For the radio quiet quasars, 〈αE〉≈1.2, if one assumes that there is no absorption in excess of the galactic column. We combine the x-ray data with new ground based optical and near-IR spectrophotometry obtained at the Steward 2.3 m and Multiple Mirror Telescope, and data from the literature. The spectral energy distributions are compared to those of low redshift objects. For the radio quiet quasars with z>2.5, the mean 〈αox〉∼1.8. This is larger than the mean for quasars with z
• Bechtold, J., Elvis, M., Fiore, F., Kuhn, O., Cutri, R. M., Mcdowell, J. C., Rieke, M., Siemiginowska, A., & Wilkes, B. J. (1994). X-ray spectral evolution of high redshift quasars. Astronomical Journal, 108(3), 759-765.
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  Abstract: At z≈3, the x-ray spectra of radio-loud and radio-quiet quasars are different. High-redshift radio-quiet quasars either have large absorbing columns, NH, and steeper power law spectral indices, αE, than low redshift quasars, or no absorption and similar αE's. In contrast, the radio-loud quasars at high redshift have substantial absorption and similar αE's to low redshift quasars. Implications for the interpretation of the evolution of the luminosity function of quasars are discussed. If the absorption arises outside the central engine for both radio-loud and radio-quiet quasars, then radio-quiet quasars differ from the radio-loud quasars in that their emitted power law spectrum has evolved with redshift. We argue that this favors models where quasars are numerous and short-lived, rather than rare and long-lived.
• Eisner, J. A., Rieke, G. H., Rieke, M. J., Flaherty, K. M., Arnold, T. J., Stone, J. M., Cortes, S. R., Cox, E., Hawkins, C., Cole, A., Zajac, S., & Rudolph, A. L. (1994). Time-monitoring observations of the ro-vibrational overtone CO bands in young stars. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 434(1), 407-414.
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  We present near-infrared spectra of a sample of T Tauri, Herbig Ae/Be and FU Ori objects. Using the FSPEC instrument on the Bok 90-inch telescope, we obtained K-band spectra with a resolution of approximate to 3500. Here, we present spectra of the delta v = 2-0 and delta v = 3-1 bandheads of ro-vibrational transitions of carbon monoxide. We observed these spectra over multiple epochs spaced by a few days and approximately one month. Several of our targets show CO emission or absorption features. However, we see little evidence of variability in these features across multiple epochs. We compare our results with previous observations and discuss the physical implications of non-variable CO emission across the sampled time-scales.
• Friedli, D., Wozniak, H., Rieke, M., Martinet, L., & Bratschi, P. (1994). Disc galaxies with multiple triaxial structures .2. JHK surface photometry and numerical simulations. ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES, 118(3), 461-479.
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  We present detailed JHK surface photometry with ellipse fits of 13 galaxies selected from previous optical observations as likely candidates for having a secondary bar or a triaxial bulge within the primary bar. We have found 7 double-barred galaxies, 3 double-barred galaxies with an additional intermediate structure with twisted isophotes, and 3 galaxies with a bar and central twisted isophotes. A global analysis of the structural parameter characteristics in the I- and K-bands is presented. Various numerical models of galaxies with bars within bars are also analysed using the ellipse fitting technique and compared to the observations. A thorough review of the possible hypotheses able to explain this phenomenon is given with emphasis on the most likely ones.
• Houck, ., Soifer, B., Weedman, D., Higdon, S., Higdon, J., Herter, T., Brown, M., Dey, A., Jannuzi, B., Le Floc'h, E., Rieke, M., Armus, L., Charmandaris, ., Brandl, B., & Teplitz, H. (1994). Spectroscopic redshifts to z > 2 for optically obscured sources discovered with the Spitzer Space Telescope. ASTROPHYSICAL JOURNAL, 622(2), L105-L108.
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  We have surveyed a field covering 9.0 deg(2) within the NOAO Deep Wide-Field Survey region in Bootes with the Multiband Imaging Photometer on the Spitzer Space Telescope (SST) to a limiting 24 mu m flux density of 0.3 mJy. Thirty-one sources from this survey with F-24 mu m > 0.75 mJy that are optically very faint (R greater than or similar to 24.5 mag) have been observed with the low-resolution modules of the Infrared Spectrograph on SST (IRS). Redshifts derived primarily from strong silicate absorption features are reported here for 17 of these sources; 10 of these are optically invisible (R greater than or similar to 26 mag), with no counterpart in B-W, R, or I. The observed redshifts for 16 sources are 1.7 < z < 2.8. These represent a newly discovered population of highly obscured sources at high redshift with extreme infrared-to-optical ratios. Using IRS spectra of local galaxies as templates, we find that a majority of the sources have mid-infrared spectral shapes most similar to ultraluminous infrared galaxies powered primarily by active galactic nuclei. Assuming that the same templates also apply at longer wavelengths, bolometric luminosities exceed 10(13) L-circle dot.
• Mcleod, B., Rieke, M., & Weedman, D. (1994). Infrared observations of the dark matter lens candidate Q2345+007. Astrophysical Journal Letters, 433(2), 528-532.
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  Abstract: Deep K-band observations are presented of the double image quasar Q2345+007. This has the largest separation (7″.1) of any quasar image pair considered as gravitationally lensed, so the required lens is massive (1013 M⊙). No lens has been detected in previous deep images at visible wavelengths, and we find no lens to limiting K magnitude 20.0 in the infrared image. This constrains any lens to being much less luminous than brightest cluster galaxies, while the lens must be much more massive than such galaxies to produce the observed separation. Because spectral data indicate exceptional intrinsic similarity in the quasar image components, this pair remains as the most intriguing example of an observed configuration requiring the presence of massive, concentrated dark matter acting as a gravitational lens.
• Rieke, M. J. (1994). Using nicmos arrays to study galaxies. Experimental Astronomy, 3(1-4), 9-16.
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  Abstract: The 256×256 HgCdTe arrays developed for the NICMOS (Near-Infrared Camera and Multi-object Spectrometer) project have proven to be very capable devices for extragalactic imaging. This paper describes a sampling of extragalactic results from NICMOS arrays. A brief summary of the history of the development of these arrays, and their outstanding performance characteristics is also given. © 1994 Kluwer Academic Publishers.
• Rieke, M., Trost, T., & Grauer, R. (1994). Coupled Vlasov and two-fluid codes on GPUs. JOURNAL OF COMPUTATIONAL PHYSICS, 283, 436-452.
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  We present a way to combine Vlasov and two-fluid codes for the simulation of acollisionless plasma in large domains while keeping full information on the velocity distribution in localised areas of interest. This is made possible by solving the full Vlasov equation in one region while the remaining area is treated by a 5-moment two-fluid code. In such atreatment, the main challenge of coupling kinetic and fluid descriptions is the interchange of physically correct boundary conditions between the different plasma models. In contrast to other treatments, we do not rely on any specific form of the distribution function, e. g. a Maxwellian type. Instead, we combine an extrapolation of the distribution function and a correction of the moments based on the fluid data. Thus, throughout the simulation both codes provide the necessary boundary conditions for each other. A speed-up factor of around 10 is achieved by using GPUs for the computationally expensive solution of the Vlasov equation. Additional major savings are obtained due to the coupling where the amount of savings roughly corresponds to the fraction of the domain where the kinetic equations are solved. The coupled codes were then tested on the propagation of whistler waves and on the GEM reconnection challenge. (C) 2014 The Authors. Published by Elsevier Inc.
