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Title:
Tracing the Mass-Dependent Star Formation History of Late-Type Galaxies using X-Ray Emission: Results from the Chandra Deep Fields
Authors:
Lehmer, B. D.; Brandt, W. N.; Alexander, D. M.; Bell, E. F.; Hornschemeier, A. E.; McIntosh, D. H.; Bauer, F. E.; Gilli, R.; Mainieri, V.; Schneider, D. P.; Silverman, J. D.; Steffen, A. T.; Tozzi, P.; Wolf, C.
Affiliation:
AA(Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802.; Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK.), AB(Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802.), AC(Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK.), AD(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany.), AE(Laboratory for X-Ray Astrophysics, NASA Goddard Space Flight Center, Code 662, Greenbelt, MD 20771.), AF(Astronomy Department, University of Massachusetts, 710 North Pleasant Street, Amherst, MA 01007.), AG(Columbia Astrophysics Laboratory, Columbia University, Pupin Laboratories, 550 West 120th Street, Room 1418, New York, NY 10027.), AH(Istituto Nazionale di Astrofisica (INAF)-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy.), AI(European Southern Observatory, Karl-Schwarschild-Strasse 2, D-85748 Garching, Germany.; Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching bei München, Germany.), AJ(Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802.), AK(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching bei München, Germany.; Institute of Astronomy, Department of Physics, Eidgenössische TechnischeHochschule, ETH Zurich, CH-8093, Switzerland.), AL(Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802.), AM(Istituto Nazionale di Astrofisica (INAF)-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy.), AN(Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK.)
Publication:
The Astrophysical Journal, Volume 681, Issue 2, pp. 1163-1182. (ApJ Homepage)
Publication Date:
07/2008
Origin:
UCP
ApJ Keywords:
Cosmology: Observations, Galaxies: Active, Galaxies: General, Galaxies: Spiral, Stars: Formation, Surveys, X-Rays: Galaxies, X-Rays: General
DOI:
10.1086/588459
Bibliographic Code:
2008ApJ...681.1163L

Abstract

We report on the X-ray evolution over the last ~9 Gyr of cosmic history (i.e., since z=1.4) of late-type galaxy populations in the Chandra Deep Field-North and Extended Chandra Deep Field-South (CDF-N and E-CDF-S, respectively; jointly CDFs) survey fields. Our late-type galaxy sample consists of 2568 galaxies, which were identified using rest-frame optical colors and HST morphologies. We utilized X-ray stacking analyses to investigate the X-ray emission from these galaxies, emphasizing the contributions from normal galaxies that are not dominated by active galactic nuclei (AGNs). Over this redshift range, we find significant increases (factors of ~5-10) in the X-ray-to-optical mean luminosity ratio (LX/LB) and the X-ray-to-stellar mass mean ratio (LX/M*) for galaxy populations selected by LB and M*, respectively. When analyzing galaxy samples selected via SFR, we find that the mean X-ray-to-SFR ratio (LX/SFR) is consistent with being constant over the entire redshift range for galaxies with SFR = 1-100 Msolar yr-1, thus demonstrating that X-ray emission can be used as a robust indicator of star formation activity out to z~1.4. We find that the star formation activity (as traced by X-ray luminosity) per unit stellar mass in a given redshift bin increases with decreasing stellar mass over the redshift range z = 0.2-1, which is consistent with previous studies of how star formation activity depends on stellar mass. Finally, we extend our X-ray analyses to Lyman break galaxies at z~3 and estimate that LX/LB at z~3 is similar to its value at z=1.4.
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