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Your search keyword '"Lubin, L. M."' showing total 2 results
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2 results on '"Lubin, L. M."'

1. SPITZER ULTRA FAINT SURVEY PROGRAM (SURFS UP). II. IRAC-DETECTED LYMAN-BREAK GALAXIES AT 6 less than or similar to z less than or similar to 10 BEHIND STRONG-LENSING CLUSTERS

Author

Huang, Kuang-Han, Bradac, Marusa, Lemaux, Brian C., Ryan, R. E., Hoag, Austin, Castellano, Marco, Amorin, Ricardo, Fontana, Adriano, Brammer, Gabriel B., Cain, Benjamin, Lubin, L. M., Merlin, Emiliano, Schmidt, Kasper B., Schrabback, Tim, Treu, Tommaso, Gonzalez, Anthony H., von Der Linden, Anja, Knight, Robert I., Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Argelander-Institut für Astronomie (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Department of Physics [Santa Barbara] (PHYSICS-UCSB), University of California [Santa Barbara] (UCSB), University of California-University of California, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), University of California [Santa Barbara] (UC Santa Barbara), and University of California (UC)-University of California (UC)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; We study the stellar population properties of the IRAC-detected 6 less than or similar to z less than or similar to 10 galaxy candidates from the Spitzer UltRa Faint SUrvey Program. Using the Lyman Break selection technique, we find a total of 17 galaxy candidates at 6 less than or similar to z less than or similar to 10 from Hubble Space Telescope images (including the full-depth images from the Hubble Frontier Fields program for MACS 1149 and MACS 0717) that have detections at signal-to-noise ratios \textgreater= 3 in at least one of the IRAC 3.6 and 4.5 mu m channels. According to the best mass models available for the surveyed galaxy clusters, these IRAC-detected galaxy candidates are magnified by factors of similar to 1.2-5.5. Due to the magnification of the foreground galaxy clusters, the rest-frame UV absolute magnitudes M-1600 are between -21.2 and -18.9 mag, while their intrinsic stellar masses are between 2 x 10(8)M(circle dot) and 2.9 x 10(9)M(circle dot). We identify two Ly alpha emitters in our sample from the Keck DEIMOS spectra, one at z(Ly alpha) = 6.76 (in RXJ 1347) and one at z(Ly alpha) = 6.32 (in MACS 0454). We find that 4 out of 17 z greater than or similar to 6 galaxy candidates are favored by z less than or similar to 1 solutions when IRAC fluxes are included in photometric redshift fitting. We also show that IRAC [3.6]-[4.5] color, when combined with photometric redshift, can be used to identify galaxies which likely have strong nebular emission lines or obscured active galactic nucleus contributions within certain redshift windows.

