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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 (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). 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
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=(3/4xνICpeakSpeak)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
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