• Cotera, A., Whitney, B., Young, E., Wolff, M., Wood, K., Povich, M., Schneider, G., Rieke, M., & Thompson, R. (1993). High-resolution near-infrared images and models of the circumstellar disk in HH 30. ASTROPHYSICAL JOURNAL, 556(2), 958-969.
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  We present Hubble Space Telescope near-infrared camera and multiobject spectrometer observations of the reflection nebulosity associated with the T Tauri star HH 30. The images show the scattered-light pattern characteristic of a highly inclined, optically thick disk with a prominent dust lane whose width decreases with increasing wavelength. The reflected nebulosity exhibits a lateral asymmetry in the upper lobe on the opposite side to that reported in previously published Wide Field Planetary Camera 2 images. The radiation transfer model that most closely reproduces the data has a flared accretion disk with dust grains larger than standard interstellar medium grains by a factor of approximately 2.1. A single hot spot on the stellar surface provides the necessary asymmetry to fit the images and is consistent with previous modeling of the light curve and images. Photometric analysis results in an estimated extinction of A(V) greater than or similar to 80; however, since the photometry measures only scattered light rather than direct stellar flux, this a lower limit. The radiative transfer models require an extinction of A(V) = 7900.
• Kulkarni, V., Calzetti, D., Bergeron, L., Rieke, M., Axon, D., Skinner, C., Colina, L., Sparks, W., Daou, D., Gilmore, D., Holfeltz, S., MacKenty, J., Noll, K., Ritchie, C., Schneider, G., Schultz, A., Storrs, A., Suchkov, A., & Thompson, R. (1993). Unveiling the hidden nucleus of IC 5063 with NICMOS. ASTROPHYSICAL JOURNAL, 492(2), L121-+.
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  We present high-resolution near-infrared images of the Seyfert 2 galaxy IC 5063 obtained using the Neat-Infrared Camera and Multiobject Spectrometer (NICMOS) in broadband filters at 1.1, 1.6, and 2.2 mu m (FWHM approximate to 0".21 at 2.2 mu m). The images show a very red unresolved point source at the center of the galaxy, confirming the existence of the obscured active nucleus inferred from previous ground-based studies. The 2.2 mu m flux, supplemented with ground-based L'-band observations, suggests thermal emission equivalent to a blackbody at a temperature of 720 K. We ascribe the emission not to direct light from the nucleus, but to hot dust in the inner part of the torus. The 1.6 mu m emission is only minimally affected by the hot dust emission. The luminosity of the central source producing most of the 1.6 mu m emission, not corrected for extinction, is 1.5 x 10(41) ergs s(-1), integrated over the F160W filter only.
• Minniti, D., Olszewski, E. W., & Rieke, M. (1993). The Bulge of M33. Astrophysical Journal Letters, 410(2 PART 2), L79-L82.
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  Abstract: H-band imaging of the central region of the Local Group galaxy M33 reveals a bulge with effective radius 0.5 kpc. The brightest bulge stars are resolved. After subtraction of disk contamination, we conclude that the brightest M33 bulge stars are substantially brighter than the brightest stars found in the Milky Way bulge. This fact suggests that the star formation histories of all bulges are not the same; specifically, M33's bulge underwent a star formation episode less than 1 Gyr ago.
• RIX, H., CARLETON, N., RIEKE, G., & RIEKE, M. (1993). PROBING INTERMEDIATE SEYFERT-GALAXIES BY PA-BETA SPECTROSCOPY. ASTROPHYSICAL JOURNAL, 363(2), 480-487.
• Rix, H., & Rieke, M. J. (1993). Tracing the stellar mass in M51. Astrophysical Journal Letters, 418(1), 123-134.
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  Abstract: We present optical and IR surface photometry of M51 (NGC 5194) at B, V, R, I, J, K, and CO(2.3 μm). These data are used to establish whether K band (2.2 μm) images of spiral galaxies provide reliable maps of stellar surface mass density features such as massive spiral arms or bars. The main distorting agents in the mapping at shorter wavelengths are dust extinction and luminous young stars. From modeling the color changes across the main dust lanes in M51, we find the optical depths to be ∼0.5 in the K band. For these optical depths the K band flux is attenuated by only ≲10% even in the dust lanes. From monitoring the gravity-sensitive CO(2.3 μm) index across the spiral arms we find that young, red supergiants do not distort significantly the K band image except in one small patch. OB associations are visible in the K band images but only cover a very small fraction of the spiral arms. On this basis, we conclude that K band images of face-on galaxies do trace the massive disk star population and allow a mapping of the azimuthal variation in the surface mass density of the stellar disk. In M51 we find the surface mass density contrast (arm/interarm) to range from 1.8 to 3, comparable to results from N-body simulations of the galaxy's tidal encounter with NGC 5195. This density contrast is larger than the light contrast in I band images, where the spiral arm crest is affected by dust extinction. The spiral arm amplitudes in M51 clearly show smooth, strong radial variations, with a maximum at ∼130″ and minima at 45″ and 170″. These variations may arise from interference of a pre-existing spiral pattern with the tidally induced spiral arms. An ongoing K band imaging study of a sample of spiral galaxies will yield a more representative picture of the role of bars and massive spiral arm features.
• Scoville, N., Evans, A., Thompson, R., Rieke, M., Hines, D., Low, F., Dinshaw, N., Surace, J., & Armus, L. (1993). NICMOS imaging of infrared-luminous galaxies. ASTRONOMICAL JOURNAL, 119(3), 991-1061.
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  We present near-infrared images obtained with the Hubble Space Telescope NICMOS camera for a sample of nine luminous [LIGs: L-IR(8-1000 mu m) greater than or equal to 10(11) L.] and 15 ultraluminous (ULIGS: L-IR greater than or equal to 10(12) L.) infrared galaxies. The sample includes representative systems classified as warm (f(25 mu m)/f(60 mu m) > 0.2) and cold (f(25 mu m)/f(60 mu m) less than or equal to 0.2) based on the mid-infrared colors and systems with nuclear emission lines classified as H II (i.e., starburst), QSO, Seyfert, and LINER. The morphologies of the sample galaxies are diverse and provide further support for the idea that they are created by the collision or interactions of spiral galaxies. Although no new nuclei are seen in the NICMOS images, the NICMOS images do reveal new spiral structures, bridges, and circumnuclear star clusters. The colors and the luminosities of the observed clusters are consistent with them being young (10(7)-10(8) yr), formed as a result of galactic interactions, and having masses much greater than those of Galactic globular clusters. In NGC 6090 and VV 114, they are preferentially situated along the area of overlap of the two galactic disks. With the exception of IR 17208-0018, all of the ULIGs have at least one compact (2.2 mu m FWHM less than or equal to 200 pc) nucleus. Analysis of the near-infrared colors (i.e., m(1.1-1.6) vs. m(1.6-2.2)) derived from 1." 1 diameter apertures suggests that the warm galaxies have near-infrared colors consistent with QSO+hot dust emission and the cold galaxies, as a group, have near-infrared colors consistent with reddened starlight. In addition, the cold ULIG UGC 5101 (and possibly three others) have near-infrared colors suggesting additional active galactic nucleus-like near-infrared components in their nuclei. In a 2 kpc diameter aperture measurement, the global colors of all of the cold galaxies except UGC 5101 are consistent with starlight with a few magnitudes of visual extinction. The general dichotomy of the near-infrared properties of the warm and the cold galaxies are further supported by the light distributions: seven of the eight warm galaxies have unresolved nuclear emission that contributes significantly (i.e., greater than or equal to 30%-40%) to the total near-infrared luminosity. The smooth, more extended light observed in all of the galaxies is most likely composed of giant and supergiant stars, but evidence at longer wavelengths suggests that these stars contribute little to the high 8-1000 mu m luminosity of these galaxies. Finally, light profiles of nine of the 24 systems were fitted well by an r(1/4) law (and not so well by an exponential disk profile). Whether these star systems eventually become massive central bulges or giant elliptical galaxies will depend on how efficiently the present ISM is converted into stars.
