γ-RAY AND PARSEC-SCALE JET PROPERTIES OF A COMPLETE SAMPLE OF BLAZARS FROM THE MOJAVE PROGRAM
M. L. ListerDepartment of Physics, Purdue University, 525 Northwestern Avenue, West Lafayette, IN 47907, USAM. F. AllerDepartment of Astronomy, University of Michigan, 817 Dennison Building, Ann Arbor, MI 48 109, USAH. D. AllerDepartment of Astronomy, University of Michigan, 817 Dennison Building, Ann Arbor, MI 48 109, USAT. HovattaDepartment of Physics, Purdue University, 525 Northwestern Avenue, West Lafayette, IN 47907, USAK. I. KellermannNational Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USAY. Y. KovalevMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, GermanyEileen T. MeyerDepartment of Physics and Astronomy, Rice University, Houston, TX 77005, USAA. B. PushkarevCrimean Astrophysical Observatory, 98409 Nauchny, Crimea, UkraineE. RosDepartament d'Astronomia i Astrofísica, Universitat de València, E-46100 Burjassot, Valéncia, SpainM. AckermannKavli Institute for Particle Astrophysics and CosmologyE. AntoliniDipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, ItalyL. BaldiniIstituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, ItalyJ. BalletUniversité Paris CitéG. BarbielliniDipartimento di Fisica, Università di Trieste, I-34127 Trieste, ItalyD. BastieriDipartimento di Fisica "G. Galilei," Università di Padova, I-35131 Padova, ItalyK. BechtolW. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USAR. BellazziniIstituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, ItalyB. BerenjiW. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USAR. D. BlandfordStanford UniversityE. D. BloomW. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USAMoritz BoeckDr. Remeis-Sternwarte Bamberg & ECAP, Sternwartstrasse 7, D-96049 Bamberg, GermanyE. BonamenteDipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, ItalyA. W. BorglandW. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USAJ. BregeonIstituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, ItalyM. BrigidaIstituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, ItalyP. BruelLaboratoire Leprince-Ringuet, École polytechnique, CNRS/IN2P3, Palaiseau, FranceR. BuehlerStanford UniversityS. BusonIstituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, ItalyG. A. CaliandroInstitut de Ciències de l'Espai (IEEE-CSIC), Campus UAB, 08193 Barcelona, SpainR. A. CameronStanford UniversityP. A. CaraveoINAF-Istituto di Astrofisica Spaziale e Fisica Cosmica, I-20133 Milano, ItalyJ. M. CasandjianCEA Paris-SaclayE. CavazzutiAgenzia Spaziale Italiana (ASI) Science Data Center, I-00044 Frascati (Roma), ItalyC. CecchiDipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, ItalyChin-Shin ChangMax-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, GermanyE. CharlesW. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USAA. ChekhtmanC. C. CheungNational Academies of Sciences, Engineering, and MedicineJ. ChiangStanford UniversityS. CipriniASI Science Data Center, I-00044 Frascati (Roma), ItalyR. ClausKavli Institute for Particle Astrophysics and CosmologyJ. Cohen-TanugiUniversité de MontpellierJ. M. ConradDepartment of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, SwedenS. CutiniAgenzia Spaziale Italiana (ASI) Science Data Center, I-00044 Frascati (Roma), ItalyF. de PalmaDipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, ItalyC. D. DermerSpace Science Division, Naval Research Laboratory, Washington, DC 20375-5352, USAE. do Couto e SilvaW. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USAP. S. DrellKavli Institute for Particle Astrophysics and CosmologyA. Drlica-WagnerStanford UniversityC. FavuzziDipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, ItalyS. FeganLaboratoire Leprince-RinguetE. C. FerraraNASA Goddard Space Flight Center, Greenbelt, MD 20771, USAJ. FinkeSpace Science Division, Naval Research Laboratory, Washington, DC 20375-5352, USAW. B. FockeStanford UniversityP. FortinLaboratoire Leprince-Ringuet, École polytechnique, CNRS/IN2P3, Palaiseau, FranceY. FukazawaDepartment of Physical Sciences, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, JapanP. FuscoIstituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, ItalyF. GarganoIstituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, ItalyD. GasparriniAgenzia Spaziale Italiana (ASI) Science Data Center, I-00044 Frascati (Roma), ItalyN. GehrelsNASA Goddard Space Flight Center, Greenbelt, MD 20771, USAS. GermaniIstituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, ItalyN. GigliettoIstituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, ItalyF. GiordanoDipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, ItalyM. GirolettiINAF