J/ApJ/851/33 Multi-wavelength analysis of CGRaBS blazars (Paliya+, 2017)
General physical properties of CGRaBS blazars.
Paliya V.S., Marcotulli L., Ajello M., Joshi M., Sahayanathan S., Rao A.R.,
Hartmann D.
<Astrophys. J., 851, 33 (2017)>
=2017ApJ...851...33P 2017ApJ...851...33P
ADC_Keywords: Active gal. nuclei; Gamma rays; X-ray sources; Redshifts
Keywords: galaxies: active ; galaxies: jets ; gamma rays: galaxies ;
quasars: general
Abstract:
We present the results of a multi-frequency, time-averaged analysis of
blazars included in the Candidate Gamma-ray Blazar Survey catalog. Our
sample consists of 324 γ-ray detected (γ-ray loud) and 191
γ-ray undetected (γ-ray quiet) blazars; we consider all
the data up to 2016 April 1. We find that both the γ-ray loud
and γ-ray quiet blazar populations occupy similar regions in the
WISE color-color diagram, and γ-ray loud sources are brighter in
the radio and X-ray bands. A simple one-zone synchrotron
inverse-Compton emission model is applied to derive the physical
properties of both populations. We find that the central black hole
mass and accretion disk luminosity (Ldisk) computed from the
modeling of the optical-UV emission with a Shakura-Sunyaev disk
reasonably matches that estimated from the optical spectroscopic
emission-line information. A significantly larger Doppler boosting in
the γ-ray loud blazars is noted, and their jets are more
radiatively efficient. On the other hand, the γ-ray quiet
objects are more MeV-peaked and thus could be potential targets for
next-generation MeV missions. Our results confirm earlier findings
about the accretion-jet connection in blazars; however, many of the
γ-ray quiet blazars tend to deviate from the recent claim that
the jet power exceeds Ldisk in blazars. A broadband study,
considering a larger set of γ-ray quiet objects and also
including BL Lacs, will be needed to confirm/reject this hypothesis as
well as to verify the evolution of the powerful high-redshift blazars
into their low-power nearby counterparts.
Description:
Here, we present the results of our study on the blazars included in
the Candidate Gamma-ray Blazars Survey catalog (CGRaBS; Healey+ 2008,
J/ApJS/175/97).
To determine the γ-ray detected CGRaBS blazars, we cross-match
CGRaBS with all of the Fermi-LAT catalogs6 (3FGL, 2FGL, 1FGL, and 0FGL).
Further, we look into the HEASARC archive for the availability of
multi-wavelength data, particularly X-rays. In our final sample, we
keep only sources that have an existing multi-wavelength data set as
well as redshift information either given in Fermi-LAT AGN catalogs or
in CGRaBS.
Our results are based on the time-averaged study of CGRaBS sources, as
we have considered all of the available multi-wavelength data (up to
2016 April 1) without producing multiple SEDs with only contemporaneous
data for each source.
We use all of the data from the three instruments onboard the Swift
satellite: the Burst Alert Telescope (BAT, 15-150keV), the X-ray
Telescope (XRT, 0.3-10keV), and the Ultraviolet Optical Telescope
(UVOT), which can observe in six filters, V,B,U,UVW1,UVM2, and UVW2.
The XMM-Newton data (0.3-10keV) are analyzed using the Science
Analysis Software version 15.0.0.
We reduce the Chandra Advanced CCD Imaging Spectrometer data (ACIS,
0.3-7keV) using the package Chandra Interactive Analysis of
Observations (CIAO, version 4.9) and the associated calibration
database (v 4.7.3).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 109 310 The results of the spectral analysis of the Swift-XRT
data for the γ-ray loud blazars
table3.dat 109 173 *The results of the the Swift-XRT data analysis
for γ-ray quiet blazars
table5.dat 97 324 The SED parameters associated with the modeling of
the broadband emission in the γ-ray loud blazars
table6.dat 97 191 The SED parameters associated with the modeling of the
broadband emission in the γ-ray quiet blazars
table7.dat 40 324 The jet powers derived from the modeling of
the broadband emission in the γ-ray loud blazars
table8.dat 40 191 The jet powers derived from the modeling of the
broadband emission in the γ-ray quiet blazars
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Note on table3.dat: CGRaBS J0422+0219 (included in 1LAC,
Abdo+, 2010, J/ApJ/715/429) and CGRaBS J1508-1548 have been removed
from the final source list; addendum by the author - updated at CDS.