• Yun, J. L., Clemens, D. P., Mccaughrean, M. J., & Rieke, M. (1993). Near-infrared discovery of the L810 nebula illuminator. Astrophysical Journal Letters, 408(2 PART 2), L101-L103.
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  Abstract: As part of a deep near-infrared imaging survey for infrared point sources in Bok globules, we have discovered the illuminator of the optical reflection nebula seen toward the Bok globule L810. The illuminator (L810 1RS) is located at the position predicted by Scarrott, Rolph, & Tadhunter from analysis of their optical polarimetry. This source is very red (J - K ∼ 3.9) and bright (mK = 10.7), and has an estimated bolometric luminosity of 890 L⊙. Additionally, we found a near-infrared nebula which extends 20″ symmetrically to the north and to the south of L810 IRS, exhibiting an hourglass shape. Both the morphology and the orientation of the near-infrared nebula are in good agreement with the morphology and orientation of the high-velocity molecular outflow associated with L810. Finally, we found a near-infrared jetlike structure whose axis is collinear with L810 IRS. Together, these findings indicate that L810 IRS is likely to be a deeply embedded, very active intermediate-mass young stellar object within the L810 cloud.
• Zaritsky, D., Rix, H., & Rieke, M. (1993). Inner spiral structure of the galaxy M51. Nature, 364(6435), 313-315.
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  Abstract: MODELLING the structure and kinematics of spiral galaxies requires accurate maps of the mass-tracing stellar population. But this has hitherto been difficult because of dust obscuration and the presence of luminous young stars. To minimize the effects of dust and maximize sensitivity to the dominant stellar population, we have obtained K-band (2.2-μm) images of the nearby 'grand-design' spiral galaxy NGC5194 (M51). Our observations reveal remarkable dynamical structures not visible in conventional optical images. We find that the spiral arms extend significantly further towards the galaxy's centre than previously observed and can be traced continuously through almost three revolutions - roughly twice as far as with optical images. The coherence of the arms over this large radial range challenges current theories of spiral structure. We suggest that a combination of several mechanisms, such as the interaction of M51 with the neighbouring galaxy NGC5195, forcing by the central 'bar', or distortions from density waves, is required to generate the observed structure.
• Hinz, J. L., Misselt, K., Rieke, M. J., Rieke, G. H., Smith, P. S., Blaylock, M., & Gordon, K. D. (1992). Extended emission by dust in the dwarf galaxy UGC 10445. ASTROPHYSICAL JOURNAL, 651(2), 874-881.
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  We present Spitzer Space Telescope images of the isolated dwarf galaxy UGC 10445. The galaxy is detected at all photometric bands (3.6-160 mu m), as well as in the Multiband Imaging Photometer for Spitzer (MIPS) spectral energy distribution mode (55-95 mu m). We derive a star formation rate of 0.25 M(circle dot)yr(-1), based on H alpha and infrared flux densities. There is over 10(6) M-circle dot of cold dust (T similar to 18 K) in the galaxy, represented by 160 mu m emission, which extends to a larger radius than the ultraviolet (UV), optical, and near-infrared light. Such extended emission has been seen previously only in dwarf galaxies in cluster environments. We suggest that the source of heating for this dust is UV light, originating in star-forming complexes. To produce the large quantity of dust requires a higher rate of star formation in the past than is currently observed.
• KUHN, O., BECHTOLD, J., CUTRI, R., ELVIS, M., & RIEKE, M. (1992). THE SPECTRAL ENERGY-DISTRIBUTION OF THE Z=3 QUASAR - HS-1946+7658. ASTROPHYSICAL JOURNAL, 438(2), 643-649.
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  For the bright z = 3.02 radio-quiet quasar, HS 1946+7658, we have obtained radio to X-ray data within the past year: 5 GHz and 1415 MHz data from the VLA; IR photometry at J, H, K, L' (3.4 mu m) and N; IR spectroscopy; UBVRI photometry; optical spectrophotometry and high-resolution spectra; and an X-ray spectrum from the ROSAT PSPC. The spectral energy distribution (SEC) constructed from these data is compared to the mean SED for a set of low-redshift quasars, and while they appear generally similar, there are several differences. In relation to the low-redshift mean, the SED of HS 1946+7658 shows (1) only an upper limit at 10 mu m (a rest wavelength of 2.5 mu m) indicating that HS 1946+7658 does not have a strong near-IR excess such as hot dust would produce; (2) relatively weak Fe II and Balmer continuum emission at similar to 3000 Angstrom; and (3) a steeper turndown shortward of Ly alpha, even after correction for the Ly alpha forest absorption lines.
• Tegler, S. C., Campins, H., Larson, S., Kleine, M., Kelly, D., & Rieke, M. (1992). Simultaneous visible and near-infrared spectrophotometry of comet Austin 1989c₁. Astrophysical Journal Letters, 396(2), 711-716.
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  Abstract: Simultaneous visible and near-infrared spectra of comet Austin were obtained with the 1.5 m and 2.3 m telescopes of the University of Arizona Observatories on 1990 May 16. The visible spectrum obtained with the IHW spectrograph covers the 3126-9490 Å wavelength interval, while the near-infrared spectrum obtained with the germanium spectrometer covers the 9036-12794 Ä wavelength interval. For the first time, we present simultaneous measurements of integrated band fluxes for the CN B 2Σ+ - X 2Σ+ (violet) and A 2Π+ - X 2Σ+ (red) systems. We also present a CN spectrum and CN band flux ratios calculated from a fluoresence equilibrium model. From a comparison between the observed and calculated CN spectra and band flux ratios, we find that red system oscillator strengths determined from recent ab initio calculations appropriately describe the radiative properties of CN molecules.
• Elston, R., Bechtold, J., Lowenthal, J., & Rieke, M. (1991). Emission from the z = 2 damped Lyα absorber toward Q1215 + 333. Astrophysical Journal Letters, 373(2 PART 2), L39-L42.
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  Abstract: We have detected narrow emission lines at 1.118 μm and 1.456 μm in the spectrum of the z = 2.606 quasar Q1215 + 333, corresponding to [O II] λ3727 and Hβ at z = 1.9984, the redshift of a damped Lyα absorber toward this quasar. The intensity of the Hβ line is 7.6 ± 2 × 10-16 ergs cm-2 s-1, which corresponds to a line luminosity of 5 × 1042 ergs s-1 h-2100 (q0 = 0.5). If we assume that the photoionization producing the emission is due purely to massive star formation with a Salpeter initial mass function, we find a total star formation rate of 100 M⊙ yr-1 h-2100. Given the uncertainty in the initial mass function and cosmological parameters, this star formation rate is very uncertain. However, the star formation rate is well above those inferred from Lyα emission-line searches of similar systems, implying effective destruction of Lyα photons. The intensity of the [O II] λ3727 line is 1.6 ± 0.3 × 10-15 ergs cm-2 s-1. The ratio [O II]/Hβ ≈ 2 and the weakness of the ratio [O III] λ5007/β < 0.5 is typical of star formation regions with gas at nearly solar metallicity.
