The X‐Ray Evolution of Early‐Type Galaxies in the Extended Chandra Deep Field–South

Lehmer, Bret; Brandt, W. N.; Alexander, D. M.; Bell, Eric F.; McIntosh, Daniel H.; Bauer, F. E.; Hasinger, G.; Mainieri, V.; Miyaji, Takeshi; Schneider, Donald P.; Steffen, A. T.

doi:10.1086/511297

Cited by 71 publications

(100 citation statements)

References 140 publications

(176 reference statements)

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“…Lehmer et al (2007) use the Chandra Deep Fields to study the AGN fraction in early-type galaxies (to z ∼ 0.7) and find evolution consistent with the (1 + z) 3 PLE model frequently fit to the luminosity function of X-rayselected AGNs (hereafter, the AGN XLF; Ueda et al 2003;Barger et al 2005;Hasinger et al 2005). Similar behavior is also noted in an earlier analysis of the stacked X-ray properties of early-type galaxies in a 1.4 deg 2 field in the NOAO Deep Wide-Field Survey (Brand et al 2005).…”

Section: Comparison To Previous Field Fractionsmentioning

confidence: 85%

THE FIELD X-RAY AGN FRACTION TOz= 0.7 FROM THECHANDRAMULTIWAVELENGTH PROJECT AND THE SLOAN DIGITAL SKY SURVEY

Haggard

Green

Anderson

et al. 2010

ApJ

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We employ the Chandra Multiwavelength Project (ChaMP) and the Sloan Digital Sky Survey (SDSS) to study the fraction of X-ray-active galaxies in the field to z = 0.7. We utilize spectroscopic redshifts from SDSS and ChaMP, as well as photometric redshifts from several SDSS catalogs, to compile a Parent sample of more than 100,000 SDSS galaxies and nearly 1600 Chandra X-ray detections. Detailed ChaMP volume completeness maps allow us to investigate the local fraction of active galactic nuclei (AGNs), defined as those objects having broadband X-ray luminosities L X (0.5-8 keV) 10 42 erg s −1 , as a function of absolute optical magnitude, X-ray luminosity, redshift, mass, and host color/morphological type. In five independent samples complete in redshift and i-band absolute magnitude, we determine the field AGN fraction to be between 0.16% ± 0.06% (for z 0.125 and −18 > M i > −20) and 3.80% ± 0.92% (for z 0.7 and M i < −23). We find excellent agreement between our ChaMP/SDSS field AGN fraction and the Chandra cluster AGN fraction, for samples restricted to similar redshift and absolute magnitude ranges: 1.19% ± 0.11% of ChaMP/SDSS field galaxies with 0.05 < z < 0.31 and absolute R-band magnitude more luminous than M R < −20 are AGNs. Our results are also broadly consistent with measures of the field AGN fraction in narrow, deep fields, though differences in the optical selection criteria, redshift coverage, and possible cosmic variance between fields introduce larger uncertainties in these comparisons.

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Section: Comparison To Previous Field Fractionsmentioning

confidence: 85%

THE FIELD X-RAY AGN FRACTION TOz= 0.7 FROM THECHANDRAMULTIWAVELENGTH PROJECT AND THE SLOAN DIGITAL SKY SURVEY

Haggard

Green

Anderson

et al. 2010

ApJ

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“…However, successive generations of X-ray telescopes with improved sensitivity, larger effective areas, and superior spatial resolution are now beginning to allow a more in-depth study of the hotgas component in unprecedented detail, which in turn sheds new light on the formation history of galaxies. Using the excellent angular resolution of the Chandra X-ray telescope, studies are directly detecting and isolating the X-ray emission from stellar processes such as the low-mass X-ray binary population that have plagued the previous generation of X-ray telescopes, particularly in the low stellar mass regime (e.g., Sivakoff et al 2004;Boroson et al 2011;Lehmer et al 2014), as well as exploring the X-ray halos in early-type galaxies as a function of cosmic time (e.g., Lehmer et al 2007;Civano et al 2014;Paggi et al 2015) and probing the thermal gas content (e.g., Diehl & Statler 2007;Jeltema et al 2008;Memola et al 2009;Bogdán et al 2012aBogdán et al , 2012bKim & Fabbiano 2013Su et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