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See also:
VIII/65 : 1.4GHz NRAO VLA Sky Survey (NVSS) (Condon+ 1998)
VIII/76 : Leiden/Argentine/Bonn (LAB) Survey of Galactic HI (Kalberla+ 2005)
VII/273 : The Half Million Quasars (HMQ) catalogue (Flesch, 2015)
VII/274 : The Roma BZCAT - 5th edition (Massaro+, 2015)
J/ApJS/123/79 : Third EGRET catalog (3EG) (Hartman+, 1999)
J/ApJS/171/61 : Survey of Flat-Spectrum Radio Sources (Healey+, 2007)
J/ApJS/175/97 : CGRaBS: survey of γ-ray blazar cand. (Healey+, 2008)
J/ApJS/183/46 : Fermi/LAT bright gamma-ray source list (0FGL) (Abdo+, 2009)
J/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009)
J/ApJ/715/429 : First Fermi-LAT AGN catalog (1LAC) (Abdo+, 2010)
J/ApJ/740/98 : Synchroton peak for blazars & radio galaxies (Meyer+, 2011)
J/ApJS/194/45 : QSO properties from SDSS-DR7 (Shen+, 2011)
J/ApJ/748/68 : WISE IR colors of gamma-ray blazars (D'Abrusco+, 2012)
J/A+A/541/A160 : Planck + X/γ observations of blazars (Giommi+, 2012)
J/ApJS/199/31 : Fermi LAT second source catalog (2FGL) (Nolan+, 2012)
J/ApJ/748/49 : Opt. spectroscopy of 1LAC broad-line blazars (Shaw+, 2012)
J/other/RMxAA/48.9 : Opt. spectrosc. atlas of MOJAVE AGNs (Torrealba+, 2012)
J/ApJS/207/19 : Hard X-ray survey from Swift-BAT (Baumgartner+, 2013)
J/ApJ/780/73 : Redshifts of BL Lac objects from Fermi (Ajello+, 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/810/L9 : 1.5Jy MOJAVE AGN sample and 3FGL data (Lister+, 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/ApJS/224/26 : SEDs of Roma BZCAT blazars (Mao+, 2016)
J/A+A/591/A21 : Optical flux behaviour of Fermi blazars (Marchesini+, 2016)
J/ApJS/228/9 : Physical param. of ∼300000 SDSS-DR12 QSOs (Kozlowski, 2017)
Byte-by-byte Description of file: table[23].dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- CGRaBS CGRaBS object identifier (JHHMM+DDMM)
12- 16 F5.2 10+20/cm2 NH [0/33] Galactic neutral H column
density from Kalberla+ (2005, VIII/76)
18- 23 F6.2 ks Exp [0.4/622.8] Exposure time
25- 30 F6.2 10-12mW/m2 FX [0.02/197] Observe 0.3-10 keV flux
32- 37 F6.2 10-12mW/m2 b_FX [0/195] Lower limit boundary on FX
39- 44 F6.2 10-12mW/m2 B_FX [0.1/319] Upper limit boundary on FX
46- 50 F5.2 --- GammaX [-3/2.9] Power-law photon index (1)
52- 56 F5.2 --- b_GammaX [-2.3/2.5] Lower limit boundary on GammaX
58- 61 F4.2 --- B_GammaX [0/6.8] Upper limit boundary on GammaX
63- 67 F5.2 --- BetaX [-0.5/1.6]? Curvature parameter of
the log parabola model
69- 73 F5.2 --- b_BetaX [-0.6/1.2]? Lower limit boundary on BetaX
75- 79 F5.2 --- B_BetaX [-0.4/1.8]? Upper limit boundary on BetaX
81- 87 F7.2 --- stats [1.3/1009] Statistics of model fitting
89- 91 I3 --- dof [2/770] Degrees of freedom
93- 99 F7.2 [-] Pf-test [-111.6/0]? log of probability of null
hypothesis derived from the f-test
101-102 A2 --- Model Best fitted model (PL=power law or
LP=log parabola)
104-109 A6 --- Fit Adopted statistic (chi2 fitting or
C-statistics (Cash 1979ApJ...228..939C 1979ApJ...228..939C))
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Note (1): or spectral slope of the log parabola model at the pivot energy.
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Byte-by-byte Description of file: table[56].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- CGRaBS CGRaBS object identifier (JHHMM+DDMM)
12- 15 F4.2 --- z [0.02/5.5] Spectroscopic redshift
17- 20 F4.1 deg theta [2/10] Viewing angle
22- 26 F5.2 [Msun] logMbh [7.3/10.1] log black hole mass
28 A1 --- Type Adopted method to derive logMbh and
logLd (1)
30- 34 F5.2 [10-7W] logLd [42.2/48] log accretion disk luminosity;
in erg/s units
36- 40 F5.3 pc Rdis [0.004/0.7] Dissipation distance
42- 46 F5.3 pc RBLR [0.001/1.1] Broad line region (BLR) size
48- 51 F4.1 --- delta [5.7/22.5] Doppler factor
53- 54 I2 --- Gamma [5/22] Bulk Lorentz factor
56- 58 F3.1 10-4T B [0.1/6.4] Magnetic field strength; Gauss
60- 62 F3.1 --- p [1.3/2.3] Spectral slope of broken power-law
electron distribution before energy break
64- 66 F3.1 --- q [3.2/5.6] Spectral slope of broken power-law
electron distribution after energy break
68- 70 I3 --- gammaMin [1/200] Minimum Lorentz factor (2)
72- 77 I6 --- gammab [14/354179] Break Lortentz factor (2)
79- 85 I7 --- gammaMax [700/4000000] Maximum Lortentz factor (2)
87- 91 F5.2 [10-7J/cm3] logUe [-3.4/0.8]? log particle energy density;
in erg/cm3 units (3)
93- 97 F5.1 --- CD [0.1/183.5] Compton dominance
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Note (1): Code as follows:
A = assumed;
D = disk fitting;
E = empirical relation;
O = optical spectroscopy;
N = not used (see Table 9).
Note (2): Of the emitting electron distribution.
Note (3): A blank indicates a -infinity value.
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Byte-by-byte Description of file: table[78].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- CGRaBS CGRaBS object identifier (JHHMM+DDMM)
12- 16 F5.2 [10-7W] logPele [42.3/45.8] log electron power
18- 22 F5.2 [10-7W] logPmag [41.4/47] log magnetic power
24- 28 F5.2 [10-7W] logPrad [42.4/47.7] log radiative power
30- 34 F5.2 [10-7W] logPkin [42.7/48.4] log kinetic power
36- 40 F5.2 [10-7W] logPjet [43/48.4] log total jet power (1)
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Note (1): The jet power is just the sum of the electron, magnetic and
kinetic powers. All jet powers are evaluated for a two-sided jet.
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History:
From electronic version of the journal
Acknowledgements:
Vaidehi S. Paliya [Clemson University, USA]
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 06-Jul-2018