J/ApJS/226/20 X-ray, opt. & radio SEDs of Fermi blazars (Fan+, 2016)
The spectral energy distributions of Fermi blazars.
Fan J.H., Yang J.H., Liu Y., Luo G.Y., Lin C., Yuan Y.H., Xiao H.B.,
Zhou A.Y., Hua T.X., Pei Z.Y.
<Astrophys. J. Suppl. Ser., 226, 20-20 (2016)>
=2016ApJS..226...20F 2016ApJS..226...20F (SIMBAD/NED BibCode)
ADC_Keywords: Energy distributions ; BL Lac objects ; QSOs ; Radio sources ;
X-ray sources ; Gamma rays ; Redshifts
Keywords: BL Lacertae objects: general; galaxies: active; galaxies: jets;
quasars: general
Abstract:
In this paper, multiwavelength data are compiled for a sample of 1425
Fermi blazars to calculate their spectral energy distributions (SEDs).
A parabolic function, log(νFν)=P1(logν-P2)2+P3, is
used for SED fitting. Synchrotron peak frequency (logνp),
spectral curvature (P1), peak flux (νpFνp), and integrated
flux (νFν) are successfully obtained for 1392 blazars (461
flat-spectrum radio quasars [FSRQs], 620 BL Lacs [BLs], and 311
blazars of uncertain type [BCUs]; 999 sources have known redshifts).
Monochromatic luminosity at radio 1.4GHz, optical R band, X-ray at
1keV and γ-ray at 1GeV, peak luminosity, integrated luminosity,
and effective spectral indices of radio to optical (αRO) and
optical to X-ray (αOX) are calculated. The "Bayesian
classification" is employed to logνp in the rest frame for 999
blazars with available redshift, and the results show that three
components are enough to fit the logνp distribution; there is no
ultra-high peaked subclass. Based on the three components, the
subclasses of blazars using the acronyms of Abdo+ (2010, J/ApJ/716/30)
are classified, and some mutual correlations are also studied.
Description:
In this paper, we discuss a sample of 1425 Fermi-detected blazars
(FSRQs, BLs, and BCUs) from the 3FGL (Acero et al. 2015, J/ApJS/218/23).
The multifrequency data (radio to X-ray bands) collected from NED are
used to calculate their spectral energy distributions (SEDs). SEDs
have been successfully fitted only for 1392 sources.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 130 1392 Sample for blazars
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See also:
VII/274 : The Roma BZCAT - 5th edition (Massaro+, 2015)
J/A+A/591/A130 : Dynamic SEDs of southern blazars - DSSB (Krauss+, 2016)
J/ApJ/810/14 : Third catalog of LAT-detected AGNs (3LAC) (Ackermann+, 2015)
J/ApJ/810/L9 : 1.5Jy MOJAVE AGN sample and 3FGL data (Lister+, 2015)
J/ApJS/218/23 : Fermi LAT third source catalog (3FGL) (Acero+, 2015)
J/other/AstBu/70.264 : Sample of 877 blazars (Mingaliev+, 2015)
J/other/RAA/14.1135 : Doppler factor for a Fermi blazar sample (Fan+, 2014)
J/other/RAA/13.259 : γ-ray Doppler factor for Fermi blazars (Fan+, 2013)
J/ApJS/206/13 : Blazars with γ-ray counterparts. II. (Massaro+, 2013)
J/A+A/538/A26 : BL Lac objects beyond z=1.3 (Rau+, 2012)
J/ApJ/761/125 : X and γ spectral indexes of Fermi blazars (Fan+, 2012)
J/ApJS/199/31 : Fermi LAT second source catalog (2FGL) (Nolan+, 2012)
J/ApJ/743/171 : The 2LAC catalog (Ackermann+, 2011)
J/ApJ/741/30 : Radio/γ-ray correlation in AGN (Ackermann+, 2011)
J/ApJ/740/98 : Synchroton peak for blazars and radio galaxies (Meyer+, 2011)
J/A+A/535/A69 : AGN Fermi/LAT γ-ray and 37GHz fluxes (Nieppola+, 2011)
