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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
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:
FileName Lrecl Records Explanations
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
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.
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
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))
Note (1): or spectral slope of the log parabola model at the pivot energy.
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
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.
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)
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.
History: From electronic version of the journal Acknowledgements: Vaidehi S. Paliya [Clemson University, USA]
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 06-Jul-2018
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