Istituto di Radioastronomia, 40129 Bologna, ItalyT. GlanzmanStanford UniversityG. GodfreyKavli Institute for Particle Astrophysics and CosmologyI. A. GrenierCommissariat à l'Énergie Atomique et aux Énergies AlternativesS. GuiriecCenter for Space Plasma and Aeronomic Research (CSPAR), University of Alabama in Huntsville, Huntsville, AL 35899, USAD. HadaschInstitut de Ciències de l'Espai (IEEE-CSIC), Campus UAB, 08193 Barcelona, SpainM. HayashidaStanford UniversityE. HaysNASA Goddard Space Flight Center, Greenbelt, MD 20771, USAD. HoranÉcole PolytechniqueR. E. HughesDepartment of Physics, Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USAG. JóhannessonScience Institute, University of Iceland, IS-107 Reykjavik, IcelandA. S. JohnsonW. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USAM. KadlerDr. Remeis-Sternwarte Bamberg & ECAP, Sternwartstrasse 7, D-96049 Bamberg, GermanyH. KatagiriCollege of Science, Ibaraki University, 2-1-1, Bunkyo, Mito 310-8512, JapanJ. KataokaResearch Institute for Science and Engineering, Waseda University, 3-4-1, Okubo, Shinjuku, Tokyo 169-8555, JapanJ. KnödlsederInstitut de Recherche en Astrophysique et PlanétologieM. KussIstituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, ItalyJ. LandéStanford UniversityF. LongoDipartimento di Fisica, Università di Trieste, I-34127 Trieste, ItalyF. LoparcoDipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, ItalyB. LottCNRS/IN2p3, Centre d'Études Nucléaires de Bordeaux Gradignan, Université Bordeaux 1, 33175 Gradignan, FranceM. N. LovelletteSpace Science Division, Naval Research Laboratory, Washington, DC 20375-5352, USAP. LubranoDipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, ItalyG. M. MadejskiStanford UniversityM. N. MazziottaIstituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, ItalyW. McConvilleDepartment of Physics and Department of Astronomy, University of Maryland, College Park, MD 20742, USAJ. E. McEneryDepartment of Physics and Department of Astronomy, University of Maryland, College Park, MD 20742, USAJ. MéhaultLaboratoire Univers et Particules de MontpellierP. F. MichelsonKavli Institute for Particle Astrophysics and CosmologyTsunefumi MizunoDepartment of Physical Sciences, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, JapanC. MonteDipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, ItalyM. E. MonzaniStanford UniversityA. MorselliIstituto Nazionale di Fisica Nucleare, Sezione di Roma "Tor Vergata," I-00133 Roma, ItalyI. V. MoskalenkoW. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USAS. MurgiaStanford UniversityM. Naumann-GodóUniversité Paris CitéS. NishinoDepartment of Physical Sciences, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan
2011en
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Annotatsiya
We investigate the Fermi Large Area Telescope γ-ray and 15 GHz Very Long Baseline Array radio properties of a joint γ-ray and radio-selected sample of active galactic nuclei (AGNs) obtained during the first 11 months of the Fermi mission (2008 August 4-2009 July 5). Our sample contains the brightest 173 AGNs in these bands above declination –30° during this period, and thus probes the full range of γ-ray loudness (γ-ray to radio band luminosity ratio) in the bright blazar population. The latter quantity spans at least 4 orders of magnitude, reflecting a wide range of spectral energy distribution (SED) parameters in the bright blazar population. The BL Lac objects, however, display a linear correlation of increasing γ-ray loudness with synchrotron SED peak frequency, suggesting a universal SED shape for objects of this class. The synchrotron self-Compton model is favored for the γ-ray emission in these BL Lac objects over external seed photon models, since the latter predict a dependence of Compton dominance on Doppler factor that would destroy any observed synchrotron SED-peak-γ-ray-loudness correlation. The high-synchrotron peaked (HSP) BL Lac objects are distinguished by lower than average radio core brightness temperatures, and none display large radio modulation indices or high linear core polarization levels. No equivalent trends are seen for the flat-spectrum radio quasars (FSRQs) in our sample. Given the association of such properties with relativistic beaming, we suggest that the HSP BL Lac objects have generally lower Doppler factors than the lower-synchrotron peaked BL Lac objects or FSRQs in our sample.
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