J/ApJ/716/30 SED of Fermi bright blazars (Abdo+, 2010)
The spectral energy distribution of Fermi bright blazars.
Abdo A.A., Ackermann M., Agudo I., Ajello M., Aller H.D., Aller M.F.,
Angelakis E., Arkharov A.A., Axelsson M., Bach U., Baldini L., Ballet J.,
Barbiellini G., Bastieri D., Baughman B.M., Bechtol K., Bellazzini R.,
Benitez E., Berdyugin A., Berenji B., Blandford R.D., Bloom E.D.,
Boettcher M., Bonamente E., Borgland A.W., Bregeon J., Brez A., Brigida M.,
Bruel P., Burnett T.H., Burrows D., Buson S., Caliandro G.A.,
Calzoletti L., Cameron R.A., Capalbi M., Caraveo P.A., Carosati D.,
Casandjian J.M., Cavazzuti E., Cecchi C., Celik O., Charles E., Chaty S.,
Chekhtman A., Chen W.P., Chiang J., Chincarini G., Ciprini S., Claus R.,
Cohen-Tanugi J., Colafrancesco S., Cominsky L.R., Conrad J., Costamante L.,
Cutini S., D'Ammando F., Deitrick R., D'Elia V., Dermer C.D.,
de Angelis A., de Palma F., Digel S.W., Donnarumma I., do Couto e Silva E.,
Drell P.S., Dubois R., Dultzin D., Dumora D., Falcone A., Farnier C.,
Favuzzi C., Fegan S.J., Focke W.B., Forne E., Fortin P., Frailis M.,
Fuhrmann L., Fukazawa Y., Funk S., Fusco P., Gomez J.L., Gargano F.,
Gasparrini D., Gehrels N., Germani S., Giebels B., Giglietto N., Giommi P.,
Giordano F., Giuliani A., Glanzman T., Godfrey G., Grenier I.A.,
Gronwall C., Grove J.E., Guillemot L., Guiriec S., Gurwell M.A.,
Hadasch D., Hanabata Y., Harding A.K., Hayashida M., Hays E., Healey S.E.,
Heidt J., Hiriart D., Horan D., Hoversten E.A., Hughes R.E., Itoh R.,
Jackson M.S., Johannesson G., Johnson A.S., Johnson W.N., Jorstad S.G.,
Kadler M., Kamae T., Katagiri H., Kataoka J., Kawai N., Kennea J., Kerr M.,
Kimeridze G., Knodlseder J., Kocian M.L., Kopatskaya E.N., Koptelova E.,
Konstantinova T.S., Kovalev Y.Y., Kovalev Yu.A., Kurtanidze O.M., Kuss M.,
Lande J., Larionov V.M., Latronico L., Leto P., Lindfors E., Longo F.,
Loparco F., Lott B., Lovellette M.N., Lubrano P., Madejski G.M., Makeev A.,
Marchegiani P., Marscher A.P., Marshall F., Max-Moerbeck W.,
Mazziotta M.N., McConville W., McEnery J.E., Meurer C., Michelson P.F.,
Mitthumsiri W., Mizuno T., Moiseev A.A., Monte C., Monzani M.E.,
Morselli A., Moskalenko I.V., Murgia S., Nestoras I., Nilsson K.,
Nizhelsky N.A., Nolan P.L., Norris J.P., Nuss E., Ohsugi T., Ojha R.,
Omodei N., Orlando E., Ormes J.F., Osborne J., Ozaki M., Pacciani L.,
Padovani P., Pagani C., Page K., Paneque D., Panetta J.H., Parent D.,
Pasanen M., Pavlidou V., Pelassa V., Pepe M., Perri M., Pesce-Rollins M.,
Piranomonte S., Piron F., Pittori C., Porter T.A., Puccetti S., Rahoui F.,
Raino S., Raiteri C., Rando R., Razzano M., Reimer A., Reimer O.,
Reposeur T., Richards J.L., Ritz S., Rochester L.S., Rodriguez A.Y.,
Romani R.W., Ros J.A., Roth M., Roustazadeh P., Ryde F.,
Sadrozinski H.F.-W., Sadun A., Sanchez D., Sander A., Saz Parkinson P.M.,
Scargle J.D., Sellerholm A., Sgro C., Shaw M.S., Sigua L.A., Siskind E.J.,
Smith D.A., Smith P.D., Spandre G., Spinelli P., Starck J.-L.,
Stevenson M., Stratta G., Strickman M.S., Suson D.J., Tajima H.,
Takahashi H., Takahashi T., Takalo L.O., Tanaka T., Thayer J.B.,
Thayer J.G., Thompson D.J., Tibaldo L., Torres D.F., Tosti G.,
Tramacere A., Uchiyama Y., Usher T.L., Vasileiou V., Verrecchia F.,
Vilchez N., Villata M., Vitale V., Waite A.P., Wang P., Winer B.L.,
Wood K.S., Ylinen T., Zensus J.A., Zhekanis G.V., Ziegler M.
