J/MNRAS/504/5726 IR lines of AGNs accretion disk (Fernandez-Ontiveros+, 2021)
X-ray binary accretion states in active galactic nuclei? Sensing the accretion
disc of supermassive black holes with mid-infrared nebular lines.
Fernandez-Ontiveros J.A., Munoz-Darias T.
<Mon. Not. R. Astron. Soc. 504, 5726-5740 (2021)>
=2021MNRAS.504.5726F 2021MNRAS.504.5726F (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, X-ray ; Active gal. nuclei ; Accretion ; Black holes ;
Nebulae ; Photometry, infrared
Keywords: accretion, accretion discs - galaxies: active - galaxies: jets -
quasars: emission lines - galaxies: Seyfert - infrared: ISM
Abstract:
Accretion states, which are universally observed in stellar mass black
holes in X-ray binaries, might be expected in active galactic nuclei
(AGN). This is the case at low luminosities, when the jet-corona
coupling dominates the energy output in both populations. Previous
attempts to extend this framework to a wider AGN population have been
extremely challenging due to heavy hydrogen absorption of the
accretion disc continuum and starlight contamination from the host
galaxies. We present the luminosity-excitation diagram (LED), based on
the [O IV]25.9um and [Ne II]12.8um mid-infrared nebular line
fluxes. This tool enables to probe the accretion disc contribution to
the ionizing continuum. When applied to a sample of 167 nearby AGN,
the LED recovers the characteristic q-shaped morphology outlined by
individual X-ray binaries during a typical accretion episode, allowing
us to tentatively identify the main accretion states. The soft state
would include broad-line Seyferts and about half of the Seyfert 2
population, showing highly excited gas and radio-quiet cores
consistent with disc-dominated nuclei, in agreement with previous
studies. The hard state mostly includes low-luminosity AGN
(≤ 10-3^ LEdd) characterized by low-excitation radio-loud nuclei and
a negligible disc contribution. The remaining half of Seyfert 2 nuclei
and the bright LINERs show low excitation at high accretion
luminosities and could be identified with the bright hard and
intermediate states. Their hosts show ongoing star formation in the
central kiloparsecs. We discuss the above scenario, its potential
links with the galaxy evolution picture, and the possible presence of
accretion state transitions in AGN, as suggested by the growing
population of changing-look quasars.
Description:
Our sample comprises mid-IR line fluxes of 162 AGN obtained with the
Spitzer/Infrared Spectrograph (IRS) using the high-spectral resolution
(HR) mode (10-37 um, R ∼ 600). These include Seyfert galaxies from the
12 micron sample of galaxies (Rush, Malkan & Spinoglio
1993ApJS...89....1R 1993ApJS...89....1R), whose mid-IR line fluxes were measured by
Tommasin et al. (2008ApJ...676..836T 2008ApJ...676..836T) and Tommasin et al.
(2010ApJ...709.1257T 2010ApJ...709.1257T). To cover the low-luminosity domain, we
incorporated the AGN spectroscopic data base in Fernandez-Ontiveros et
al. (2016ApJS..226...19F 2016ApJS..226...19F) plus Spitzer/IRS-HR measurements of LINERs
from Dudik, Satyapal & Marcu (2009ApJ...691.1501D 2009ApJ...691.1501D) and Goulding &
Alexander (2009MNRAS.398.1165G 2009MNRAS.398.1165G). Finally, five AGN observed with the
Short Wavelength Spectrometer (2.4 - 45 um, R ∼ 1000-2000; de Graauw
et al. 1996A&A...315L..49D 1996A&A...315L..49D) onboard ISO were added (Sturm et al.
2002A&A...393..821S 2002A&A...393..821S ; Verma et al. 2003A&A...403..829V 2003A&A...403..829V; Satyapal,
Sambruna & Dudik 2004A&A...414..825S 2004A&A...414..825S) for a total sample of 167 local
Universe AGN.