• MCLEOD, B., RIEKE, M., & WEEDMAN, D. (1990). INFRARED OBSERVATIONS OF THE DARK-MATTER LENS CANDIDATE-Q2345+007. ASTROPHYSICAL JOURNAL, 433(2), 528-532.
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  Deep K-band observations are presented of the double image quasar Q2345+007. This has the largest separation (7.1'') of any quasar image pair considered as gravitationally lensed, so the required lens is massive (10(13) M.). No lens has been detected in previous deep images at visible wavelengths, and we find no lens to limiting K magnitude 20.0 in the infrared image. This constrains any lens to being much less luminous than brightest cluster galaxies, while the lens must be much more massive than such galaxies to produce the observed separation. Because spectral data indicate exceptional intrinsic similarity in the quasar image components, this pair remains as the most intriguing example of an observed configuration requiring the presence of massive, concentrated dark matter acting as a gravitational lens.
• Palamara, D. P., Brown, M. J., Jannuzi, B. T., Dey, A., Stern, D., Pimbblet, K. A., Weiner, B. J., Ashby, M. L., Kochanek, C. S., Gonzalez, A., Brodwin, M., Le Floc'h, E., & Rieke, M. (1990). THE CLUSTERING OF EXTREMELY RED OBJECTS. ASTROPHYSICAL JOURNAL, 764(1).
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  We measure the clustering of extremely red objects (EROs) in approximate to 8 deg(2) of the NOAO Deep Wide Field Survey Bootes field in order to establish robust links between ERO(z approximate to 1.2) and local galaxy (z < 0.1) populations. Three different color selection criteria from the literature are analyzed to assess the consequences of using different criteria for selecting EROs. Specifically, our samples are (R - K-s) > 5.0 (28,724 galaxies), (I - K-s) > 4.0 (22,451 galaxies), and (I - [3.6]) > 5.0 (64,370 galaxies). Magnitude-limited samples show the correlation length (r(0)) to increase for more luminous EROs, implying a correlation with stellar mass. We can separate star-forming and passive ERO populations using the (K-s - [24]) and ([3.6]-[24]) colors to K-s = 18.4 and [3.6] = 17.5, respectively. Star-forming and passive EROs in magnitude-limited samples have different clustering properties and host dark halo masses and cannot be simply understood as a single population. Based on the clustering, we find that bright passive EROs are the likely progenitors of greater than or similar to 4L* elliptical galaxies. Bright EROs with ongoing star formation were found to occupy denser environments than star-forming galaxies in the local universe, making these the likely progenitors of greater than or similar to L* local ellipticals. This suggests that the progenitors of massive greater than or similar to 4L* local ellipticals had stopped forming stars by z greater than or similar to 1.2, but that the progenitors of less massive ellipticals (down to L*) can still show significant star formation at this epoch.
• Stocke, J. T., Rieke, G. H., & Lebofsky, M. J. (1981). New observational constraints on the M87 jet. NATURE, 294(5839), 319-322.
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  New observations at 1.6-3.45 mu m confirm the presence of a dramatic (Delta alpha similar to 1) break between radio-IR wavelengths and 6,000 angstrom, in the spectrum of the M87 jet. These data, in combination with data taken in other spectral regions, show that the individual knots in the M87 jet have nearly the same spectral indices and nearly the same large (Delta alpha similar to 1) spectral break. This large spectral break and the constancy of spectral properties between the knots pose serious constraints for models of the M87 jet.

Proceedings Publications

• Chu}, L., Hodapp, K., Rieke, M., Meyer, M., Greene, T., & Team, {. (2017, jun). JWST NIRCam WFSS Ice Feature Spectroscopy in Nearby Molecular Cores. In American Astronomical Society Meeting Abstracts \#230, 230.
• Frye, B. L., Rieke, M. J., Willmer, C. N., Egami, E., Ferruit, P., Alberts, S., Bunker, A., Charlot, S., Chevallard, J., Dressler, A., Eisenstein, D., Endsley, R., Franx, M., Hainline, K., Jakobsen, P., Lake, E., Maiolino, R., Rix, H., Robertson, B., , Stark, D., et al. (2017, June). NIRcam-NIRSpec GTO Observations of Galaxy Evolution. In AAS, 230.
• Rieke, M., Ferruit, P., Alberts, S., Bunker, A., Charlot, S., Chevallard, J., Dressler, A., Egami, E., Eisenstein, D., Endsley, R., Franx, M., Frye, B., Hainline, K., Jakobsen, P., Lake, E., Maiolino, R., Rix, H., Robertson, B., Stark, D., , Williams, C., et al. (2017, jun). NIRcam-NIRSpec GTO Observations of Galaxy Evolution. In American Astronomical Society Meeting Abstracts \#230, 230.
• Hinz, J. L., Rieke, M. J., Rieke, G. H., Smith, P. S., Misselt, K., Blaylock, M., Gordon, K. D., Chary, R., Teplitz, H., & Sheth, K. (2013). Dust in dwarfs and low surface brightness galaxies. In SECOND ANNUAL SPITZER SCIENCE CENTER CONFERENCE: INFRARED DIAGNOSTICS OF GALAXY EVOLUTION, 381, 153-156.
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  We describe Spitzer images of a sample of dwarf and low surface brightness galaxies, using the high sensitivity and spatial resolution to explore the morphologies of dust in these galaxies. For the starbursting dwarf UGC 10445, we present a complete infrared spectral energy distribution and modeling of its individual dust components. We find that its diffuse cold (T=19 K) dust component extends beyond its near-infrared disk and speculate that the most plausible source of heating is ultraviolet photons from starforming complexes. We find that the mass of T= 19 K dust in UGC 10445 is surprisingly large, with a lower limit of 3 x 10(6) M-circle dot. We explore the implications of having such a high dust content on the nature and evolution of the galaxy.
• Sivanandam, S., Rieke, M. J., Rieke, G., Sun, M., & Sarazin, C. L. (2013, jan). Ram-Pressure Stripping of Molecular Gas and Dust in Nearby Cluster Galaxies. In American Astronomical Society Meeting Abstracts, 221, #226.02.
• Sellgren, K., Cotera, A., Figer, D., Yusef-Zadeh, F., Blum, R., Rieke, G., Anantharamaiah, K., Najarro, F., Simpson, J., Goss, W., Mezger, P., Falcke, H., Sanders, R., Wardle, M., Stolovy, ., Narayan, R., Lazio, T., Maeda, Y., Rieke, M., , Biermann, P., et al. (2012). Discussion Session V: How, when, where and why are stars formed in the Galactic Center?. In CENTRAL PARSECS OF THE GALAXY, 186, 358-370.
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  This is an edited transcript of a discussion session about star formation in the Galactic Center that took place during the Galactic Center conference "The Central Parsecs" in Tucson, Arizona, Sep. 11, 1998. The session was chaired by the moderator as indicated in the author list. The discussions were taped, transcribed, and finally edited by an editor who is listed as co-author. The contributions of the conference participants are preceded by their names and thus references to specific aspects and ideas of this discussion session must also include a reference to the respective speaker(s), e.g., in a footnote.
