J/ApJS/262/18 Spectral energy distributions for 4FGL blazars (Yang+, 2022)
The spectral energy distributions for 4FGL blazars.
Yang J.H., Fan J.H., Liu Y., Tuo M.X., Pei Z.Y., Yang W.X., Yuan Y.H.,
He S.L., Wang S.H., Wang X.C., Chen X.J., Qu X.H., Cao Q., Tao Q.Y.,
Zhang Y.L., Liu C.Q., Nie J.J., Liu L.F., Jiang D.K., Jiang A.N., Liu B.,
Yang R.S.
<Astrophys. J. Suppl. Ser., 262, 18 (2022)>
=2022ApJS..262...18Y 2022ApJS..262...18Y
ADC_Keywords: Active gal. nuclei; Gamma rays; X-ray sources; Optical;
Radio sources; Redshifts; BL Lac objects; QSOs
Keywords: Active galactic nuclei ; Gamma-ray sources ; Blazars ; Quasars ;
BL Lacertae objects ; Spectral energy distribution
Abstract:
In this paper, the multiwavelength data from radio to X-ray bands for
2709 blazars in the 4FGL-DR3 catalog are compiled to calculate their
spectral energy distributions using a parabolic equation
log(νfν)=P1(logν-P2)2+P3. Some important parameters
including spectral curvature (P1), synchrotron peak frequency (P2,
logνp), and peak luminosity (logLp) are obtained. Based on
those parameters, we discussed the classification of blazars using the
"Bayesian classification" and investigated some mutual correlations.
We came to the following results. (1) Based on the Bayesian
classification of synchrotron peak frequencies, the 2709 blazars can
be classified into three subclasses, i.e., log(νp/Hz)<13.7 for
low synchrotron peak blazars (LSPs), 13.7<log(νp/Hz)<14.9 for
intermediate synchrotron peak blazars (ISPs), and log(νp/Hz)>14.9
for high synchrotron peak blazars (HSPs), and there are 820 HSPs,
750 ISPs, and 1139 LSPs. (2) The γ-ray emission has the closest
relationship with radio emission, followed by optical emission, while
the weakest relationship is that with X-ray emission. The γ-ray
luminosity is also correlated with the synchrotron peak luminosity.
(3) There are strong positive correlations between the curvature
(1/|P1|) and the peak frequency (logνp) for all subclasses
(FSRQs, (high, intermediate, and low) BL Lacertae objects). For
different subclasses, the correlation slopes are different, which
implies that there are different acceleration mechanisms and emission
processes for different subclasses of blazars.
Description:
In this paper, we will calculate the SEDs of synchrotron emissions for
the blazars in the Fourth Fermi-LAT 12-year Source catalog (4FGL-DR3,
Cat. IX/67). The multiwavelength data from radio to X-ray are obtained
from the NASA/IPAC Extragalactic Database (NED).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 100 2709 Blazars sample and the SEDs fitting results
for 2709 blazars
refs.dat 94 178 References
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See also:
IX/67 : Incremental Fermi LAT 4th source cat. (4FGL-DR3) (Fermi-LAT col., 2022)
J/A+A/281/355 : X-ray AGN content of Molonglo 408MHz survey (Brinkmann+ 1994)
J/A+AS/109/267 : Radio to X-Ray distribution of BL Lac Objects (Giommi+, 1995)
J/A+A/375/739 : Hard X-ray properties of blazars (Donato+, 2001)
J/AJ/129/2542 : BL Lac from SDSS (Collinge+, 2005)
J/A+A/445/441 : SED of BL Lacertae objects (Nieppola+, 2006)
J/A+A/476/759 : X-ray properties of AGN from the CJF sample (Britzen+, 2007)
J/A+A/488/867 : Synchrotron peak frequency of 135 AGN (Nieppola+, 2008)
