J/ApJ/757/25 Fermi/LAT AGN at 5GHz (Linford+, 2012)
Gamma-ray loudness, synchrotron peak frequency, and parsec-scale properties of
blazars detected by the Fermi Large Area Telescope.
Linford J.D., Taylor G.B., Schinzel F.K.
<Astrophys. J., 757, 25 (2012)>
=2012ApJ...757...25L 2012ApJ...757...25L
ADC_Keywords: Active gal. nuclei ; BL Lac objects ; Gamma rays ; Radio sources
Keywords: BL Lacertae objects: general; galaxies: active; galaxies: jets;
galaxies: nuclei; gamma rays: galaxies; quasars: general;
radio continuum: galaxies
Abstract:
The parsec-scale radio properties of 232 active galactic nuclei, most
of which are blazars, detected by the Large Area Telescope (LAT) on
board the Fermi Gamma-ray Space Telescope have been observed
contemporaneously by the Very Long Baseline Array (VLBA) at 5GHz. Data
from both the first 11 months (1FGL) and the first 2 years (2FGL) of
the Fermi mission were used to investigate these sources' γ-ray
properties. We use the ratio of the γ-ray-to-radio luminosity as
a measure of γ-ray loudness. We investigate the relationship of
several radio properties to γ-ray loudness and to the
synchrotron peak frequency. There is a tentative correlation between
γ-ray loudness and synchrotron peak frequency for BL Lac objects
in both 1FGL and 2FGL, and for flat-spectrum radio quasars (FSRQs) in
2FGL. We find that the apparent opening angle tentatively correlates
with γ-ray loudness for FSRQs, but only when we use the 2FGL
data. We also find that the total VLBA flux density correlates with
the synchrotron peak frequency for BL Lac objects and FSRQs. The core
brightness temperature also correlates with synchrotron peak
frequency, but only for the BL Lac objects. The low-synchrotron-peaked
(LSP) BL Lac object sample shows indications of contamination by FSRQs
which happen to have undetectable emission lines. There is evidence
that the LSP BL Lac objects are more strongly beamed than the rest of
the BL Lac object population.
Description:
The radio observations of our 232 LAT-detected AGNs were done with the
VLBA at 5GHz between 2009 November and 2010 July. This is the sample
described in more detail in Linford et al. (2012, Cat. J/ApJ/744/177).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 97 232 LAT-detected AGNs data
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See also:
J/A+A/562/A64 : Fermi detection of BL Lac objects (Wu+, 2014)
J/ApJS/208/17 : 2nd Fermi LAT cat. of gamma-ray pulsars (2PC) (Abdo+, 2013)
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/MNRAS/424/2832 : Pulsars in γ-ray sources (Lee+, 2012)
J/MNRAS/424/L64 : AGN/pulsar distinction for 2FGL sources (Mirabal+, 2012)
J/ApJ/753/83 : Associations to 1FGL sources (Ackermann+, 2012)
J/ApJ/744/177 : VLBA 5GHz observations of Fermi/LAT AGNs (Linford+, 2012)
J/ApJ/743/171 : The 2LAC catalog (Ackermann+, 2011)
J/ApJ/742/66 : New Fermi/LAT extragalactic sources (Teng+, 2011)
J/ApJ/742/27 : 15GHz and jet properties of MOJAVE blazars (Lister+, 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/ApJS/194/29 : Observations of blazars at 15GHz (Richards+, 2011)
J/ApJ/722/520 : Gamma-ray light curves of Fermi blazars (Abdo+, 2010)
J/ApJ/722/L7 : Fermi/LAT detected MOJAVE AGNs (Pushkarev+, 2010)