<Astrophys. J., 716, 30-70 (2010)>
=2010ApJ...716...30A 2010ApJ...716...30A (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; Energy distributions ; X-ray sources ;
Photometry, infrared ; Photometry, UBV ; Radio sources
Keywords: BL Lacertae objects: general - galaxies: active - quasars: general -
gamma rays: galaxies - radiation mechanisms: non-thermal
Abstract:
We have conducted a detailed investigation of the broadband spectral
properties of the γ-ray selected blazars of the Fermi LAT Bright
AGN Sample (LBAS, Cat. J/ApJ/700/597). By combining our accurately
estimated Fermi γ-ray spectra with Swift, radio, infra-red,
optical, and other hard X-ray/γ-ray data, collected within 3
months of the LBAS data taking period, we were able to assemble
high-quality and quasi-simultaneous spectral energy distributions
(SED) for 48 LBAS blazars. We have used these SED to characterize the
peak intensity of both the low- and the high-energy components. The
results have been used to derive empirical relationships that estimate
the position of the two peaks from the broadband colors (i.e., the
radio to optical, αro, and optical to X-ray, αox,
spectral slopes) and from the γ-ray spectral index. While more
than 50% of known radio bright high energy peaked (HBL) BL Lacs are
detected in the LBAS sample, only less than 13% of known bright
broad-lined flat spectrum radio quasars (FSRQs) and LBL BL Lacs are
included. This suggests that the latter sources, as a class, may be
much fainter γ-ray emitters than LBAS blazars, and could in fact
radiate close to the expectations of simple synchrotron self-Compton
(SSC) models. We categorized all our sources according to a new
physical classification scheme based on the generally accepted
paradigm for Active Galactic Nuclei and on the results of this SED
study.
Description:
Multi-frequency observations of LBAS blazars were carried out between
2008 August and October with Fermi, and between 2008 May and 2009
January with Swift and other space and ground-based facilities.
