J/A+A/689/A327 Low-luminosity radio AGNs catalogue (Wang+, 2024)
The fundamental plane of black hole activity for low-luminosity radio
active galactic nuclei across 1 < z < 4.
Wang Y., Wang T., Ho L.C., Zhong Y., Luo B.
<Astron. Astrophys. 689, A327 (2024)>
=2024A&A...689A.327W 2024A&A...689A.327W (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Galaxies, radio ; Galaxy catalogs
Keywords: galaxies: active - galaxies: general - galaxies: nuclei -
Abstract:
The fundamental plane of black hole activity describes the correlation
between radio luminosity (LR), X-ray luminosity (LX), and black
hole mass (MBH). It reflects a connection between the accretion disc
and the jet. However, the dependence of the fundamental plane on
various physical properties of active galactic nuclei (AGNs) and host
galaxies remains unclear, especially for low-luminosity AGNs, which is
important for understanding the accretion physics in AGNs. Here, we
explore the dependence of the fundamental plane on the radio loudness,
Eddington-ratio (lambdaEdd), redshift, and galaxy star formation
properties (star-forming galaxies and quiescent galaxies) across
0.1<z≤4 for radio AGNs. Based on current deep and large surveys, our
studies can extend to lower luminosities and higher redshifts. From
the deep and large multi-wavelength surveys in the GOODS-N, GOODS-S,
and COSMOS/UltraVISTA fields, we constructed a large and homogeneous
radio AGN sample consisting of 208 objects with available estimates
for LR and LX. Then we divided the radio AGN sample into 141
radio-quiet AGNs and 67 radio-loud AGNs according to the radio
loudness defined by the ratio of LR to LX, and explored the
dependence of the fundamental plane on different physical properties
of the two populations, separately. The ratio of LR to LX shows a
bimodal distribution that is well described by two single Gaussian
models. The cross point between these two Gaussian components
corresponds to a radio-loudness threshold of log (LR/LX)=-2.73.
The radio-quiet AGNs have a significantly larger Eddington ratio than
the radio-loud AGNs. Our radio-quiet and radio-loud AGNs show a
significantly different fundamental plane, which indicates a
significant dependence of the fundamental plane on the radio loudness.
For both radio-quiet and radio-loud AGNs, the fundamental plane shows
a significant dependence on lambda_Edd, but no dependence on redshift.
The fundamental plane shows a significant dependence on the galaxy
star formation properties for radio-quiet AGNs, while for radio-loud
AGNs this dependence disappears. The fundamental plane sheds important
light on the accretion physics and X-ray emission origins of central
engines. X-ray emission of radio-quiet AGNs at 0.01<lambdaEdd<0.1
are produced by a combination of advection-dominated accretion flow
(ADAF) and synchrotron radiation from the jet, while at
0.1<lambdaEdd<1 they mainly follow the synchrotron jet model. The
origins of X-ray emission of radio-loud AGNs are consistent with a
combination of ADAF and the synchrotron jet model at lambdaEdd<0.01,
agree with the synchrotron jet model at 0.01<lambdaEdd<0.1, and
follow a combination of the standard thin disc and a jet model at
lambdaEdd>0.1.
Description:
This work presents the radio AGN sample selected from the GOODS-N,
GOODS-S, and COSMOS/UltraVISTA fields, which consists of 208 objects
with available estimates for radio luminosity and X-ray luminosity.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 113 208 Radio AGN catalog with various physical properties
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See also:
J/ApJS/207/24 : GOODS-S CANDELS multiwavelength catalog (Guo+, 2013)
J/ApJ/853/172 : "Super-deblended" dust emission in galaxies. I. (Liu+, 2018)
J/ApJ/864/56 : "Super-deblended" dust emission in gal. II. COSMOS (Jin+, 2018)
J/ApJS/243/22 : CANDELS/SHARDS multiwavelength cat. in GOODS-N (Barro+, 2019)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Field [GOODSN, GOODSS, COSMOS] Survey name (1)
8- 15 I8 --- ID Source ID (2)
17- 26 F10.6 deg RAdeg Right ascension (J2000)
28- 37 F10.6 deg DEdeg Declination (J2000)
39- 44 F6.4 --- z redshift (3)
46- 47 A2 --- Rtype [RL RQ] Radio AGN type (RL or RQ) (4)
49- 55 F7.4 [10-7W] logLR Rest-frame 5GHz radio luminosity from AGN
(log scale) (5)
57- 62 F6.4 [10-7W] e_logLR Error on rest-frame 5GHz radio luminosity from
AGN (log scale)
64- 70 F7.4 [10-7W] logLX Rest-frame 2-10keV X-ray luminosity from AGN
(log scale) (6)
72- 77 F6.4 [10-7W] e_logLX Error on rest-frame 2-10keV X-ray luminosity
from AGN (log scale)
79- 84 F6.4 [Msun] logMBH Black hole mass (log scale) (7)
86- 91 F6.4 [Msun] e_logMBH Error on black hole mass (log scale)
93- 99 F7.4 --- logEdd Eddington ratio (log scale)
101-103 A3 --- Host-SF [SFG QG] Host galaxy star-formation properties
(SFG or QG) (8)
105-113 F9.4 [Gyr] logsSFR Specific star formation rate (log scale)
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Note (1): "GOODSN" for the GOODS-N field,
"GOODSS" for the GOODS-S field, [HSN2014] NNNNN in Simbad,
"COSMOS" for the COSMOS/UltraVISTA field.
Note (2): ID is from Liu et al. (2018, J/ApJ/853/172)
(same as Barro et al. 2019, J/ApJS/243/22) for the GOODS-N,
from Guo et al. (2013, J/ApJS/207/24) for the GOODS-S,
from Jin et al. (2018, J/ApJ/864/56) for the COSMOS.
Note (3): Redshifts were collected from
Liu et al. (2018, J/ApJ/853/172) for the GOODS-N,
from Guo et al. (2013, J/ApJS/207/24) for the GOODS-S,
from Jin et al. (2018, J/ApJ/864/56) for the COSMOS.
Note (4): "RQ" for radio-quiet AGN, "RL" for radio-loud AGN;
they are classified by the ratio of
rest-frame 5GHz radio luminosity from AGN (LR) to
rest-frame 2-10keV X-ray luminosity from AGN (LX).
Note (5): The rest-frame 5GHz radio luminosity from AGN had been subtracted
from the contribution from star formations.
Note (6): The rest-frame 2-10keV X-ray luminosity from AGN had been subtracted
from the contribution from X-ray binaries.
Note (7): Black hole masses were inferred from the stellar mass according to
the relation between stellar mass and black hole mass in
Greene et al. (2020ARA&A..58..257G 2020ARA&A..58..257G).
Note (8): "SFG" for star-forming galaxy, "QG" for quiescent galaxy;
they are classified by the UVJ selection criteria in
Schreiber et al. (2015A&A...575A..74S 2015A&A...575A..74S).
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Acknowledgements:
Yijun Wang, wangyijun(at)nju.edu.cn
(End) Patricia Vannier [CDS] 01-Jul-2024