J/ApJ/718/587 : The Fermi-AT20G catalog (Mahony+, 2010)
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/ApJS/188/405 : Fermi-LAT first source catalog (1FGL) (Abdo+, 2010)
J/AJ/138/1874 : MOJAVE. VI. Kinematic analysis of blazar jets (Lister+, 2009)
J/ApJ/707/L56 : VLBI and bright Fermi/LAT sources (Kovalev, 2009)
J/ApJ/706/L7 : The Fermi LAT sky as seen by INTEGRAL/IBIS (Ubertini+, 2009)
J/ApJ/700/597 : FERMI LAT detected blazars (Abdo+, 2009)
J/A+A/488/867 : Synchrotron peak frequency of 135 AGN (Nieppola+, 2008)
J/ApJ/658/203 : VLBA imaging and polarimetry survey at 5GHz (Helmboldt+, 2007)
J/A+A/445/441 : SED of BL Lacertae objects (Nieppola+, 2006)
http://www.physics.purdue.edu/astro/MOJAVE/ : MOJAVE homepage
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Source name
(FHHMMm+DDMM; J2000 or JHHMMm+DDMM) (1)
13 A1 --- f_Name [a] Source in MOJAVE (2)
15- 18 A4 --- --- [1FGL]
20- 31 A12 --- 1FGL 1FGL name (JHHMM.m+DDMM)
33 A1 --- f_1FGL [b] multiple radio associations in 1LAC (2)
35- 38 A4 --- --- [2FGL]
40- 51 A12 --- 2FGL 2FGL name if any (JHHMM.m+DDMM)
53 A1 --- f_2FGL [cd] potential confusions (2)
55- 71 A17 --- AName Alternative AGN name
73- 75 A3 --- OT Optical type from 2LAC/1LAC (3)
77- 79 A3 --- SED SED type (4)
81- 84 A4 --- r_SED SED reference (5)
86- 91 I6 --- Grl [545/186614]? γ-ray loudness using
1FGL data (6)
93- 97 I5 --- Gr2 [404/95093]? γ-ray loudness using
2FGL data (6)
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Note (1): designation of source:
* If name starts with "J" it is a VIPS (VLBA Imaging and Polarimetry
Survey; Helmboldt et al. 2007, J/ApJ/658/203), or a pre-1FGL MOJAVE source;
* If name starts with "F" it is a source targeted specifically for its
presence in 1FGL.
Note (2): Flag as follows:
a = MOJAVE source that was included in Lister et al. (2011, J/ApJ/742/27).
For more data, visit the MOJAVE Web site
http://www.physics.purdue.edu/astro/MOJAVE/MOJAVEIItable.html or see
Lister et al. (2009, Cat. J/AJ/138/1874; 2011, Cat. J/ApJ/742/27).
b = Indicates a LAT source which is associated with multiple radio sources
with high (≥80%) probability in 1LAC.
c = Indicates a LAT source which is associated with multiple radio sources
with high (≥80%) probability in 2LAC.
d = Indicates a 2FGL source that is considered to be potentially confused
with galactic diffuse emission.
Note (3): Optical type as follows:
bzb = BL Lac object,
bzq = FSRQ (flat spectrum radio quiet)
agn = non-blazar AGN,
agu = AGN of uncertain type,
sbg = starburst galaxy
Note (4): SED type as follows:
LSP = low-synchrotron-peaked,
ISP = intermediate-synchrotron-peaked,
HSP = high-synchrotron-peaked
Note (5): Reference as follows:
0FGL = Abdo et al. 2010, Cat. J/ApJ/716/30
N-06 = Nieppola et al. 2006, Cat. J/A+A/445/441
N-08 = Nieppola et al. 2008, Cat. J/A+A/488/867
A-11 = Aatrokoski et al. 2011A&A...536A..15P 2011A&A...536A..15P
M-11 = Meyer et al. 2011, Cat. J/ApJ/740/98
2LAC = estimated using technique in Ackermann et al. 2011, Cat. J/ApJ/743/171
fit = log-parabolic fit to NED data.
Note (6): Gr, the γ-ray loudness is the ratio of γ-ray to radio
luminosity.
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 20-May-2014