J/ApJ/715/429 : First Fermi-LAT AGN catalog (1LAC) (Abdo+, 2010)
J/ApJ/716/30 : SED of Fermi bright blazars (Abdo+, 2010)
J/ApJ/743/171 : The 2LAC catalog (Ackermann+, 2011)
J/A+A/535/A69 : AGN Fermi/LAT γ-ray and 37GHz fluxes (Nieppola+, 2011)
J/ApJ/761/125 : X and γ spectral indexes of Fermi blazars (Fan+, 2012)
J/other/RAA/14.1135 : Doppler factor for a Fermi blazar sample (Fan+, 2014)
J/ApJ/810/14 : Third catalog of LAT-detected AGNs (3LAC) (Ackermann+, 2015)
J/ApJS/226/20 : X-ray, opt. & radio SEDs of Fermi blazars (Fan+, 2016)
J/ApJ/835/L38 : Fermi blazars with Doppler factors (Fan+, 2017)
J/ApJS/247/33 : The Fermi LAT fourth source catalog (4FGL) (Abdollahi+, 2020)
J/ApJ/892/105 : 4th catalog of Fermi LAT-detected AGNs (4LAC) (Ajello+, 2020)
J/ApJ/914/42 : Radio follow-up to 4FGL-DR2 sources (Bruzewski+, 2021)
J/ApJS/253/10 : 12yrs of R-band photometry of the quasar 3C 454.3 (Fan+, 2021)
J/ApJS/253/46 : Optical spectroscopy of Fermi blazars (Paliya+, 2021)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- --- [4FGL]
6- 18 A13 --- 4FGL 4FGL blazar name (JHHMM.m+DDMMa)
20- 23 A4 --- C1 Classification, 4FGL-DR3 catalog (1)
25- 27 A3 --- C2 Classification, peak frequency (2)
29- 33 F5.3 --- z [0/4.32]? Redshift
35- 42 A8 --- r_z References for z (see refs.dat file)
44- 48 F5.2 --- P1 [-0.3/-0.04] Parabolic fit, spectral
curvature (3)
50- 53 F4.1 [Hz] P2 [12/18.7] Parabolic fit, synchrotron peak
frequency, log(νp) (3)
55- 60 F6.2 [mW/m2] P3 [-13.4/-9.6] Parabolic fit, peak flux,
log(νpfνp), in log(erg/s/cm2)
units (3)
62- 66 F5.2 [10-7W] logLp [34.6/47.8] Peak luminosity
in log(erg/s) units
68- 72 F5.2 [10-7W] logLR [31.6/45.4]? 1.4GHz radio luminosity
in log(erg/s) units
74- 78 F5.2 [10-7W] logLO [34.8/47.4]? 2.43+1014Hz optical luminosity
in log(erg/s) units
80- 84 F5.2 [10-7W] logLX [39.9/47.8]? 1keV X-ray luminosity
in log(erg/s) units
86- 90 F5.2 [10-7W] logLg [34.5/48.8] 1GeV γ-ray luminosity
in log(erg/s) units
92- 95 F4.2 --- alpha-RO [0.01/0.9]? Radio to optical
effective spectral index
97-100 F4.2 --- alpha-OX [0.48/2.1]? Optical to X-ray
effective spectral index
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Note (1): The classification is obtained from 4FGL-DR3 catalogue as follows:
BLL = BL Lac objects (1142 occurrences);
FSRQ = flat spectrum radio quasar (760 occurrences);
BCU = blazars of Uncertain type (807 occurrences).
Note (2): The classification is given by the peak frequency of synchrotron
emission as follows:
LSP = low synchrotron peak frequency blazar, log(nu-p/Hz)<13.7
(1139 occurrences)
ISP = intermediate synchrotron peak frequency blazar,
13.7<log(nu-p/Hz)<14.9 (750 occurrences)
HSP = high synchrotron peak frequency blazar, log(nu-p/Hz)>14.9
(820 occurrences).
Note (3): Parameters obtained from fitting SED with a parabolic equation,
log(nu*fnu)=P1(log(nu)-P2)2+P3R. Here peak frequencies (P2) have
not been corrected by redshift.
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Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Ref Reference code
10- 28 A19 --- BibCode Bibcode of the reference
30- 52 A23 --- Auth First author's name(s)
54- 94 A41 --- Comm Comment
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 17-Nov-2022