J/A+A/590/A80 2-10keV luminosity function of AGN (Ranalli+, 2016)
The 2-10 keV unabsorbed luminosity function of AGN from the LSS, CDFS, and
COSMOS surveys.
Ranalli P., Koulouridis E., Georgantopoulos I., Fotopoulou S., Hsu L.-T.,
Salvato M., Comastri A., Pierre M., Cappelluti N., Carrera F.J.,
Chiappetti L., Clerc N., Gilli R., Iwasawa K., Pacaud F., Paltani S.,
Plionis E., Vignali C.
<Astron. Astrophys. 590, A80 (2016)>
=2016A&A...590A..80R 2016A&A...590A..80R (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; X-ray sources ; Models
Keywords: surveys - galaxies: active - X-rays: general - methods: statistical
Abstract:
The XMM-Large scale structure (XMM-LSS), XMM-Cosmological evolution
survey (XMM-COSMOS), and XMM-Chandra deep field south (XMM-CDFS)
surveys are complementary in terms of sky coverage and depth.
Together, they form a clean sample with the least possible variance in
instrument effective areas and point spread function. Therefore this
is one of the best samples available to determine the 2-10keV
luminosity function of active galactic nuclei (AGN) and their
evolution. The samples and the relevant corrections for incompleteness
are described. A total of 2887 AGN is used to build the LF in the
luminosity interval 1042-1046erg/s and in the redshift interval
0.001-4. A new method to correct for absorption by considering the
probability distribution for the column density conditioned on the
hardness ratio is presented.
Description:
The XMM-LSS, XMM-CDFS, and XMM-COSMOS are three surveys with
complementary properties in terms of luminosity and redshift coverage.
We used these three surveys to derive Bayesian estimates of the
unabsorbed luminosity function (LF) of AGN in the 2-10keV band. The
LF estimates are presented as a set of samples from the posterior
probability distribution of the LF parameters. The LF is parameterised
as a double power-law, with either the luminosity and density
evolution (LADE) model, or the luminosity-dependent density evolution
(LDDE) model. The double power-law is described by Eq.(10) in the
paper. The LADE and LDDE models are described by Eqs.(11-14) and
Eqs.(15-17), respectively. A Fortran 2008 implementation of these
models can be found in file src2/lumf_funcs.f90 of the LFTools
package, in the classes doublepowerlaw, ladevol, and lddevol (see the
paper).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
lade-c.dat 166 7565 LF samples from XMM-CDFS, LADE model
lade-k.dat 166 7007 LF samples from XMM-COSMOS, LADE model
lade-l.dat 166 7050 LF samples from XMM-LSS, LADE model
lade-lck.dat 166 7066 LF samples from all surveys together, LADE model
ldde-c.dat 166 7622 LF samples from XMM-CDFS, LDDE model
ldde-k.dat 166 8450 LF samples from XMM-COSMOS, LDDE model
ldde-l.dat 166 7749 LF samples from XMM-LSS, LDDE model
ldde-lck.dat 166 7403 LF samples from all surveys together, LDDE model
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Byte-by-byte Description of file: lade-*.dat ldde-*.dat
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Bytes Format Units Label Explanations
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1- 21 E21.18 --- norm Normalisation (1)
23- 43 E21.18 --- gamma1 Exponent of the first branch of the power-law
45- 65 E21.18 --- gamma2 Exponent of the second branch of the power-law
67- 82 F16.13 [10-7W] Lstar Knee luminosity of the LF
84-100 F17.15 --- zc Critical redshift
102-122 F21.18 --- p1 First luminosity evolution slope
124-144 E21.18 --- p2 Second luminosity evolution slope
146-166 E21.18 --- d Density evolution slope
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Note (1): The values in the table are defined as: norm=6+log10(A) where A is
the normalisation defined in Eq.(10) of the paper.
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Acknowledgements:
Piero Ranalli, piero(at)astro.lu.se
(End) Piero Ranalli [Lund Observatory], Patricia Vannier [CDS] 12-Feb-2016