J/ApJ/783/83ivo://CDS.VizieR/J/ApJ/783/83doi:10.26093/cds/vizier.17830083CDSLiao N.H.Bai J.M.Liu H.T.Weng S.S.Chen L.Li F.2017-07-06T06:26:15Z2016-04-15T09:34:41ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frbl-lacertae-objectsinfrared-photometryvisible-astronomybroad-band-photometryS5 0716+714 is a typical BL Lacertae object. In this paper we present the analysis and results of long-term simultaneous observations in the radio, near-infrared, optical, X-ray, and {gamma}-ray bands, together with our own photometric observations for this source. The light curves show that the variability amplitudes in {gamma}-ray and optical bands are larger than those in the hard X-ray and radio bands and that the spectral energy distribution (SED) peaks move to shorter wavelengths when the source becomes brighter, which is similar to other blazars, i.e., more variable at wavelengths shorter than the SED peak frequencies. Analysis shows that the characteristic variability timescales in the 14.5GHz, the optical, the X-ray, and the {gamma}-ray bands are comparable to each other. The variations of the hard X-ray and 14.5GHz emissions are correlated with zero lag, and so are the V band and {gamma}-ray variations, which are consistent with the leptonic models. Coincidences of {gamma}-ray and optical flares with a dramatic change of the optical polarization are detected. Hadronic models do not have the same natural explanation for these observations as the leptonic models. A strong optical flare correlating a {gamma}-ray flare whose peak flux is lower than the average flux is detected. The leptonic model can explain this variability phenomenon through simultaneous SED modeling. Different leptonic models are distinguished by average SED modeling. The synchrotron plus synchrotron self-Compton (SSC) model is ruled out because of the extreme input parameters. Scattering of external seed photons, such as the hot-dust or broad-line region emission, and the SSC process are probably both needed to explain the {gamma}-ray emission of S5 0716+714.2014ApJ...783...83Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/783/83CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJS/218/18 : 2004-2012 BVRI observations of blazar S5 0716+714 (Dai+, 2015)J/A+A/558/A92 : S5 0716+714 microvariability observation (Bhatta+, 2013)J/ApJS/199/31 : Fermi LAT second source catalog (2FGL) (Nolan+, 2012)J/AJ/143/108 : B'V'R' photometry of the BL Lac object S5 0716+714 (Wu+, 2012)J/ApJ/743/171 : The 2LAC catalog (Ackermann+, 2011)J/ApJ/716/30 : SED of Fermi bright blazars (Abdo+, 2010)J/ApJ/715/429 : First Fermi-LAT AGN catalog (1LAC) (Abdo+, 2010)J/ApJS/188/405 : Fermi-LAT first source catalog (1FGL) (Abdo+, 2010)J/ApJ/700/597 : FERMI LAT detected blazars (Abdo+, 2009)J/ApJS/185/511 : Optical microvariability of S5 0716+714 (Poon+, 2009)J/AJ/136/1846 : BVRI light curves of S5 0716+714 (Zhang+, 2008)J/AJ/133/1599 : B'V'R' photometry of S5 0716+714 (Wu+, 2007)J/AZh/83/310 : BV(RI)c photometry of S5 0716+714 (Amirkhanyan+, 2006)J/A+A/451/435 : BV(RI)c photometry of S5 0716+714 (Montagni+, 2006)J/AJ/129/1818 : Photometry of S5 0716+714 (Wu+, 2005)J/A+A/402/151 : S5 0716+714 UBVRI photometry (Raiteri+, 2003)J/A+AS/136/455 : BVRI photometry of 3 BL Lac objects (Bai+, 1999)J/A+AS/132/83 : BVRI photometry of 7 BL Lac objects (Bai+ 1998)J/A+A/327/61 : BV(RI)c photometry of S5 0716+714 (Ghisellini+ 1997)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/783/83https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/783/83http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/783/83https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/783/83https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/783/83http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/783/83GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapInfraredOpticaldefaultJ/ApJ/783/83/table1Multiband photometric data from Yunnan observatoriesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJDModified Julian date of the observationdtime.epochfloat<mag>[12.3/14.7] Nightly averaged magnitude in Flt (1)magphot.magfloate_<mag>[0.002/0.05] Uncertainty in <mag>magstat.error;phot.magfloatFlt[BVRI] Filter used in the observation (B, V, R, I)instr.setup;obschar