J/MNRAS/448/1060 Fermi/LAT broad emission line blazars (Ghisellini+, 2015)
Fermi/LAT broad emission line blazars.
Ghisellini G., Tavecchio F.
<Mon. Not. R. Astron. Soc., 448, 1060-1077 (2015)>
=2015MNRAS.448.1060G 2015MNRAS.448.1060G (SIMBAD/NED BibCode)
ADC_Keywords: BL Lac objects
Keywords: radiation mechanisms: non-thermal - BL Lacertae objects: general -
quasars: general - gamma-rays: general
Abstract:
We study the broad emission line blazars detected in the γ-ray
band by the Large Area Telescope onboard the Fermi satellite and
with the optical spectrum studied by Shaw et al. (2012, Cat.
J/ApJ/748/49, hereafter S12, and 2013, Cat. J/ApJ/764/135, hereafter
S13). The observed broad line strength provides a measure of the
ionizing luminosity of the accretion disc, while the
γ-luminosity is a proxy for the bolometric non-thermal beamed
jet emission. The resulting sample, composed by 217 blazars, is the
best suited to study the connection between accretion and jet
properties. We compare the broad emission line properties of these
blazars with those of radio-quiet and radio-loud quasars present in
the Sloan Digital Sky Survey, to asses differences and similarities of
the disc luminosity and the virial black hole mass. For most sources,
we could derive the black hole mass by reproducing the IR-optical-UV
data with a standard accretion disc spectrum, and we compared the
black hole masses derived with the two methods. The distributions of
the masses estimated in the two ways agree satisfactorily. We then
apply a simple, one-zone, leptonic model to all the 217 objects of our
sample. The knowledge of the black hole mass and disc luminosity helps
to constrain the jet parameters. On average, they are similar to what
found by previous studies of smaller samples of sources.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 58 195 The FSRQs in our sample
tablea2.dat 42 26 The BL Lac objects considered in this paper,
drawn from the sample of S13
tablea3.dat 120 196 Parameters used to model the SED
tablea4.dat 120 26 Parameters for BL Lac objects in S13
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See also:
J/ApJ/748/49 : Optical spectroscopy of 1LAC broad-line blazars (Shaw+, 2012)
J/ApJ/764/135 : Spectroscopic redshifts of BL Lac objects (Shaw+, 2013)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Name (HHMM+DDMM), from S12
11- 29 A19 --- OName Other name, from NED
31- 35 F5.3 --- z Redshift
37- 40 F4.2 [Msun] logMHb ?=- Black hole mass calculated through the
virial method by S12 using the Hβ line
42- 45 F4.2 [Msun] logMMgII ?=- Black hole mass calculated through the
virial method by S12 using the MgII line
47- 50 F4.2 [Msun] logMCIV ?=- Black hole mass calculated through the
virial method by S12 using the CIV line
52- 55 F4.2 [Msun] logMfit Black hole mass estimated in this paper
through the disc-fitting method
56 A1 --- f_logMfit [)] ) for values that could not be evaluated
through the disc-fitting method
58 A1 --- n_logMfit Note on logMfit (1)
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Note (1): Notes as follows:
- = In most cases, values that could not be evaluated are equal to the
virial masses (within a factor 2).
1 = In a minority of cases, values that could not be evaluated differ
from the virial values, because a value larger than the virial
one has been adopted to avoid super-Eddington or nearly
Eddington disc luminosities
2 = In a minority of cases, values that could not be evaluated differ
from the virial values, because a value smaller than the virial
one has been adopted to avoid to overproduce the NIR-optical flux
3 = In a minority of cases, values that could not be evaluated differ
from the virial values, because a value larger than the virial one
has been adopted to avoid to overproduce the optical-UV flux.
* = When the disc-fitting method could use only one point to find a value
for the black hole mass. This is the value used for the jet model.
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Name Name (HHMM+DDMM), from S13
11- 31 A21 --- OName Other name, from NED
33- 37 F5.3 --- z Redshift
39- 42 F4.2 [Msun] logMfit Mass used in the fitting model
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Byte-by-byte Description of file: tablea3.dat tablea4.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- Sample Sample (S12 or S13)
5- 13 A9 --- Name Name (HHMM_DDMM)
15- 19 F5.3 --- z Redshift
21- 27 F7.3 10+38W Ld45 Accretion disk luminosity
29- 34 E6.2 10+38W Ppe45 Power injected in the blob calculated in the
comoving frame (P'e,45)
36- 40 F5.2 gauss B Magnetic field
42- 45 I4 --- Rdiss Dissipation radius in units of RS
47- 50 F4.1 --- Gamma Bulk Lorentz factor at Rdiss
51 A1 --- n_Gamma Note on vewing angle if not set to 3 (1)
53- 57 E5.2 --- gammamax Maximum random Lorentz factor of the
injected electrons
59- 63 I5 --- gammab Break random Lorentz factor of the
injected electrons
65- 73 F9.2 --- gammapeak Random Lorentz factor of the electrons
emitting at the peak of the SED
75- 81 F7.2 --- gammacool Random Lorentz factor of the electrons
cooling in one dynamical time R=c
84- 89 F6.3 10-7J/cm3 Up Total (magnetic+radiative) energy density in
the comoving frame (U')
91- 94 F4.1 --- s1 Slope of the injected electron distribution
95- 99 F5.2 --- s2 Slope of the injected electron distribution
100-106 E7.3 Msun/yr dM/dtin Mass accretion rate
108-113 E6.4 Msun/yr dM/dtout Mass outflowing rate
116-120 F5.2 [Lsun] logLd Disc luminosity according to S12
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Note (1): Note on viewing angle value as follows:
a = θv= 2
b = θv= 2.3
c = θv= 2.4
d = θv= 2.5
e = θv= 3.5
f = θv= 4
g = θv= 6
h = θv= 10
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 05-Aug-2015