We present the table1.dat which is the entire sample (167 AGN). This
includes 55 Seyfert 1 nuclei (Sy1; red triangles in Fig. 4), 22
Seyfert 1 with hidden-broad lines (Sy1h; violet diamonds), 39 Seyfert
2 (Sy2; green squares), and 51 LINERs (blue circles). More details in
the section 2.2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 148 167 Sample of Seyfert and LINER galaxies compiled
for this study
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See also:
VII/157 : The Extended 12um galaxy sample (Rush+ 1993)
J/ApJS/226/19 : FIR spectra of AGNs from Herschel
(Fernandez-Ontiveros+, 2016)
J/MNRAS/398/1165 : AGN in nearby galaxies (Goulding+, 2009)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name Galxy name (Name)
16- 17 I2 h RAh Right ascension (J2000)
19- 20 I2 min RAm Right ascension (J2000)
22- 28 F7.4 s RAs Right ascension (J2000)
30 A1 --- DE- Sign of declination (J2000)
31- 32 I2 deg DEd Declination (J2000)
34- 35 I2 arcmin DEm Declination (J2000)
37- 43 F7.4 arcsec DEs Declination (J2000)
45- 53 F9.6 --- z Redshift (z)
55- 61 F7.2 Mpc D Distance (D) (2)
63- 68 A6 --- r_D Reference paper of D (RefD) (3)
70- 73 A4 --- SpType Spectral type of the galaxy (Type) (1)
75- 79 F5.3 [Msun] log(MBH) Black hole mass (logMssBH) (4)
81- 91 A11 --- r_log(MBH) Reference paper of MBH (RefM) (5)
93- 97 F5.2 [-] log(L) Luminosity in units of Eddington
luminosity LEdd (logL)
99-106 F8.3 10-17W/m2 [OIV] Integrated line fluxes of OIV
at 25.9 um ([OIV]25.9um)
108-113 F6.3 10-17W/m2 e_[OIV] Mean error on [OIV] (e_[OIV])
115-121 F7.3 10-17W/m2 [NeII] Integrated line fluxes of NeII
at 12.8 um ([NeII]12.8um)
123-128 F6.3 10-17W/m2 e_[NeII] Mean error on [NeII] (e_[NeII])
130-136 F7.2 10-17W/m2 PAH ? Integrated line fluxes of the
polycyclic aromatic hydrocarbon (PAH)
band at 11.3 um (PAH)
138-143 F6.2 10-17W/m2 e_PAH ? Mean error on PAH (e_PAH)
145-148 F4.2 [-] log(Frad/FX) ? Radio loudness defined as the flux
continuum ratio between 8.4 GHz
and 2-10 keV (logFrad/FX) (6)
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Note (1): Spectral type as:
S1 = Seyfert 1
S1h = Seyfert 1 with hidden broad lines
S2 = Seyfert 2
LIN = LINER
Note (2): Alternatively, distances are based on a flat-OmegaCDM cosmology
(H0 = 73 km/s/Mpc, Omegam = 0.27, Omegalambda = 0.73)
Note (3): Redshift-independent distances are used when available, see references
as follows:
CAC07 = Cackett et al. 2007MNRAS.380..669C 2007MNRAS.380..669C
CAN11 = Cantiello et al. 2011A&A...532A.154C 2011A&A...532A.154C
COR08 = Cortes et al. 2008ApJ...683...78C 2008ApJ...683...78C
DK02 = Dolphin & Kennicutt 2002AJ....123..207D 2002AJ....123..207D
EKH00 = Ekholm et al. 2000A&A...355..835E 2000A&A...355..835E
FER00 = Ferrarese et al. 2000ApJ...529..745F 2000ApJ...529..745F
FER07 = Ferrarese et al. 2007ApJ...654..186F 2007ApJ...654..186F
GAN13 = Ganeshalingam et al. 2013MNRAS.433.2240G 2013MNRAS.433.2240G
GER11 = Gerke et al. 2011ApJ...743..176G 2011ApJ...743..176G
JEN03 = Jensen et al. 2003ApJ...583..712J 2003ApJ...583..712J
JHA07 = Jha et al. 2007ApJ...659..122J 2007ApJ...659..122J
KAN03 = Kanbur et al. 2003A&A...411..361K 2003A&A...411..361K
MAN11 = Mandel et al. 2011ApJ...731..120M 2011ApJ...731..120M
MIE05 = Mieske et al. 2005A&A...438..103M 2005A&A...438..103M
MCQ16a = McQuinn et al. 2016AJ....152..144M 2016AJ....152..144M
MCQ16b = McQuinn et al. 2016ApJ...826...21M 2016ApJ...826...21M
MCQ17 = McQuinn et al. 2017AJ....154...51M 2017AJ....154...51M
NAS11 = Nasonova et al. 2011A&A...532A.104N 2011A&A...532A.104N
RAD11 = Radburn-Smith et al. 2011ApJS..195...18R 2011ApJS..195...18R
REI19 = Reid et al. 2019ApJ...886L..27R 2019ApJ...886L..27R
RES14 = Rest et al. 2014ApJ...795...44R 2014ApJ...795...44R
RIE11 = Riess et al. 2011ApJ...730..119R 2011ApJ...730..119R