Published
2016

2. The Spitzer Extragalactic Representative Volume Survey (SERVS): Survey Definition and Goals

Author

E. A. Gonzalez-Solares, Roy R. Gal, Ray P. Norris, Luca Bizzocchi, Jamie Stevens, Huub Röttgering, S. A. Stanford, Marguerite Pierre, Giovanni Covone, Anna Sajina, Scott Chapman, A. M. J. Mortier, E. Dyke, D. Rigopoulou, Janine Pforr, Hugo Messias, S. Foucaud, A. Rettura, G. Parish, Steve Rawlings, S. J. Oliver, James Dunlop, H. C. Ferguson, Jose Afonso, N. Castro, Russell H. Taylor, Chris Simpson, Ian Smail, Bruno M. B. Henriques, Ross J. McLure, Nick Seymour, S. E. Ridgway, Lori M. Lubin, Tanya Urrutia, Jason Surace, Ismael Perez-Fournon, Antonio Cava, D. M. Nielsen, N. Dubois, M. Trichas, C. J. Lonsdale, Aprajita Verma, Gordon T. Richards, J. T. Falder, Minh Huynh, Philip Best, N. Christopher, James E. Geach, Jacqueline Hodge, R. H. Becker, David M. Alexander, E. van Kampen, Duncan Farrah, David L. Clements, Gordon K. Squires, Marco Grossi, A. Martinez-Sansigre, Alberto Franceschini, Alastair C. Edge, Mattia Vaccari, M. D. Lehnert, J. K. Grant, Peter A. Thomas, Masami Ouchi, Evanthia Hatziminaoglou, J.-S. Huang, Claudia Maraston, Gillian Wilson, Anthony C. S. Readhead, O. LeFevre, Mark Lacy, C. K. Xu, M. Kim, Gregory R. Zeimann, Samantha Hickey, A. K. Romer, Lucia Marchetti, Michael Rowan-Robinson, I. G. Rosebloom, Matt J. Jarvis, David Bonfield, Andreea Petric, J. C. Mauduit, Rob Ivison, Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), National Radio Astronomy Observatory [Charlottesville] (NRAO), National Radio Astronomy Observatory (NRAO), Department of Physics and Astronomy [Brighton] (DPA), University of Sussex, Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), Institute of Cosmology and Gravitation [Portsmouth] (ICG), University of Portsmouth, Dipartimento di Fisica e Astronomia 'Galileo Galilei', Università degli Studi di Padova = University of Padua (Unipd), University of the Western Cape (UWC), Visual servoing in robotics, computer vision, and augmented reality (Lagadic), Inria Sophia Antipolis - Méditerranée (CRISAM), Institut National de Recherche en Informatique et en Automatique (Inria)-Institut National de Recherche en Informatique et en Automatique (Inria)-Inria Rennes – Bretagne Atlantique, Institut National de Recherche en Informatique et en Automatique (Inria)-SIGNAUX ET IMAGES NUMÉRIQUES, ROBOTIQUE (IRISA-D5), Institut de Recherche en Informatique et Systèmes Aléatoires (IRISA), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université de Bretagne Sud (UBS)-École normale supérieure - Rennes (ENS Rennes)-Institut National de Recherche en Informatique et en Automatique (Inria)-Télécom Bretagne-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS)-Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université de Bretagne Sud (UBS)-École normale supérieure - Rennes (ENS Rennes)-Institut National de Recherche en Informatique et en Automatique (Inria)-Télécom Bretagne-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche en Informatique et Systèmes Aléatoires (IRISA), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université de Bretagne Sud (UBS)-École normale supérieure - Rennes (ENS Rennes)-Télécom Bretagne-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Univ California Davis] (Physics - UC Davis), University of California [Davis] (UC Davis), University of California (UC)-University of California (UC), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), National Optical Astronomy Observatory (NOAO), Observatório Astronómico de Lisboa, Centro de Astronomia e Astrofísica da Universidade de Lisboa (CAAUL), Universidade de Lisboa = University of Lisbon (ULISBOA), Department of Physics and Astronomy [Riverside], University of California [Riverside] (UC Riverside), Department of Physics [Montréal], McGill University = Université McGill [Montréal, Canada], International Centre for Radio Astronomy Research (ICRAR), The University of Western Australia (UWA)-Government of Western Australia-Curtin University [Perth], Planning and Transport Research Centre (PATREC)-Planning and Transport Research Centre (PATREC), CSIRO Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Department of Physics - Drexel University, Drexel University, Lawrence Livermore National Laboratory (LLNL), Department of Physics [Durham University], Durham University, Royal Observatory Edinburgh (ROE), University of Edinburgh, Instituto de Astrofisica de Canarias (IAC), Department of Physics [Oxford], University of Oxford, Astrophysics Group, Blackett Laboratory, Imperial College London-Imperial College London, Dipartimento di Scienze Fisiche [Naples], University of Naples Federico II = Università degli studi di Napoli Federico II, Institute for Computational Cosmology (ICC), Space Telescope Science Institute (STSci), National Taiwan Normal University (NTNU), University of Hawai'i [Honolulu] (UH), Department of Physics and Astronomy [Calgary], University of Calgary, European Southern Observatory (ESO), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [Madison], University of Wisconsin-Madison, Carnegie Institution for Science, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Caltech Department of Astronomy [Pasadena], Cerro Tololo Inter-American Observatory, Leiden Observatory [Leiden], Universiteit Leiden, Haverford College, Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), Leibniz Institute for Astrophysics Potsdam (AIP), Mauduit, J. C., Lacy, M., Farrah, D., Surace, J. A., Jarvis, M., Oliver, S., Maraston, C., Vaccari, M., Marchetti, L., Zeimann, G., Gonzalez Solares, E. A., Pforr, J., Petric, A. O., Henriques, B., Thomas, P. A., Afonso, J., Rettura, A., Wilson, G., Falder, J. T., Geach, J. E., Huynh, M., Norris, R. P., Seymour, N., Richards, G. T., Stanford, S. A., Alexander, D. M., Becker, R. H., Best, P. N., Bizzocchi, L., Bonfield, D., Castro, N., Cava, A., Chapman, S., Christopher, N., Clements, D. L., Covone, Giovanni, Dubois, N., Dunlop, J. S., Dyke, E., Edge, A., Ferguson, H. C., Foucaud, S., Franceschini, A., Gal, R. R., Grant, J. K., Grossi, M., Hatziminaoglou, E., Hickey, S., Hodge, J. A., Huang, J. S., Ivison, R. J., Kim, M., Lefevre, O., Lehnert, M., Lonsdale, C. J., Lubin, L. M., Mclure, R. J., Messias, H., Martinez Sansigre, A., Mortier, A. M. J., Nielsen, D. M., Ouchi, M., Parish, G., Perez Fournon, I., Pierre, M., Rawlings, S., Readhead, A., Ridgway, S. E., Rigopoulou, D., Romer, A. K., Rosebloom, I. G., Rottgering, H. J. A., Rowan Robinson, M., Sajina, A., Simpson, C. J., Smail, I., Squires, G. K., Stevens, J. A., Taylor, R., Trichas, M., Urrutia, T., van Kampen, E., Verma, A., Xu, C. K., Universita degli Studi di Padova, University of the Western Cape, CentraleSupélec-Télécom Bretagne-Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National de Recherche en Informatique et en Automatique (Inria)-École normale supérieure - Rennes (ENS Rennes)-Université de Bretagne Sud (UBS)-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-CentraleSupélec-Télécom Bretagne-Université de Rennes 1 (UR1), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-Institut de Recherche en Informatique et Systèmes Aléatoires (IRISA), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-École normale supérieure - Rennes (ENS Rennes)-Université de Bretagne Sud (UBS)-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA), Department of Physics [Davis], University of California-University of California, Universidade de Lisboa (ULISBOA), University of California [Riverside] (UCR), University of Oxford [Oxford], Università degli studi di Napoli Federico II, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Carnegie Institution for Science [Washington], and Universiteit Leiden [Leiden]