• Wilson, J. C., Hearty, F., Skrutskie, M. F., Majewski, S. R., Schiavon, R., Eisenstein, D., Gunn, J., Gillespie, B., Weinberg, D., Blank, B., Henderson, C., Smee, S., Barkhouser, R., Harding, A., Hope, S., Fitzgerald, G., Stolberg, T., Arns, J., Nelson, M., , Brunner, S., et al. (2012, jan). Apache Point Observatory Galactic Evolution Experiment (APOGEE) Spectrograph. In American Astronomical Society Meeting Abstracts #219, 219, #428.02.
• Becklin, E., Cotera, A., Genzel, R., Gezari, D., Ghez, A., Rieke, G., Yusef-Zadeh, F., Melia, F., Townes, C., Eckart, A., Reid, M., Falcke, H., Narayan, R., Bower, G., Wardle, M., Stolovy, ., Zhao, J., Rieke, M., Falcke, H., , Cotera, A., et al. (2011). Discussion session I: What is the central matter distribution?. In CENTRAL PARSECS OF THE GALAXY, 186, 49-63.
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  This is an edited transcript of a discussion session about the mass concentration and the evidence for a central black hole in the Galactic Center that took place during the Galactic Center conference "The Central Parsecs" in Tucson, Arizona, Sep. 7-11, 1998. The session was chaired by the moderator as indicated in the author list. The discussions were taped, transcribed, and finally edited by an editor who is listed as co-author. The contributions of the conference participants are preceded by their names and thus references to specific aspects and ideas of this discussion session must also include a reference to the respective speaker(s), e.g., in a footnote.
• BECHTOLD, J., CUTRI, R., RIEKE, M., ELVIS, M., FIORE, F., WILKES, B., Schlegel, E., & Petre, R. (2010). IR TO X-RAY SPECTRAL ENERGY-DISTRIBUTIONS OF HIGH-REDSHIFT QUASARS. In SOFT X-RAY COSMOS, 105-109.
• Hinz, J. L., Engelbracht, C. W., Willmer, C. N., Rieke, G. H., Rieke, M. J., Misselt, K., Smith, P. S., Blaylock, M., Gordon, K. D., , ., Funes, J., & Corsini, E. (2010). The Spatial Distribution of Cold Dust in Nearby Galaxies. In FORMATION AND EVOLUTION OF GALAXY DISKS, 396, 119-122.
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  We review results from the Spitzer MIPS instrument regarding the spatial distribution of cold dust; emission in a variety of nearby galaxies, focusing on their outer disks. Large masses of cold dust can be observed surrounding objects of varying physical size and morphological type, including galaxies quite low in mass. The cold dust emission represented by the MIPS 70 and 160 pm images extends well beyond the optical and near-infrared disks of M 31 and M 33, as is also the case for nearby starbursting dwarfs. The amount of detectable cold dust emission is dependent on the amount of diffuse, non-ionizing ultraviolet photons produced by the young stellar population. Therefore, many more galaxies with lower rates of star formation may have large amounts of very cold dust that escape detection. The existence of such cold dust halos allows us to probe issues regarding the assembly, storage, and retention of dust in disk galaxies and to better understand how the dust interacts with its environment. For instance, tracing gas-to-dust ratios far into disks allows us to distinguish between methods of dust production and transportation, and comparing with other wavelengths enables us to locate the sources of dust heating.
• ELSTON, R., RIEKE, G., RIEKE, M., & KRON, R. (2009). THE STUDY OF GALAXY EVOLUTION USING A LARGE AREA 2-MU SURVEY. In EVOLUTION OF THE UNIVERSE OF GALAXIES, 10, 289-291.
• Wilson, J. C., Hearty, F., Skrutskie, M. F., Majewski, S., Schiavon, R., Eisenstein, D., Gunn, J., Blank, B., Henderson, C., Smee, S., Barkhouser, R., Harding, A., Fitzgerald, G., Stolberg, T., Arns, J., Nelson, M., Brunner, S., Burton, A., Walker, E., , Lam, C., et al. (2008). The Apache Point Observatory Galactic Evolution Experiment (APOGEE) high-resolution near-infrared multi-object fiber spectrograph. In GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY III, 7735.
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  The Apache Point Observatory Galactic Evolution Experiment (APOGEE) will use a dedicated 300-fiber, narrow-band (1.5-1.7 micron), high resolution (R similar to 30,000), near-infrared spectrograph to survey approximately 100,000 giant stars across the Milky Way. This survey, conducted as part of the Sloan Digital Sky Survey III (SDSS III), will revolutionize our understanding of kinematical and chemical enrichment histories of all Galactic stellar populations. The instrument, currently in fabrication, will be housed in a separate building adjacent to the 2.5 m SDSS telescope and fed light via approximately 45-meter fiber runs from the telescope. The instrument design includes numerous technological challenges and innovations including a gang connector that allows simultaneous connection of all fibers with a single plug to a telescope cartridge that positions the fibers on the sky, numerous places in the fiber train in which focal ratio degradation must be minimized, a large (290 mm x 475 mm elliptically-shaped recorded area) mosaic-VPH, an f/1.4 six-element refractive camera featuring silicon and fused silica elements with diameters as large as 393 mm, three near-infrared detectors mounted in a 1 x 3 mosaic with sub-pixel translation capability, and all of these components housed within a custom, LN2-cooled, stainless steel vacuum cryostat with dimensions 1.4 m x 2.3 m x 1.3 m.
• Perez-Gonzalez, P. G., Rieke, G. H., Le Floch, E., Papovich, C., Huang, J. S., Barmby, P., Dole, H., Egami, E., Alonso-Herrero, A., Rigby, J. R., Bei, L., Blaylock, M., Engelbracht, C. W., Fazio, G. G., Gordon, K. D., Misselt, K. A., Morrison, J. E., Muzerolle, J., Rieke, M. J., , Willner, S. P., et al. (2007). Cosmological surveys with the Spitzer Space Telescope. In II INTERNATIONAL GTC WORKSHOP: SCIENCE WITH GTC 1ST-LIGHT INSTRUMENTS AND THE LMT, 24, 205-209.
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  NASA's Spitzer Space Telescope (formerly known as the Space Infrared Telescope Facility SIRTF) is now on normal science operation and open to the international community. One of the Guaranteed Time Observer programs consists in a series of surveys using the two imaging instruments on Spitzer: MIPS (observing at 24, 70, and 160 microns) and IRAC (3.6, 4.5, 5.6 and 8 microns). The program includes observations to various depths, from wide field shallow, to very deep confusion limited surveys. We are also conducting a series of supporting programs (including also data from the spectrograph on Spitzer, IRS) to help interpret what we see in the deep surveys, e.g., the characterization of the spectral energy distributions of about 150 QSOs, and an extensive study of low-metallicity nearby star-forming galaxies. GTC first light is scheduled when the first well-established results from our Cosmological Surveys program will be released, offering us an incomparable facility to perform spectroscopic and photometric follow-ups of mid- and far-infrared selected sources. Moreover, the combination of the GTC, Spitzer and the Large Millimeter Telescope (LMT) facilities will allow us to study the galaxy populations in the Universe with a sensitivity and a coverage of the electromagnetic spectrum that have no precedents until today.
