J/A+A/672/A137 AGN and host galaxy co-evolution (Lopez+, 2023)
The miniJPAS survey: AGN and host galaxy co-evolution of X-ray selected sources.
Lopez I.E., Brusa M., Bonoli S., Shankar F., Acharya N., Laloux B.,
Dolag K., Georgakakis A., Lapi A., Ramos Almeida C., Salvato M.,
Chaves-Montero J., Coelho P., Diaz-Garcia L.A., Fernandez-Ontiveros J.A.,
Hernan-Caballero A., Gonzalez Delgado R.M., Marquez I., Povic M., Soria R.,
Queiroz C., Rahna P.T., Abramo R., Alcaniz J., Benitez N., Carneiro S.,
Cenarro J., Cristobal-Hornillos D., Dupke R., Ederoclite A.,
Lopez-Sanjuan C., Marin-Franch A., Mendes de Oliveira C., Moles M.,
Sodre L.Jr., Taylor K., Varela J., Ramio H.V.
<Astron. Astrophys. 672, A137 (2023)>
=2023A&A...672A.137L 2023A&A...672A.137L (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Redshifts ; Photometry, SDSS
Keywords: galaxies: evolution - galaxies: active - galaxies: nuclei -
galaxies: photometry - quasars: supermassive black holes
Abstract:
Studies indicate strong evidence of a scaling relation in the local
Universe between the supermassive black hole mass (MBH) and the
stellar mass of their host galaxies (M*). They even show similar
histories across cosmic times of their differential terms: the star
formation rate (SFR) and black hole accretion rate (BHAR). However, a
clear picture of this coevolution is far from being understood.
We selected an X-ray sample of active galactic nuclei (AGN) up to
z=2.5 in the miniJPAS footprint. Their X-ray to infrared spectral
energy distributions (SEDs) have been modeled with the CIGALE code,
constraining the emission to 68 bands, from which 54 are the narrow
filters from the miniJPAS survey. For a final sample of 308 galaxies,
we derived their physical properties, such as their M*, SFR, star
formation history (SFH), and the luminosity produced by the accretion
process of the central BH (LAGN). For a subsample of 113 sources, we
also fit their optical spectra to obtain the gas velocity dispersion
from the broad emission lines and estimated the MBH. We calculated the
BHAR in physical units depending on two radiative efficiency regimes.
We find that the Eddington ratios (Edd) and its popular proxy (LX/M*)
have a difference of 0.6dex, on average, and a KS test indicates that
they come from different distributions. Our sources exhibit a
considerable scatter on the MBH-M* scaling relation, which can
explain the difference between Edd and its proxy.
We also modeled three evolution scenarios for each source to recover
the integral properties at z=0. Using the SFR and BHAR, we show a
notable diminution in the scattering between MBH-M*. For the last
scenario, we considered the SFH and a simple energy budget for the AGN
accretion, and we retrieved a relation similar to the calibrations
known for the local Universe.
Our study covers 1deg2 in the sky and is sensitive to biases in
luminosity. Nevertheless, we show that, for bright sources, the link
between the differential values (SFR and BHAR) and their decoupling
based on an energy limit is the key that leads to the local MBH-M*
scaling relation. In the future, we plan to extend this methodology to
a thousand degrees of the sky using JPAS with an X-ray selection from
eROSITA, to obtain an unbiased distribution of BHAR and Eddington
ratios.
Description:
We present the sources and physical parameters derived from our work.
The sources also have extra information, e.g., the magnitude in the r
band and X-ray luminosities from literature. The physical parameters
were obtained through a SED fitting with 68 bands, covering from X-ray
to mid-IR. Black hole masses were obtained by fitting the broad line
region of the source spectra and using the sigma-BH mass relation.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 60 347 Sources catalog
table6.dat 90 309 Physical parameters
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See also:
https://www.j-pas.org/datareleases/minijpas_public_data_release_pdr201912 :
MiniJ-PAS Public Data Release (PDR201912)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- ID ID used in this work
(aegis_NNN, egs_NNNN or xmmrm_NNNN)
12- 21 A10 --- JPAS ID used in miniJPAS catalog (NNNN-NNNNN)
23- 29 F7.3 deg RAdeg Right ascension of the optical/IR counterpart
(J2000)
31- 36 F6.3 deg DEdeg Declination of the optical/IR counterpart
(J2000)
38- 42 F5.3 --- zsp Spectroscopic redshift
44- 49 F6.3 mag rmag r band magnitude from SDSS
51- 55 F5.2 [10-7W] logLX ? log luminosity in the 2-10keV band
57- 60 F4.1 [cm-2] logNH log intrinsic hydrogen column density
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- ID ID used in this work
14- 18 F5.2 [Msun] logMstar log stellar mass (1)
23- 26 F4.2 [Msun] e_logMstar Error on log stellar mass
28- 34 F7.2 Msun/yr SFR Star formation rate (1)
37- 42 F6.2 Msun/yr e_SFR Error on star formation rate
47- 50 F4.2 [Msun] logMBH ? log black hole mass (2)
55- 58 F4.2 [Msun] e_logMBH ? Error on log black hole mass
62- 66 F5.2 [10-7W] logLAGN log bolometric AGN luminosity
71- 74 F4.2 [10-7W] e_logLAGN Error on log bolometric AGN luminosity
79- 82 F4.2 Msun/yr BHAR ? Black hole accretion rate (3)
86- 90 F5.2 --- logEdd ? log Eddington ratio
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Note (1): logMstar, SFR and logLAGN were derived from the SED fitting.
Note (2): logMBH are derived from the spectral fitting.
Note (3): BHAR are calculated by Eq. 2.
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Acknowledgements:
Ivan Lopez, ivanezequiel.lopez2(at)unibo.it
(End) Patricia Vannier [CDS] 23-Mar-2023