Goulding

Greene

et al. 2016

ApJ

115

156

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Studies of the physical properties of local elliptical galaxies are shedding new light on galaxy formation. Here we present the hot-gas properties of 33 early-type systems within the MASSIVE galaxy survey that have archival Chandra X-ray observations, and we use these data to derive X-ray luminosities (L X,gas ) and plasma temperatures (T gas ) for the diffuse gas components. We combine this with the ATLAS 3D survey to investigate the X-ray-optical properties of a statistically significant sample of early-type galaxies across a wide range of environments. When X-ray measurements are performed consistently in apertures set by the galaxy stellar content, we deduce that all early types (independent of galaxy mass, environment, and rotational support) follow a universal scaling law such that µL T X,gas gas 4.5 . We further demonstrate that the scatter in L X,gas around both K-band luminosity (L K ) and the galaxy stellar velocity dispersion (s e ) is primarily driven by T gas , with no clear trends with halo mass, radio power, or angular momentum of the stars. It is not trivial to tie the gas origin directly to either stellar mass or galaxy potential. Indeed, our data require a steeper relation between L L , K X,gas , and s e than predicted by standard mass-loss models. Finally, we find that T gas is set by the galaxy potential inside the optical effective radius. We conclude that within the innermost 10-30 kpc region, early types maintain pressure-supported hot gas, with a minimum T gas set by the virial temperature, but the majority show evidence for additional heating.

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“…Averaging the X-ray counts at the known positions of the targets enhances the signal-to-noise ratio (S/N) for source populations with fluxes below the detection limit. Through stacking, the relationship between X-rays and other galaxy properties (e.g., SFR, stellar mass, dust attenuation) has been investigated for low-redshift galaxies (z < 1.4; Ptak et al 2001;Hornschemeier et al 2002;Laird et al 2005;Lehmer et al 2007Lehmer et al , 2008Watson et al 2009;Symeonidis et al 2011), intermediate-redshift LBGs (1.5 < z < 3; Brandt et al 2001;Reddy & Steidel 2004), and distant LBGs (3 < z < 6; Brandt et al 2001;Laird et al 2006;Lehmer et al 2005b;Cowie et al 2012). These stacking studies highlight the use of X-rays from normal galaxies to study the star formation history of the universe.…”

Section: Introductionmentioning

confidence: 99%

THE X-RAY STAR FORMATION STORY AS TOLD BY LYMAN BREAK GALAXIES IN THE 4 Ms CDF-S

Basu-Zych

Lehmer

Hornschemeier

et al. 2012

ApJ

Self Cite

112

114

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We present results from deep X-ray stacking of >4000 high-redshift galaxies from z ≈ 1 to 8 using the 4 Ms Chandra Deep Field-South data, the deepest X-ray survey of the extragalactic sky to date. The galaxy samples were selected using the Lyman break technique based primarily on recent Hubble Space Telescope ACS and WFC3 observations. Based on such high specific star formation rates (sSFRs): log SFR/M * > −8.7, we expect that the observed properties of these Lyman break galaxies (LBGs) are dominated by young stellar populations. The X-ray emission in LBGs, eliminating individually detected X-ray sources (potential active galactic nucleus), is expected to be powered by X-ray binaries and hot gas. We find, for the first time, evidence of evolution in the X-ray/SFR relation. Based on X-ray stacking analyses for z < 4 LBGs (covering ∼90% of the universe's history), we find that the 2-10 keV X-ray luminosity evolves weakly with redshift (z) and SFR as log L X = 0.93 log(1 + z) + 0.65 log SFR + 39.80. By comparing our observations with sophisticated X-ray binary population synthesis models, we interpret that the redshift evolution of L X /SFR is driven by metallicity evolution in high mass X-ray binaries, likely the dominant population in these high sSFR galaxies. We also compare these models with our observations of X-ray luminosity density (total 2-10 keV luminosity per Mpc 3 ) and find excellent agreement. While there are no significant stacked detections at z 5, we use our upper limits from 5 z 8 LBGs to constrain the supermassive black hole accretion history of the universe around the epoch of reionization.

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The X‐Ray Evolution of Early‐Type Galaxies in the Extended Chandra Deep Field–South

Cited by 71 publications

References 140 publications

THE FIELD X-RAY AGN FRACTION TOz= 0.7 FROM THECHANDRAMULTIWAVELENGTH PROJECT AND THE SLOAN DIGITAL SKY SURVEY

THE FIELD X-RAY AGN FRACTION TOz= 0.7 FROM THECHANDRAMULTIWAVELENGTH PROJECT AND THE SLOAN DIGITAL SKY SURVEY

The Massive Survey. Iv. The X-Ray Halos of the Most Massive Early-Type Galaxies in the Nearby Universe

THE X-RAY STAR FORMATION STORY AS TOLD BY LYMAN BREAK GALAXIES IN THE 4 Ms CDF-S

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