• Murray, S., Forman, W., Jones, C., Kenter, A., Green, P., Fabricant, D., Fazio, G., Jannuzi, B., Dey, A., Najita, J., Brown, M., Brand, K., Shields, J., McNamara, B., Rieke, M., Kochanek, C., Hasinger, G., & Turner, M. (2006). X-ray 3 dimensional survey in the NDWFS Bootes field: Large area Chandra shallow X-ray survey -I. In UV AND GAMMA-RAY SPACE TELESCOPE SYSTEMS, PTS 1 AND 2, 5488, 242-250.
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  In March and April 2003, the Chandra X-ray Observatory carried out a series of 126 short observations (5 ksec each) covering a continuous area of the Bootes constellation to construct a large area shallow X-ray survey. These observations were carried out as collaboration of Guest Observer (C. Jones PI) and Guaranteed Time Observer (S. Murray PI) programs. We present here, in Paper 1, an initial analysis of the survey data and the source detection process, showing the sky coverage, exposure map, and some of the collective properties of the resulting catalog of sources. The Bootes area was selected to overlap a well studied region where optical, and radio data, to sufficient depth, have already been obtained making the identification of candidate counterparts straight forward. In 5 ksec, we reach a limiting flux of similar to10(-3) CtS(-1) (corresponding to similar to 10(-14) erg CM(-2)s(-1) 0.5 - 7.0 keV). We examine the spatial distribution of the sources in this (similar to)9.3 square degree survey region using several techniques to search for evidence of cosmic variance in the X-ray source density on scales as small as the ACIS-I field of view ((similar to)16x16 arc minutes). With follow up optical spectroscopy using the MMT/Hectospec, we can obtain spectroscopic redshifts for about 1/3 - 1./2 of the X-ray sources, which can be used to look for evidence of large scale structures traced by AGN associated with the cosmic web.
• Papovich, C., Le Floc'h, E., Dole, H., Egami, E., Perez-Gonzalez, P., Rieke, G., Rieke, M., , ., DeGrijs, R., & Delgado, R. (2006). Understanding infrared-luminous starbursts in distant galaxies. In Starbursts: From 30 Doradus to Lyman Break Galaxies, 329, 285-288.
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  New surveys with the Spitzer space telescope identify distant starburst and active galaxies by their strong emission at far-infrared (IR) wavelengths. Using deep Spitzer surveys at 24 and 70 mu m coupled with HST imaging in the Chandra Deep Field South, we study the relation between galaxy morphology and IR-active stages of galaxy evolution. IR-lummous galaxies span a wide range of morphology. At z similar to 1, there is a correlation between the relative fraction of galaxies with morphological distortions (multiple nuclei, tidal tails, etc.) and increasing IR luminosity, which suggests that the strong starbursts at high redshift arise from galaxy interactions. However, the majority of IR-lummous galaxies do not have exceptionally asymmetric morphologies, and galaxies with strong asymmetries correspond to a range of galaxy IR activity. We conclude that the relation between galaxy morphology and IR activity is highly complex, and strongly dependent on the initial conditions of galaxy interactions.
• Davila, P., Bos, B., Contreras, J., Evans, C., Greenhouse, M., Hobbs, G., Holota, W., Huff, L., Hutchings, J., Jamieson, T., Lightsey, P., Morbey, C., Murowinski, R., Rieke, M., Rowlands, N., Steakley, B., Wells, M., Plate, M., Wright, G., & Mather, J. (2005). The James Webb Space Telescope science instrument suite: An overview of optical designs. In OPTICAL, INFRARED, AND MILLIMETER SPACE TELESCOPES, PTS 1-3, 5487, 611-627.
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  The James Webb Space Telescope (JWST) Observatory, the follow-on mission to the Hubble Space Telescope and to the Spitzer Space Facility, will yield astounding breakthroughs in the realms of infrared space science. The science instrument suite for this Observatory will consist of a Near-Infrared Camera, a Near-Infrared Spectrograph, a Mid-Infrared Instrument with imager, coronagraph and integral field spectroscopy modes, and a Fine Guider System Instrument with both a Guider module and a Tunable Filter Module. In this paper we present an overview of the optical designs of the telescope and instruments.
• Falcke, H., Kern, S., Cotera, A., Antonucci, R., Doeleman, S., Novak, G., Sanders, R., Anantharamaiah, K., Rieke, M., Biermann, P., Lazio, T., Melia, F., Falcke, H., Cotera, A., Duschl, W., Melia, F., & Rieke, M. (2005). Discussion session IX: How "standard" is the central region of our galaxy? What would the GC look like from one mpc distance?. In CENTRAL PARSECS OF THE GALAXY, 186, 536-539.
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  This is an edited transcript of a discussion session about the comparison of the Galactic Center with other galaxies and Active Galactic Nuclei (AGN) that took place during the Galactic Center conference "The Central Parsecs" in Tucson, Arizona, Sep. 7-11, 1998. The session was chaired by the moderator as indicated in the author list. The discussions were taped, transcribed, and finally edited by editors who are listed as co-authors. The contributions of the conference participants are preceded by their names and thus references to specific aspects and ideas of this discussion session must also include a reference to the respective speaker(s), e.g., in a footnote.
• Le Floc'h, E., Papovich, C., Dole, H., Egami, E., Perez-Gonzalez, P., Rieke, G., Rieke, M., Bell, E., , ., DeGrijs, R., & Delgado, R. (2005). Evolution of the IR energy density and SFH up to Z similar to 1: First results from MIPS. In Starbursts: From 30 Doradus to Lyman Break Galaxies, 329, 279-282.
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  Using deep observations of the Chandra Deep Field South obtained with MIPS at 24 mu m, we present our preliminary estimates on the evolution of the infrared (IR) luminosity density of the Universe from z = 0 to z similar to 1. We find that a pure density evolution of the IR luminosity function is clearly excluded by the data. The characteristic luminosity L*(IR) evolves at least by (1 + z)(3.5) with lookback time, but our monochromatic approach does not allow us to break the degeneracy between a pure evolution in luminosity, or an evolution in both density and luminosity. Our results imply that IR-luminous systems (L-IR >= 10(11) L circle dot) become the dominant population contributing to the co-moving IR energy density beyond z similar to 0.5 - 0.6. The uncertainties affecting our measurements are largely dominated by the poor constraints on the spectral energy distributions that are used to translate the observed 24 mu m flux into luminosities.
• Rieke, M., Wang, W., Lu, J., Luo, Z., Yang, Z., Hua, H., & Chen, Z. (2005). The JWST-NIRCam View of Galaxy Evolution. In GALAXY EVOLUTION: INFRARED TO MILLIMETER WAVELENGTH PERSPECTIVE, 446, 331-338.
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  The James Webb Space Telescope has been designed to address a range of scientific questions with those posed by discovering the early galaxies that re-ionized the Universe at the top of the list. Examining how galaxies evolved from those early objects to the galaxies we see today is another prime goal. The instrumention and telescope have been optimized for the study of galaxy evolution.
• Wilson, J. C., Hearty, F., Skrutskie, M. F., Majewski, S. R., Schiavon, R., Eisenstein, D., Gunn, J., Holtzman, J., Nidever, D., Gillespie, B., Weinberg, D., Blank, B., Henderson, C., Smee, S., Barkhouser, R., Harding, A., Hope, S., Fitzgerald, G., Stolberg, T., , Arns, J., et al. (2005). Performance of the Apache Point Observatory Galactic Evolution Experiment (APOGEE) high-resolution near-infrared multi-object fiber spectrograph. In GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY IV, 8446.