Subjects
Physics, evoluzione delle galassie, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Volume (computing), FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Quasar, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Spitzer Space Telescope, Space and Planetary Science, 0103 physical sciences, Galaxy formation and evolution, Chandra Deep Field South, survey astronomica, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the Spitzer Extragalactic Representative Volume Survey (SERVS), an 18 square degrees medium-deep survey at 3.6 and 4.5 microns with the post-cryogenic Spitzer Space Telescope to ~2 microJy (AB=23.1) depth of five highly observed astronomical fields (ELAIS-N1, ELAIS-S1, Lockman Hole, Chandra Deep Field South and XMM-LSS). SERVS is designed to enable the study of galaxy evolution as a function of environment from z~5 to the present day, and is the first extragalactic survey both large enough and deep enough to put rare objects such as luminous quasars and galaxy clusters at z>1 into their cosmological context. SERVS is designed to overlap with several key surveys at optical, near- through far-infrared, submillimeter and radio wavelengths to provide an unprecedented view of the formation and evolution of massive galaxies. In this paper, we discuss the SERVS survey design, the data processing flow from image reduction and mosaicing to catalogs, as well as coverage of ancillary data from other surveys in the SERVS fields. We also highlight a variety of early science results from the survey., 21 pages, 23 figures, published in PASP. This version differs slightly from PASP, mainly due to formatting issues. Figure 2 was also corrected from the previous version

Published
2012

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