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/709/1407 : SED of the Fermi blazars (Li+, 2010)
J/ApJ/700/597 : FERMI LAT detected blazars (Abdo+, 2009)
J/A+A/495/691 : Multifrequency catalog of blazars, Roma-BZCAT (Massaro+, 2009)
J/A+A/488/867 : Synchrotron peak frequency of 135 AGN (Nieppola+, 2008)
J/PASJ/60/161 : Multi-wave band emission from blazars (Yi+, 2008)
J/A+A/445/441 : SED of BL Lacertae objects (Nieppola+, 2006)
J/A+A/434/385 : X-ray/radio data of high energy peaked BL Lacs (Giommi+, 2005)
J/MNRAS/348/937 : The CLASS blazar survey. III. (Caccianiga+, 2004)
J/A+A/375/739 : Hard X-ray properties of blazars (Donato+, 2001)
J/A+AS/132/83 : BVRI photometry of 7 BL Lac objects (Bai+ 1998)
J/A+AS/109/267 : Radio to X-Ray distribution of BL Lac Objects (Giommi+, 1995)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- 3FGL 3FGL identifier (JHHMM.m+DDMMc)
15- 19 F5.3 --- z [0.002/3.2]? Redshift from NED
21- 22 A2 --- C SED classification code (1)
24- 28 F5.2 [10-7W] logRad [36.4/45.4]? Log radio 1.4GHz luminosity;
erg/s
30- 33 F4.2 [10-7W] e_logRad [0/0.2]? The 1σ uncertainty in logRad
35- 39 F5.2 [10-7W] logLR [40.1/47.6]? Log R band optical luminosity;
erg/s
41- 44 F4.2 [10-7W] e_logLR [0/0.2]? The 1σ uncertainty in logLR
46- 50 F5.2 [10-7W] logXr [39.3/47.1]? Log X-ray 1keV luminosity; erg/s
52- 55 F4.2 [10-7W] e_logXr [0/0.6]? The 1σ uncertainty in logXr
57- 61 F5.2 [10-7W] loggam [39.2/48.6] Log γ-ray 1GeV luminosity;
erg/s
63- 66 F4.2 [10-7W] e_loggam [0/0.3] The 1σ uncertainty in loggam
68- 71 F4.2 --- alphaRO [0.1/1]? Effective radio to optical
spectral index (2)
73- 76 F4.2 --- e_alphaRO [0/0.04]? The 1σ uncertainty in alphaRO
78- 81 F4.2 --- alphaOX [0.4/2.2]? Effective optical to X-ray
spectral index (2)
83- 86 F4.2 --- e_alphaOX [0/0.2]? The 1σ uncertainty in alphaOX
88- 92 F5.2 --- P1 [-0.5/-0.03] Spectral curvature P1
94- 97 F4.2 --- e_P1 [0/0.3]? The 1σ uncertainty in P1
99-103 F5.2 [Hz] lognup [11.6/20.2] Log synchrotron peak frequency
105-108 F4.2 [Hz] e_lognup [0/4.6]? The 1σ uncertainty in lognup
110-114 F5.2 [10-7W] logLp [40.1/47.4] Log peak luminosity; erg/s
116-119 F4.2 [10-7W] e_logLp [0/2]? The 1σ uncertainty in logLp
121-125 F5.2 [10-7W] logLbol [40.5/47.7] Log integrated, bolometric
luminosity; erg/s
127-130 F4.2 [10-7W] e_logLbol [0/2.5] The 1σ uncertainty in logLbol
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Note (1): SED classification code as follows:
HF = high synchrotron peak, flat spectrum radio quasars (9 sources);
IF = intermediate synchrotron peak, flat spectrum radio quasars (183 sources);
LF = low synchrotron peak, flat spectrum radio quasars (269 sources);
HB = high synchrotron peak, BL Lac (235 sources);
IB = intermediate synchrotron peak, BL Lac (273 sources);
LB = low synchrotron peak, BL Lac (112 sources);
HU = high synchrotron peak, U-Blazar (106 sources);
IU = intermediate synchrotron peak, U-Blazar (109 sources);
LU = low synchrotron peak, U-Blazar (96 sources);
Note (2): These are calculated by a formula
(Ledden & O'Dell 1985ApJ...298..630L 1985ApJ...298..630L),
α12=-log(f1/f2)/log(ν1/ν2),
where f1 and f2 are the flux densities in frequencies ν1 and
ν2, respectively, and f(ν)∝ν-α.
In this paper, νR=1.4GHz, νO=4.68e14Hz and
νX=2.416e17Hz are adopted.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 10-Nov-2016