The Fermi-LAT γ-ray spectra of all the LBAS sources are studied
in detail in a dedicated paper (Abdo et al. 2010ApJ...710.1271A 2010ApJ...710.1271A). Here
we derive the detailed γ-ray spectra of the 48 blazars for which
we build the quasi-simultaneous SED based on the three months of data
used to define the LBAS sample.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 113 115 Sources list and basic parameters
table2.dat 124 48 Results of Fermi-LAT data analysis
table3.dat 113 118 Results of Swift UVOT data analysis
table4.dat 75 117 Results of Swift XRT data analysis
table5.dat 36 144 Effelsberg radio data (2.6-42GHz)
table6.dat 60 24 Owens Valley Radio Observatory (OVRO) Data (15GHz)
table7.dat 33 173 RATAN-600 (1-22GHz) flux density measurements in
2008 September 10-October 3
table8.dat 48 140 GASP-WEBT data (optical, NIR, radio)
table13.dat 87 115 Blazar SED parameters
--------------------------------------------------------------------------------
See also:
I/284 : The USNO-B1.0 Catalog (Monet+ 2003)
J/ApJS/194/29 : Observations of blazars at 15GHz (Richards+, 2011)
J/A+A/520/A47 : Blazars in the Swift-BAT hard X-ray sky (Maselli+, 2010)
J/ApJ/709/1407 : SED of the Fermi blazars (Li+, 2010)
J/ApJ/699/603 : Evolution of Swift/BAT blazars (Ajello+, 2009)
J/ApJ/700/597 : FERMI LAT detected blazars (Abdo+, 2009)
J/A+A/495/691 : Multifrequency catalogue of blazars, Roma-BZCAT (Massaro+,
2009)
J/ApJS/171/61 : All-Sky Survey of Flat-Spectrum Radio Sources (Healey+, 2007)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- 0FGL Fermi/LAT name (JHHMM.m+DDMM)
14- 43 A30 --- OName Name(s) of the blazar associated with the
gamma-ray source
45- 46 I2 h RAh Hour of right ascension (J2000) (1)
48- 49 I2 min RAm Minute of right ascension (J2000)
51- 54 F4.1 s RAs Second of right ascension (J2000)
56 A1 --- DE- Sign of declination (J2000) (1)
57- 58 I2 deg DEd Degree of declination (J2000) (1)
60- 61 I2 arcmin DEm Arcminute of declination (J2000)
63- 66 F4.1 arcsec DEs Arcsecond of declination (J2000)
68- 72 F5.3 --- z ? Redshift when known
74- 78 I5 mJy F6cm ? 5GHz radio flux density (6cm); not corrected
80- 83 F4.1 mag Vmag ? Optical apparent magnitude (2)
85- 92 E8.3 mW/m2 FX ? The 0.1-2.4keV X-ray flux; not corrected (3)
94- 98 F5.2 --- aro ? Radio (5GHz) to optical (5000A) spectral slope
100-103 F4.2 --- aox ? Optical to x-ray (1keV) spectral slope
105-108 F4.2 --- arx ? Radio to x-ray spectral slope
110-113 F4.2 --- axg ? X-ray to gamma (100MeV) spectral slope
--------------------------------------------------------------------------------
Note (1): Precise equatorial coordinates taken from the BZCat catalog (Massaro
et al. 2009, Cat. J/A+A/495/691) or from NED.
Note (2): Optical apparent magnitude, Vmag, from the CRATES (Healey et al.
2007, Cat. J/ApJS/171/61) and from the USNO-B1 (Monet et al. 2003,
Cat. I/284) catalogs respectively.
Note (3): The 0.1-2.4keV X-ray flux from the BZcat (Cat. J/A+A/495/691), or
from recent Swift observations processed at the ASI Science Data
Center (ASDC), as described in Section 3.2.4.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- 0FGL Fermi/LAT name (JHHMM.m+DDMM)