SAB18 = Sabbi et al. 2018ApJS..235...23S 2018ApJS..235...23S
SAH06 = Saha et al. 2006ApJS..165..108S 2006ApJS..165..108S
SHA16 = Shappee et al. 2016ApJ...826..144S 2016ApJ...826..144S
SOR14 = Sorce et al. 2014MNRAS.444..527S 2014MNRAS.444..527S
SPR09 = Springob et al. 2007ApJS..172..599S 2007ApJS..172..599S, erratum ApJS, 182, 474
THE07 = Theureau et al. 2007A&A...465...71T 2007A&A...465...71T
TS97 = Tutui & Sofue 1997A&A...326..915T 1997A&A...326..915T
TUL88 = Tully 1988, Nearby Galaxy Catalog, Cat. VII/145
TUL09 = Tully et al. 2009AJ....138..323T 2009AJ....138..323T
TUL13 = Tully et al. 2013AJ....146...86T 2013AJ....146...86T
TUL16 = Tully et al. 2016AJ....152...50T 2016AJ....152...50T
WAN14 = Wang et al. 2014ApJ...793..108W 2014ApJ...793..108W
WEY14 = Weyant et al. 2014ApJ...784..105W 2014ApJ...784..105W
YOS14 = Yoshii et al. 2014ApJ...784L..11Y 2014ApJ...784L..11Y
Note (4): BH masses based on dynamical estimates or reverberation mapping are
used when available. Alternatively, the MBH-signma relation from Kormendy & Ho
2013ARA&A..51..511K 2013ARA&A..51..511K was adopted, using velocity dispersion measurements
compiled from the MBH literature
Note (5): MBH literature as follows :
BEN15 = Bentz & Katz 2015PASP..127...67B 2015PASP..127...67B
BET03 = Bettoni et al. 2003A&A...399..869B 2003A&A...399..869B
BOS15 = van de Bosch et al. 2015ApJS..218...10V 2015ApJS..218...10V
CAO04 = Cao & Rawlings 2004MNRAS.349.1419C 2004MNRAS.349.1419C
CAP09 = Cappellari et al. 2009ApJ...704L..34C 2009ApJ...704L..34C
CID04 = Cid Fernandes et al. 2004MNRAS.355..273C 2004MNRAS.355..273C
DAS11 = Dasyra et al. 2011ApJ...740...94D 2011ApJ...740...94D
DAV06 = Davies et al. 2006ApJ...646..754D 2006ApJ...646..754D
DAV07 = Davies et al. 2007ApJ...671.1388D 2007ApJ...671.1388D
DON14 = Dong et al. 2014ApJ...787L..20D 2014ApJ...787L..20D
FER96 = Ferrarese et al. 1996ApJ...470..444F 1996ApJ...470..444F
GEB11 = Gebhardt et al. 2011ApJ...729..119G 2011ApJ...729..119G
HO09 = Ho 2009ApJ...699..626H 2009ApJ...699..626H
HUR02 = Hure 2002A&A...395L..21H 2002A&A...395L..21H
HUR11 = Hure et al 2011A&A...530A.145H 2011A&A...530A.145H
JAR11 = Jardel et al. 2011ApJ...739...21J 2011ApJ...739...21J
KON08 = Kondratko et al. 2008ApJ...678...87K 2008ApJ...678...87K
K&H13 = Kormendy & Ho 2013ARA&A..51..511K 2013ARA&A..51..511K
KOS17 = Koss et al. 2017ApJ...850...74K 2017ApJ...850...74K
KUO11 = Kuo et al. 2011ApJ...727...20K 2011ApJ...727...20K
LAM17 = Lamperti et al. 2017MNRAS.467..540L 2017MNRAS.467..540L
LOD03 = Lodato & Bertin 2003A&A...398..517L 2003A&A...398..517L
McE95 = McElroy 1995ApJS..100..105M 1995ApJS..100..105M
NOW10 = Nowak et al. 2010MNRAS.403..646N 2010MNRAS.403..646N
OHT07 = Ohta et al. 2007ApJS..169....1O 2007ApJS..169....1O
RIF13 = Riffel et al. 2013MNRAS.429.2587R 2013MNRAS.429.2587R
SMI10 = Smirnova & Moiseev 2010MNRAS.401..307S 2010MNRAS.401..307S
SON12 = Son et al. 2012ApJ...757..140S 2012ApJ...757..140S
HyLEDA = HyperLEDA, Makarov et al. 2014A&A...570A..13M 2014A&A...570A..13M
VES02 = Vestergaard, 2002ApJ...571..733V 2002ApJ...571..733V
WIN09 = Winter et al. 2009ApJ...690.1322W 2009ApJ...690.1322W
WOL06 = Wold et al. 2006A&A...460..449W 2006A&A...460..449W
WOO05 = Woo et al. 2005ApJ...631..762W 2005ApJ...631..762W
Note (6): X-ray and radio fluxes are obtained from the NED database plus
additional measurements from:
X-ray: Bi et al. 2020ApJ...900..124B 2020ApJ...900..124B and Ricci et al. 2017ApJS..233...17R 2017ApJS..233...17R
Radio: Nagar et al. 2005A&A...435..521N 2005A&A...435..521N,
Saikia et al. 2018A&A...616A.152S 2018A&A...616A.152S and Thean et al. 2000MNRAS.314..573T 2000MNRAS.314..573T
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(End) Luc Trabelsi [CDS] 15-May-2024