J/A+A/684/A19 The XXL Survey. LII. (Slaus+, 2024)
The XXL Survey. LII. The evolution of radio AGN luminosity function determined
via parametric methods from GMRT, ATCA, VLA and Cambridge interferometer
observations.
Slaus B., Smolcic V., Ivezic Z., Fotopoulou S., Willott C.J., Pendo P.,
Vignali C., Chiappetti L., Pierre M.
<Astron. Astrophys. 684, A19 (2024)>
=2024A&A...684A..19S 2024A&A...684A..19S (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, radio ; Radio continuum ; Radio sources
Keywords: galaxies: evolution - galaxies: active -
galaxies: luminosity function, mass function -
radio continuum: galaxies - galaxies: nuclei - galaxies: statistics
Abstract:
We model the evolution of active galactic nuclei (AGN) by constructing
their radio LFs. We used a set of surveys of varying area and depth,
namely, the deep COSMOS survey of 1916 AGN sources; the wide, shallow
3CRR, 7C, and 6CE surveys, together containing 356 AGN; and the
intermediate XXL-North and South fields consisting of 899 and 1484
sources, respectively. We also used the CENSORS, BRL, Wall & Peacock,
and Config surveys, respectively consisting of 150, 178, 233, and 230
sources. Together, these surveys account for 5446 AGN sources and
constrained the LFs at high redshift and over a wide range of
luminosities (up to z~=3 and log(L/W/Hz)∈[22,29]).
We concentrated on parametric methods within the Bayesian framework,
which allowed us to perform model selection between a set of different
models. By comparing the marginalised likelihoods and both the Akaike
information criterion and the Bayesian information criterion, we show
that the luminosity-dependent density evolution (LDDE) model fits the
data best, with evidence ratios varying from 'strong' (>10) to
'decisive' (>100), according to the Jeffreys' interpretation.
The best-fitting model gives insight into the physical picture of AGN
evolution, where AGN evolve differently as a function of their radio
luminosity. We determined the number density, luminosity density, and
kinetic luminosity density as a function of redshift, and we observed
a flattening of these functions at higher redshifts, which is not
present in simpler models. We explain these trends by our use of the
LDDE model. Finally, we divided our sample into subsets according to
the stellar mass of the host galaxies in order to investigate a
possible bimodality in evolution. We found a difference in LF shape
and evolution between these subsets. All together, these findings
point to a physical picture where the evolution and density of AGN
cannot be explained well by simple models but require more complex
models either via AGN sub-populations, where the total AGN sample is
divided into sub-samples according to various properties, such as
optical properties and stellar mass, or via luminosity-dependent
functions.
Description:
The table presents a catalogue of 3479 radio sources compiled from
the COSMOS, XXL-S, 3CRR, 6C and 7C fields with their stellar masses.
The stellar masses for the COSMOS and XXL-S surveys was taken from the
respective catalogues. The remaining stellar masses were determined
from the K-band magnitudes. More details about this process can be
found in the paper. The spectral indices of the 3CRR, 6C and 7C fields
are complete and taken from the respective catalogues. The spectral
indices of the XXL-S field are filled with a value of -0.75 when
missing. The spectral indices of the COSMOS field are described in
COSMOS VLA (Smolcic et al., 2017A&A...602A...1S 2017A&A...602A...1S, Cat. J/A+A/602/A1).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 68 3479 Stellar mass catalogue
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See also:
IX/52 : XXL Survey. DR2 (Chiappetti+, 2018)
J/A+A/602/A1 : VLA-COSMOS 3 GHz Large Project (Smolcic+, 2017)
J/A+A/684/A18 : XLSSC NIKA2 sample images (Adam+, 2024)
Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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1- 30 A30 --- Name Name of the radio source
(COSMOSVLA3 JHHMMSS.ss+DDMMSS.s)
32- 36 F5.3 --- z Best available redshift for the source
38- 48 E11.5 mJy S1400MHz Source flux at 1400 MHz
50- 55 F6.3 --- alpha Spectral index of the source (1)
57- 62 F6.3 [Msun] logMstar Log stellar mass of the source
64- 68 A5 --- Survey Original survey (2)
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Note (1): set to mean of respective field when not available.
Note (2): References as follows:
C = COSMOS VLA, Smolcic et al., 2017A&A...602A...1S 2017A&A...602A...1S, Cat. J/A+A/602/A1
XXL-S = XXL-South ATCA, Butler et al., Paper XVIII, 2018A&A...620A...3B 2018A&A...620A...3B,
Cat. IX/52
3 = 3CRR, Willott et al., 1999MNRAS.309.1017W 1999MNRAS.309.1017W
6 = 6CE, Rawlings et al., 2001MNRAS.322..523R 2001MNRAS.322..523R
7 = 7C, Willott et al., 2001MNRAS.322..536W 2001MNRAS.322..536W
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Acknowledgements:
Bruno Slaus, bslaus(at)phy.hr
Lucio Chiappetti, lucio(at)lambrate.inaf.it
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(End) Bruno Slaus [Uni. Zagreb], Patricia Vannier [CDS] 27-Dec-2023