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  The Apache Point Observatory Galactic Evolution Experiment (APOGEE) uses a dedicated 300-fiber, narrow-band near-infrared (1.51-1.7 mu m), high resolution (R similar to 22,500) spectrograph to survey approximately 100,000 giant stars across the Milky Way. This three-year survey, in operation since late-summer 2011 as part of the Sloan Digital Sky Survey III (SDSS III), will revolutionize our understanding of the kinematical and chemical enrichment histories of all Galactic stellar populations. We present the performance of the instrument from its first year in operation. The instrument is housed in a separate building adjacent to the 2.5-m SDSS telescope and fed light via approximately 45-meter fiber runs from the telescope. The instrument design includes numerous innovations including a gang connector that allows simultaneous connection of all fibers with a single plug to a telescope cartridge that positions the fibers on the sky, numerous places in the fiber train in which focal ratio degradation had to be minimized, a large mosaic-VPH (290 mm x 475 mm elliptically-shaped recorded area), an f/1.4 six-element refractive camera featuring silicon and fused silica elements with diameters as large as 393 mm, three near-infrared detectors mounted in a 1 x 3 mosaic with sub-pixel translation capability, and all of these components housed within a custom, LN2-cooled, stainless steel vacuum cryostat with dimensions 1.4-m x 2.3-m x 1.3-m.
• Rieke, M., Chary, R., Teplitz, H., & Sheth, K. (2004). Future prospects: In space and on the ground. In SECOND ANNUAL SPITZER SCIENCE CENTER CONFERENCE: INFRARED DIAGNOSTICS OF GALAXY EVOLUTION, 381, 501-506.
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  Spitzer has enabled a new regime in the study of galaxy evolution by supplying imporved resolution and senstivity over previous infrared missions. Future missions promise even greater leaps with projects such as the James Webb Space Telescope (JWST) and the Atacama Large Millimeter Array (ALMA) providing HST-like resolution in the infrared and millimeter ranges. Missions such as SAFIR will be needed to complete the suite of capabilities at long wavelengths.
• VURAL, K., KOZLOWSKI, L., RASCHE, B., RIEKE, M., & LETTINGTON, A. (2004). 256X256 HGCDTE FOCAL PLANE ARRAY FOR THE HUBBLE SPACE TELESCOPE. In INFRARED TECHNOLOGY AND APPLICATIONS /, 1320, 107-108.
• Greene, T., Beichman, C., Gully-Santiago, M., Jaffe, D., Kelly, D., Krist, J., Rieke, M., Smith, E. H., Oschmann, J., Clampin, M., & MacEwen, H. (2003). NIRCam: Development and Testing of the JWST Near-Infrared Camera. In SPACE TELESCOPES AND INSTRUMENTATION 2010: OPTICAL, INFRARED, AND MILLIMETER WAVE, 7731.
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  The Near Infrared Camera (NIRCam) is one of the four science instruments of the James Webb Space Telescope (JWST). Its high sensitivity, high spatial resolution images over the 0.6 - 5 mu m wavelength region will be essential for making significant findings in many science areas as well as for aligning the JWST primary mirror segments and telescope. The NIRCam engineering test unit was recently assembled and has undergone successful cryogenic testing. The NIRCam collimator and camera optics and their mountings are also progressing, with a brass-board system demonstrating relatively low wavefront error across a wide field of view. The flight model's long-wavelength Si grisms have been fabricated, and its coronagraph masks are now being made. Both the short (0.6 - 2.3 mu m) and long (2.4 - 5.0 mu m) wavelength flight detectors show good performance and are undergoing final assembly and testing. The flight model subsystems should all be completed later this year through early 2011, and NIRCam will be cryogenically tested in the first half of 2011 before delivery to the JWST integrated science instrument module (ISIM).
• Greene, T., Beichman, C., Eisenstein, D., Horner, S., Kelly, D., Mao, Y., Meyer, M., Rieke, M., Shi, F., & Coulter, D. (2001). Observing exoplanets with the JWST NIRCam grisms - art. no. 66930G. In TECHNIQUES AND INSTUMENTATION FOR DETECTION OF EXOPLANETS III, 6693, G6930-G6930.
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  The near-infrared camera (NIRCam) on the James Webb Space Telescope (JWST) will incorporate 2 identical grisms in each of its 2 long wavelength channels. These transmission gratings have been added to assist with the coarse phasing of the JWST telescope, but they will also be used for slitless wide-field scientific observations over selectable regions of the lambda = 2.4 - 5.0 mu m wavelength range at spectroscopic resolution R equivalent to lambda/delta lambda similar or equal to 2000. We describe the grism design details and their expected performance in NIRCam. The grisms will provide point-source continuum sensitivity of approximately AB = 23 mag in 10,000 s exposures with S/N = 5 when binned to R = 1000. This is approximately a factor of 3 worse than expected for the JWST NIRSpec instrument, but the NIRCam grisms provide better spatial resolution, better spectrophotometric precision, and complete field coverage. The grisms will be especially useful for high precision spectrophotometric observations of transiting exoplanets. We expect that R = 500 spectra of the primary transits and secondary eclipses of Jupiter-sized exoplanets can be acquired at moderate or high signal-to-noise for stars as faint as M = 10 - 12 mag in 1000 s of integration time, and even bright stars (V = 5 mag) should be observable without saturation. We also discuss briefly how these observations will open up new areas of exoplanet science and suggest other unique scientific applications of the grisms.
• LLOYDHART, M., WIZINOWICH, P., WITTMAN, D., COLUCCI, D., MCLEOD, B., DEKANY, R., ANGEL, R., MCCARTHY, D., RIEKE, M., MCCAUGHREAN, M., KOHNLE, A., & MILLER, W. (2000). HIGH-RESOLUTION IMAGING AT THE MULTIPLE MIRROR TELESCOPE USING ADAPTIVE OPTICS. In ATMOSPHERIC PROPAGATION AND REMOTE SENSING, 1688, 442-452.
• Goss, W., Coker, R., Cotera, A., Kassim, N., Yusef-Zadeh, F., Reid, M., Roberts, D., Novak, G., Townes, C., Wardle, M., Anantharamaiah, K., Melia, F., Zylka, R., Sanders, R., Mezger, P., Falcke, H., Zhao, J., Coil, A., Rieke, M., , Simpson, J., et al. (1999). Discussion session VII: How do the various components of the inner 100 parsecs interact with each other?. In CENTRAL PARSECS OF THE GALAXY, 186, 465-479.
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  This is an edited transcript of a discussion session about the various components (Sgr A East & West, CND, ionized gas, large-scale radio structure etc.) filling the inner 10 to 100 parsecs of the Galactic Center that took place during the Galactic Center conference "The Central Parsecs" in Tucson, Arizona, Sep. 7-11, 1998. The session was chaired by the moderator as indicated in the author list. The discussions were taped, transcribed, and finally edited by editors who are listed as co-authors. The contributions of the conference participants are preceded by their names and thus references to specific aspects and ideas of this discussion session must also include a reference to the respective speaker(s), e.g., in a footnote.
• Horner, S., Rieke, M., , ., & Mather, J. (1999). The near infrared camera (NIRCam) for the James Webb Space Telescope (JWST). In OPTICAL, INFRARED, AND MILLIMETER SPACE TELESCOPES, PTS 1-3, 5487, 628-634.
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  The NIRCam science objectives are the detection and identification of "first light" objects, the study of star and brown dwarf formation, and the detection and characterization of planetary systems and their formation. These three science programs are also the key objectives of the JWST program as a whole. The NIRCam instrument design is optimized for these objectives within the mission constraints.
