J/ApJS/235/39 Jet properties of γ-ray-loud 3FGL AGNs (Chen, 2018)
On the jet properties of γ-ray-loud active galactic nuclei.
Chen L.
<Astrophys. J. Suppl. Ser., 235, 39 (2018)>
=2018ApJS..235...39C 2018ApJS..235...39C
ADC_Keywords: Active gal. nuclei; Gamma rays; Magnetic fields; Redshifts
Keywords: BL Lacertae objects: general ; galaxies: active ; galaxies: jets ;
quasars: general ; radiation mechanisms: non-thermal
Abstract:
Based on broadband spectral energy distributions (SEDs), we estimate
the jet physical parameters of 1392 γ-ray-loud active galactic
nuclei (AGNs), the largest sample so far. The (SED) jet power and
magnetization parameter are derived for these AGNs. Out of these
sources, the accretion disk luminosity of 232 sources and (extended)
kinetic jet powers of 159 sources are compiled from archived papers.
We find the following. (1) Flat-spectrum radio quasars (FSRQs) and BL
Lacs are well separated by Γ=-0.127logLγ+8.18 in the
γ-ray luminosity versus photon index plane with a success rate
of 88.6%. (2) Most FSRQs present a (SED) jet power larger than the
accretion power, which suggests that the relativistic jet-launching
mechanism is dominated by the Blandford-Znajek process. This result
confirms previous findings. (3) There is a significant anticorrelation
between jet magnetization and a ratio of the (SED) jet power to the
(extended) kinetic jet power, which, for the first time, provides
supporting evidence for the jet energy transportation theory: a high-
magnetization jet may more easily transport energy to a large scale
than a low-magnetization jet.
Description:
Fan+ (2016, J/ApJS/226/20) successfully obtained the broadband SED of
1392 blazars (461 FSRQs, 620 BL Lacs, and 311 BCUs). They employed a
log-parabolic function,
log(νFν)=-P1(logν-logνp)2+log(νpFνp), to
fit the SED; therefore, the synchrotron peak frequency (νp),
spectral curvature (P1), and peak flux (νpFνp) are
obtained. Of the total number of blazars, 999 have measured redshifts.
In this paper, we will study the jet physical properties of the 1392
blazars.
The data regarding the γ-ray (i.e., photon index and luminosity)
are compiled from Acero+ (2015, J/ApJS/218/23) and Ackermann+ (2015,
J/ApJ/810/14).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 80 1392 AGN jet physical parameters
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See also:
J/ApJS/123/79 : Third EGRET catalog (3EG) (Hartman+, 1999)
J/AJ/130/1418 : AGN jet kinematics (Jorstad+, 2005)
J/ApJS/166/470 : SDSS-Spitzer type I QSOs IR photometry (Richards+, 2006)
J/MNRAS/379/260 : X-ray clusters with radio emission (Magliocchetti+, 2007)
J/ApJ/657/706 : EGRET blazar gamma-ray spectrum (Nandikotkur+, 2007)
J/A+A/488/867 : Synchrotron peak frequency of 135 AGN (Nieppola+, 2008)
J/ApJ/700/597 : FERMI LAT detected blazars (Abdo+, 2009)
J/ApJ/716/30 : SED of Fermi bright blazars (Abdo+, 2010)
J/ApJ/715/429 : First Fermi-LAT AGN catalog (1LAC) (Abdo+, 2010)
J/ApJ/743/171 : The 2LAC catalog (Ackermann+, 2011)
J/ApJ/740/98 : Synchroton peak for blazars & radio galaxies (Meyer+, 2011)
J/ApJS/194/45 : QSO properties from SDSS-DR7 (Shen+, 2011)
J/other/Sci/338.355 : 1.3mm VLBI detections of M87 (Doeleman+, 2012)
J/other/Sci/338.1445 : Relativistic jets from BH systems (Nemmen+, 2012)
J/ApJ/748/49 : Opt. spectroscopy of 1LAC broad-line blazars (Shaw+, 2012)
J/AJ/146/120 : MOJAVE. X. Parsec-scale kinematics of AGNs (Lister+, 2013)
J/other/RAA/14.1135 : Doppler factor for a Fermi blazar sample (Fan+, 2014)
J/other/Nat/515.376 : Power of relativistic jets in blazars (Ghisellini+, 2014)
J/ApJS/218/23 : Fermi LAT third source catalog (3FGL) (Acero+, 2015)
J/ApJ/810/14 : Third catalog of LAT-detected AGNs (3LAC) (Ackermann+, 2015)
J/MNRAS/448/1060 : Fermi/LAT broad emission line blazars (Ghisellini+, 2015)
J/ApJ/798/134 : MOJAVE. XII. Acceleration of blazar jets (Homan+, 2015)
J/ApJS/226/20 : X-ray, opt. & radio SEDs of Fermi blazars (Fan+, 2016)
J/A+A/591/A130 : Dynamic SEDs of southern blazars - DSSB (Krauss+, 2016)
J/ApJ/835/L38 : Fermi blazars with Doppler factors (Fan+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- 3FGL 3FGL Name (JHHMM.m+DDMM)
14- 14 A1 --- f_3FGL [*] Flag on blazar type (1)
16- 20 F5.3 --- z [0.002/3.2]? redshift
22- 23 A2 --- Cl Class (2)
25- 28 F4.2 [-] log(E) [2.3/7] Log of electron peak energy
30- 33 F4.2 --- b [0.1/2.1] Curvature of electron energy
distribution
35- 38 F4.1 [cm] logR [15.4/17.4] log of radius of the emission
sphere
40- 43 F4.1 --- delta [1/99.5] Doppler factor
45- 49 F5.2 [10-4T] log(B) [-4.5/3.5] Log of strength of magnetic
field; in gauss units
51- 54 F4.1 [10-7W] logPjet [42.8/50.7] log of jet (SED) power;
in erg/s units
56- 60 F5.2 [-] log(sig) [-7.7/8.5] log of magnetization parameter (3)
62- 66 F5.2 [-] log(eta) [-0.4/0.6]? Ratio of jet SED power to
(extended) jet kinetic power
68- 71 F4.2 [Msun] logM [6.5/10]? Available log of BH mass
73- 77 F5.2 [10-7W] logLd [42.7/47.5]? Available log of disk
luminosity; in units of erg/s
79- 80 A2 --- Model Model (4)
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Note (1):
* = Blazars having extreme Doppler factors (δ<1 or δ>100).
Therefore we instead use the median values (δm∼14.3 for BL Lacs
and δm∼10.7 for FSRQs) to calculate other jet parameters
(see text for details).
Note (2): Class of the source as follows:
UF = Blazar candidate of uncertain type (BCU) classified as FSRQs
(128 occurrences);
UB = Blazar candidate of uncertain type (BCU) classified as BL Lacs
(183 occurrences);
CF = Confirmed FSRQs (461 occurrences);
CB = Confirmed BL Lacs (620 occurrences).
Note (3): We define a magnetization parameter as the ratio of energy densities
between the magnetic field and relativistic electrons σ=UB/Ue
(also called the equipartition parameter) where UB =B2/8π is the
magnetic field energy density and Ue is the electron energy density.
Note (4): Model used in this calculation as follows:
ST = synchrotron self-Compton (SSC)/Thomson;
SK = synchrotron self-Compton (SSC)/Klein-Nishina (KN);
ET = external inverse Compton "EC"/Thomson;
EK = external inverse Compton "EC"/Klein-Nishina (KN).
See section 3 for further explanations.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 24-Aug-2018