14- 20 E7.3 ph/MeV/cm2/s F100 ? Fermi/LAT flux in 100-316.2MeV band
22- 28 E7.3 ph/MeV/cm2/s e_F100 ? F100 uncertainty
30- 36 E7.3 ph/MeV/cm2/s F316 Fermi/LAT flux in 316.2-1000MeV band
38- 44 E7.3 ph/MeV/cm2/s e_F316 F316 uncertainty
46- 52 E7.3 ph/MeV/cm2/s F1000 Fermi/LAT flux in 1000-3162.3MeV band
54- 60 E7.3 ph/MeV/cm2/s e_F1000 F1000 uncertainty
62- 68 E7.3 ph/MeV/cm2/s F3162 ? Fermi/LAT flux in 3162.3-10000MeV band
70- 76 E7.3 ph/MeV/cm2/s e_F3162 ? F3162 uncertainty
78- 84 E7.3 ph/MeV/cm2/s F10000 ? Fermi/LAT flux in 10000-31623MeV band
86- 92 E7.3 ph/MeV/cm2/s e_F10000 ? F10000 uncertainty
94-100 E7.3 ph/MeV/cm2/s F31623 ? Fermi/LAT flux in 31623-100000MeV band
102-108 E7.3 ph/MeV/cm2/s e_F31623 ? F31623 uncertainty
110-116 E7.3 ph/MeV/cm2/s F100000 ? Fermi/LAT flux in 100000-316230MeV band
118-124 E7.3 ph/MeV/cm2/s e_F100000 ? F100000 uncertainty
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- 0FGL Source name (JHHMM.m+DDMM)
14- 23 A10 "YYYY/MM/DD" Date Observation date
25- 31 F7.4 mag Vmag ? Swift/UVOT V-band magnitude (1)
32 A1 --- l_Vmag Limit flag on Vmag
34- 38 F5.3 mag e_Vmag ? Vmag uncertainty (1)
40- 46 F7.4 mag Bmag ? Swift/UVOT B-band magnitude (1)
47 A1 --- l_Bmag Limit flag on Bmag
48 A1 --- f_Bmag [o] other Bmag values (2)
49- 53 F5.3 mag e_Bmag ? Bmag uncertainty (1)
55- 61 F7.4 mag Umag ? Swift/UVOT U-band magnitude (1)
62 A1 --- l_Umag Limit flag on Umag
63 A1 --- f_Umag [o] other Umag values (2)
64- 68 F5.3 mag e_Umag ? Umag uncertainty (1)
70- 76 F7.4 mag UVW1mag ? Swift/UVOT UVW1-band magnitude (1)
77 A1 --- l_UVW1mag Limit flag on UVW1mag
79- 83 F5.3 mag e_UVW1mag ? UVW1mag uncertainty (1)
85- 91 F7.4 mag UVM2mag ? Swift/UVOT UVM2-band magnitude (1)
92 A1 --- l_UVM2mag Limit flag on UVM2mag
94- 98 F5.3 mag e_UVM2mag ? UVM2mag uncertainty (1)
100-106 F7.4 mag UVW2mag ? Swift/UVOT UVW2-band magnitude (1)
107 A1 --- l_UVW2mag Limit flag on UVW2mag
109-113 F5.3 mag e_UVW2mag ? UVW2mag uncertainty (1)
--------------------------------------------------------------------------------
Note (1): All magnitudes are corrected for Galactic extinction.
Note (2):
o = Other values for J0730.4-1142, in 2008/11/08, are 13.85 and 17.96,
in UVM2-band and UVW2-band, respectively.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- 0FGL Source name (JHHMM.m+DDMM)
14- 23 A10 "YYYY/MM/DD" Date Observation date
25- 31 F7.1 s Exp Net Swift/XRT exposure time
33- 41 E9.4 --- FX Swift/XRT 2-10keV x-ray flux (1)
43- 46 F4.2 --- Gamma ? Best-fit photon index or the log parabola
parameter a (2)
48- 52 F5.3 --- e_Gamma ? Gamma uncertainty
54- 59 F6.3 --- b ? Best-fit curvature parameter b
61- 65 F5.3 --- e_b ? b uncertainty
67- 69 I3 --- dof ? Number of degrees of freedom
71- 75 F5.3 --- chi2 ? Value of the reduced χ2
--------------------------------------------------------------------------------
Note (1): When the photon statistics were too poor to allow a reliable best fit,
the flux was estimated converting the observed count rate assuming a
power-law model with photon index of 1.9 and low energy absorption due
to Galactic NH.