• THOMPSON, R., RIEKE, M., KORMOS, K., MENTZELL, E., & Fowler, A. (1999). Characterization of the NICMOS flight detectors and their capabilities. In INFRARED DETECTORS AND INSTRUMENTATION FOR ASTRONOMY, 2475, 367-375.
• MINNITI, D., RIEKE, M., OLSZEWSKI, E., & McLean, I. (1995). IR PHOTOMETRY OF GLOBULAR-CLUSTERS AND BULGE FIELDS. In INFRARED ASTRONOMY WITH ARRAYS: THE NEXT GENERATION, 190, 107-108.
• Rieke, M., Baum, S., Beichman, C., Crampton, D., Doyon, R., Eisenstein, D., Greene, T., Hodapp, K., Horner, S., Johnstone, D., Lesyna, L., Lilly, S., Meyer, M., Martin, P., McCarthy, D., Rieke, G., Roellig, T., Stauffer, J., Trauger, J., , Young, E., et al. (1994). NGST NIRCam scientific program and design concept. In IR SPACE TELESCOPES AND INSTRUMENTS, PTS 1 AND 2, 4850, 478-485.
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  The science program for the Next Generation Space Telescope (NGST) relies heavily on a high performance near-infrared imager. A design which supports the observations outlined in the Design Reference Mission (DRM) and which also supports enhanced searches for "first light" objects and planets has been developed. Key features of the design include use of refractive optics to minimize the volume and mass required, tunable filters for spectroscopic imaging, and,redundant imagers for fail-safe wavefront sensing.
• Rieke, M., , ., Cristiani, S., Renzini, A., & Williams, R. (1991). The deep infrared sky: SIRTF surveys of Chandra-South and other fields. In DEEP FIELDS, 117-122.
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  The Space Infrared Telescope Facility's cameras have been designed for efficient surveying. The Guaranteed Time Observers, the SIRTF Science Center, and several legacy science teams have laid out a comprehensive program to probe to the confusion limit from 3.6 mum to 160 mum.
• Corbin, M., Thompson, R., O'Neil, E., Rieke, M., Schneider, G., Weymann, R., StorrieLombardi, L., Sawicki, M., & Brunner, R. (1990). High redshift galaxies and QSOs in the NICMOS parallel fields. In PHOTOMETRIC REDSHIFTS AND HIGH REDSHIFT GALAXIES, 191, 247-252.
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  We present the first results of a program to identify high-redshift galaxies and QSOs in the archive of parallel images obtained by the HST NICMOS instrument during its initial lifetime. We have detected similar to 100 high-redshift galaxy candidates in the Camera 1 and Camera 2 parallel fields. The brightness profiles of these galaxies, which trace their rest-frame optical emission, reveal many of them to be fully-formed elliptical and spiral galaxies similar to those in the local universe, and the spectral energy distributions of the objects indicate that most are not actively forming stars. Using the composite QSO spectrum derived from the Large Bright Quasar Survey as a template, we also find evidence for several dust-reddened QSOs at high redshift, including candidates at z > 5. While these require spectroscopic confirmation, our color selection technique for such objects can also be applied to ground-based infrared observations.

Reviews

• Perez-Gonzalez, P., Rieke, G., Egami, E., Alonso-Herrero, A., Dole, H., Papovich, C., Blaylock, M., Jones, J., Rieke, M., Rigby, J., Barmby, P., Fazio, G., Huang, J., & Martin, C. (1995. Spitzer view on the evolution of star-forming galaxies from z=0 to z similar to 3(pp 82-107).
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  We use a 24 mu m - selected sample containing more than 8000 sources to study the evolution of star- forming galaxies in the redshift range from z = 0 to z similar to 3. We obtain photometric redshifts for most of the sources in our survey using a method based on empirically built templates spanning from ultraviolet to mid- infrared wavelengths. The accuracy of these redshifts is better than 10% for 80% of the sample. The derived redshift distribution of the sources detected by our survey peaks at around z 0: 6 1: 0 ( the location of the peak being affected by cosmic variance) and decays monotonically from z similar to 1 to z similar to 3. We have fitted infrared luminosity functions in several redshift bins in the range 0 < z less than or similar to 3. Our results constrain the density and/ or luminosity evolution of infrared- bright star- forming galaxies. The typical infrared luminosity ( L*) decreases by an order of magnitude from z similar to 2 to the present. The cosmic star formation rate ( SFR) density goes as ( 1+ z) (4. 0 +/- 0. 2) from z= 0 to 0.8. From z= 0. 8 z similar to 1. 2, the SFR density continues rising with a smaller slope. At 1: 2 < z 10(11) L(circle dot)) to the total SFR density increases steadily from z similar to 0 up to z similar to 2.5, forming at least half of the newly born stars by z similar to 1. 5. Ultraluminous infrared galaxies ( L(TIR) > 10(12) L(circle dot)) play a rapidly increasing role for z greater than or similar to 1.3.

Others

• Papovich, C., Rudnick, G., Rigby, J. R., Willmer, C. N., Smith, J. -., Finkelstein, S. L., Egami, E., & Rieke, M. (2004, DEC 1). PASCHEN-alpha EMISSION IN THE GRAVITATIONALLY LENSED GALAXY SMM J163554.2+661225 (vol 704, pg 1506, 2009). ASTROPHYSICAL JOURNAL.
• Rauscher, B. J., Stahle, C., Hill, R. J., Greenhouse, M., Beletic, J., Babu, S., Blake, P., Cleveland, K., Cofie, E., Eegholm, B., Engelbracht, C. W., Hall, D. N., Hoffman, A., Jeffers, B., Jhabvala, C., Kimble, R. A., Kohn, S., Kopp, R., Lee, D., , Leidecker, H., et al. (2000, JUN). Commentary: JWST near-infrared detector degradation-finding the problem, fixing the problem, and moving forward. AIP ADVANCES.
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  The James Webb Space Telescope (JWST) is the successor to the Hubble Space Telescope. JWST will be an infrared-optimized telescope, with an approximately 6.5 m diameter primary mirror, that is located at the Sun-Earth L2 Lagrange point. Three of JWST's four science instruments use Teledyne HgCdTe HAWAII-2RG (H2RG) near infrared detector arrays. During 2010, the JWST Project noticed that a few of its 5 mu m cutoff H2RG detectors were degrading during room temperature storage, and NASA chartered a "Detector Degradation Failure Review Board" (DD-FRB) to investigate. The DD-FRB determined that the root cause was a design flaw that allowed indium to interdiffuse with the gold contacts and migrate into the HgCdTe detector layer. Fortunately, Teledyne already had an improved design that eliminated this degradation mechanism. During early 2012, the improved H2RG design was qualified for flight and JWST began making additional H2RGs. In this article, we present the two public DD-FRB "Executive Summaries" that: (1) determined the root cause of the detector degradation and (2) defined tests to determine whether the existing detectors are qualified for flight. We supplement these with a brief introduction to H2RG detector arrays, some recent measurements showing that the performance of the improved design meets JWST requirements, and a discussion of how the JWST Project is using cryogenic storage to retard the degradation rate of the existing flight spare H2RGs. Copyright 2012 Author(s). This article is distributed under a Creative Commons Attribution 3.0 Unported License. [http://dx.doi.org/10.1063/1.4733534]