J/A+A/685/A97 AGN X-ray luminosity (3 ≤ z ≤ 6) (Pouliasis+, 2024)
Active galactic nuclei X-ray luminosity function and absorption function in
the Early Universe (3 ≤ z ≤ 6).
Pouliasis E., Ruiz A., Georgantopoulos I., Vito F., Gilli R., Vignali C.,
Ueda Y., Koulouridis E., Akiyama M., Marchesi S., Laloux B., Nagao T.,
Paltani S., Pierre M., Toba Y., Habouzit M., Vijarnwannaluk B., Garrel C.
<Astron. Astrophys. 685, A97 (2024)>
=2024A&A...685A..97P 2024A&A...685A..97P (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Redshifts ; X-ray sources
Keywords: galaxies: active - galaxies: high-redshift -
galaxies: luminosity function - mass function -
quasars: supermassive black holes - early Universe - X-rays: galaxies
Abstract:
The X-ray luminosity function (XLF) of active galactic nuclei (AGN) of
fers a robust tool to study the evolution and the growth of the
super-massive black-hole population over cosmic time. Owing to the
limited area probed by X-ray surveys, optical surveys are routinely
used to probe the accretion in the high redshift Universe z≥3.
However, optical surveys may be incomplete because they are strongly
affected by dust redenning. In this work, we derive the XLF and its
evolution at high redshifts (z≥3) using a large sample of AGNs
selected in different fields with various areas and depths covering a
wide range of luminosities. Additionally, we put the tightest yet
constraints on the absorption function in this redshift regime. In
particular, we use more than 600 soft X-ray selected (0.5-2keV)
high-z sources in the Chandra Deep fields, the Chandra COSMOS Legacy
survey and the XMM-XXL northern field. We derive the X-ray spectral
properties for all sources via spectral fitting, using a consistent
technique and model. For modeling the parametric form of the XLF and
the absorption function, we use a Bayesian methodology allowing us to
correctly propagate the uncertainties for the observed X-ray
properties of our sources and also the absorption effects. The
evolution of XLF is in agreement with a pure density evolution model
similar to what is witnessed at optical wavelengths, although a
luminosity dependent density evolution model cannot be securely ruled
out. A large fraction (∼60%) of our sources are absorbed by
column densities of NH≥1023cm-2, while ∼17% of the sources are
Compton-thick. Our results favor a scenario where both the
interstellar medium of the host and the AGN torus contribute to the
obscuration. The derived black hole accretion rate density is roughly
in agreement with the large-scale cosmological hydro-dynamical
simulations, if one takes into account the results that the X-ray AGN
are hosted by massive galaxies, while it differs from the one derived
using JWST data. The latter could be due to the differences in the AGN
and host-galaxy properties
Description:
Main properties of the high-redshift sources selected in the
XMM-XXL-N, CCLS and CDF-S/N fields and used in our analysis.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 110 807 Main properties of high-z sources
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See also:
J/ApJS/184/158 : Chandra COSMOS survey I. (Elvis+, 2009)
J/ApJS/224/15 : Improved 2Ms and 250ks Chandra catalogs (Xue+, 2016)
J/ApJ/819/62 : The COSMOS-Legacy Survey (CLS) catalog (Civano+, 2016)
J/ApJS/228/2 : Chandra Deep Field-South survey: 7Ms sources (Luo+, 2017)
Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Field Field (1)
11- 26 A16 --- ID Unique Identifier in each field (2)
28- 37 F10.6 deg RAdeg X-ray right ascension (J2000)
39- 48 F10.6 deg DEdeg X-ray declination (J2000)
50- 54 F5.3 --- z Redshift
56 I1 --- f_z [0/1] Redshift flag:
0 for photo-z, 1 for spec-z
58- 61 F4.2 --- P(z>3) Probability of a sources being at z>3
according to PDF(z)
63- 67 F5.2 [cm-2] logNH Hydrogen column density in logarithmic scale
69- 72 F4.2 [cm-2] e_logNH Hydrogen column density in logarithmic scale
lower error
74- 77 F4.2 [cm-2] E_logNH Hydrogen column density in logarithmic scale
upper error
79- 84 F6.2 [mW/m2] logFX Flux in 0.5-2 keV band in logarithmic scale
86- 89 F4.2 [mW/m2] e_logFX Flux in 0.5-2 keV band in logarithmic scale
lower error
91- 94 F4.2 [mW/m2] E_logFX Flux in 0.5-2 keV band in logarithmic scale
upper error
96-100 F5.2 [10-7J] logLX Luminosity in 2-10 keV band in logarithmic
scale
102-105 F4.2 [10-7J] e_logLX Luminosity in 2-10 keV band in logarithmic
scale lower error
107-110 F4.2 [10-7J] E_logLX Luminosity in 2-10 keV band in logarithmic
scale upper error
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Note (1): Fields are CCLS, CDF-N, CDF-S and XMM-XXL-N.
Note (2): cid_NNNNN ([ECV2009] NNNN, Elvis et al., 2009ApJS..184..158E 2009ApJS..184..158E,
Cat. J/ApJS/184/158) or lid_NNNNN ([CMC2016] lid NNNN,
Civano et al., 2016ApJ...819...62C 2016ApJ...819...62C, Cat. J/ApJ/819/62) for CCLS,
NNN ([LBX2017] NNN (NNN>300, Luo et al., 2017ApJS..228....2L 2017ApJS..228....2L,
Cat. J/ApJS/228/2) for CDF-S,
NNN ([XLB2016] CDFN NNN, Xue et al., 2016ApJS..224...15X 2016ApJS..224...15X, Cat. J/ApJS/224/15)
for CDF-N,
JHHMMSS.s+DDMMSS for XMM-XXL-N.
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Acknowledgements:
Ektoras Pouliasis, ektoraspou(at)gmail.com
(End) Patricia Vannier [CDS] 21-Feb-2024