Note (2): This column gives the power-law photon index Γ when a simple
power-law model could be used. In the case where the log parabola
model was used this column gives the a parameter which represents the
photon index at 1keV.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- 0FGL Source name
14- 23 A10 "YYYY/MM/DD" Date Observation date
25- 29 F5.2 GHz Freq Effelsberg frequency
31- 36 F6.3 Jy Flux Effelsberg flux density
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- 0FGL Source name (JHHMM.m+DDMM)
15- 18 I4 yr DateMin.Y Date of the observed minimum
19- 21 A3 "month" DateMin.M Date of the observed minimum
22- 23 I02 d DateMin.D Date of the observed minimum
25- 30 F6.3 Jy Smin Observed minimum flux density at 15GHz
32- 36 F5.3 Jy e_Smin Mean error on Smin (1)
39- 42 I4 yr DateMax.Y Date of the observed minimum
43- 45 A3 "month" DateMax.M Date of the observed minimum
46- 47 I02 d DateMax.D Date of the observed minimum
49- 54 F6.3 Jy Smax Observed maximum flux density at 15GHz
56- 60 F5.3 Jy e_Smax Mean error on Smax (1)
--------------------------------------------------------------------------------
Note (1): including the 5% absolute calibration uncertainty
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- --- [0FGL]
6- 17 A12 --- 0FGL Source name
19- 22 F4.1 GHz Freq RATAN-600 central frequency
24- 28 F5.2 Jy Flux RATAN-600 flux density
30- 33 F4.2 Jy e_Flux Flux uncertainty
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- 0FGL Source name (JHHMM.m+DDMM)
14- 19 F6.3 [Hz] lognu Log of frequency (logν)
21- 27 F7.3 --- lognuFa Average intensity of the observed frequency
29- 35 F7.3 --- lognuFu Maximum intensity of the observed frequency (1)
37- 43 F7.3 --- lognuFl Minimum intensity of the observed frequency (1)
45- 48 I4 --- N Number of data available in the period (2)
--------------------------------------------------------------------------------
Note (1): Note that Columns 4 and 5 report the error bar extremes instead of
maximum and minimum values.
Note (2): When the number of data available is reported as "0" this indicates
that the data given in the table and shown in the SED plots are not
strictly inside the period (this happens for ON 231 and 3C 279 in the
optical, and for 3C 273 in both the optical and near-IR, because of
solar conjunction), but come from immediately outside and, due to the
smoothness of the light curve, they can represent the state in
between.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table13.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- 0FGL Source name (JHHMM/m+DDMM)
14- 16 A3 --- SED [Yes/ ] SED available?
18- 23 F6.3 --- alpha Radio power-law spectral index in the range
1-100GHz (αr)
25- 28 F4.1 [Hz] lognuS ? Peak frequency of the synchrotron component
estimated directly from SED
30- 33 F4.1 [Hz] lognuS2 ? Peak frequency of the synchrotron component
estimated from aox-aro (optical/x/radio)
35- 39 F5.1 [mW/m2] lognuSF ? Peak intensity of the synchrotron component
estimated directly from SED
41- 45 F5.1 [mW/m2] lognuSF2 ? Peak intensity of the synchrotron component
estimated from aox-aro
47- 50 F4.1 [Hz] lognuIC ? Peak frequency of the inverse Compton power
estimated directly from SED (νICpeak)
52- 55 F4.1 [Hz] lognuIC2 ? Peak frequency of the inverse Compton power
estimated from Equation 5 (1)
57- 61 F5.1 [mW/m2] lognuICF ? Peak intensity of the inverse Compton power
63- 65 F3.1 [-] loggam ? Particle peak energy (Lorentz factor) (2)
67- 70 F4.1 --- Cpt ? Compton dominance (3)
72- 74 A3 --- Class SED classification (Low, Intermediate or High
Synchrotron Peaked blazar; see section 6 for
further details)
76- 87 A12 --- OClass Optical spectrum classification (BL Lac, BZU
(blazar of unknown type), FSRQ or Unidentified)
--------------------------------------------------------------------------------
Note (1): The best fit to the νICpeak-Γ relationship is
log(νICpeak)=-4.0xΓ+31.6 with Γ, the γ-ray
spectral slope taken from Table 3 of Abdo et al. (2009,
Cat. J/ApJ/700/597). See section 5.5 for further details.
Note (2): Calculated assuming a simple SSC emission mechanism, i.e.,
γSSCpeak=(3/4xνICpeak/νSpeak)0.5.
See section 7.2 for further details.
Note (3): The Compton dominance:
νICpeakF(νICpeak)/νSpeakF(νSpeak)
--------------------------------------------------------------------------------
History:
* 23-May-2012: from electronic version of the journal
* 03-Jul-2012: added table6.dat (from H. Andernach, Guanajuato Univ.)
(End) Emmanuelle Perret [CDS] 23-May-2012