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|Abstract:||We examine how the total X-ray luminosity correlates with stellar mass, stellar population, and redshift for a K-band limited sample of similar to 3500 galaxies at 0.5 < z < 2.0 from the NEWFIRM Medium Band Survey in the COSMOS field. The galaxy sample is divided into 32 different galaxy types, based on similarities between the spectral energy distributions. For each galaxy type, we further divide the sample into bins of redshift and stellar mass, and perform an X-ray stacking analysis using the Chandra COSMOS data. We find that full band X-ray luminosity is primarily increasing with stellar mass, and at similar mass and spectral type is higher at larger redshifts. When comparing at the same stellar mass, we find that the X-ray luminosity is slightly higher for younger galaxies (i.e., weaker 4000 angstrom breaks), but the scatter in this relation is large. We compare the observed X-ray luminosities to those expected from low-and high-mass X-ray binaries (XRBs). For blue galaxies, XRBs can almost fully account for the observed emission, while for older galaxies with larger 4000 angstrom breaks, active galactic nuclei (AGN) or hot gas dominate the measured X-ray flux. After correcting for XRBs, the X-ray luminosity is still slightly higher in younger galaxies, although this correlation is not significant. AGN appear to be a larger component of galaxy X-ray luminosity at earlier times, as the hardness ratio increases with redshift. Together with the slight increase in X-ray luminosity this may indicate more obscured AGNs or higher accretion rates at earlier times.|
|Electronic Publication Date:||10-Feb-2014|
|Citation:||Jones, Therese M, Kriek, Mariska, van Dokkum, Pieter G, Brammer, Gabriel, Franx, Marijn, Greene, Jenny E, Labbe, Ivo, Whitaker, Katherine E. (2014). X-RAY PROPERTIES OF K-SELECTED GALAXIES AT 0.5 < z < 2.0: INVESTIGATING TRENDS WITH STELLAR MASS, REDSHIFT AND SPECTRAL TYPE. ASTROPHYSICAL JOURNAL, 783 (10.1088/0004-637X/783/1/25|
|Type of Material:||Journal Article|
|Journal/Proceeding Title:||ASTROPHYSICAL JOURNAL|
|Version:||Final published version. Article is made available in OAR by the publisher's permission or policy.|
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