Radio–gamma-ray connection and spectral evolution in 4C +49.22 (S4 1150+49): the Fermi, Swift and Planck view

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dc.contributor.authorCutini, S.
dc.contributor.authorCiprini, S.
dc.contributor.authorOrienti, M.
dc.contributor.authorTramacere, A.
dc.contributor.authorD'Ammando, F.
dc.contributor.authorVerrecchia, F.
dc.contributor.authorPolenta, G.
dc.contributor.authorCarrasco, L.
dc.contributor.authorD'Elia, V.
dc.contributor.authorGiommi, P.
dc.contributor.authorGonzález-Nuevo, J.
dc.contributor.authorGrandi, P.
dc.contributor.authorHarrison, D.
dc.contributor.authorHays, E.
dc.contributor.authorLarsson, S.
dc.contributor.authorLähteenmäki, A.
dc.contributor.authorLeón-Tavares, J.
dc.contributor.authorLópez-Caniego, M.
dc.contributor.authorNatoli, P.
dc.contributor.authorOjha, R.
dc.contributor.authorPartridge, B.
dc.contributor.authorPorras, A.
dc.contributor.authorReyes, L.
dc.contributor.authorRecillas, E.
dc.contributor.authorTorresi, E.
dc.date.accessioned2020-04-27T13:41:56Z
dc.date.available2020-04-27T13:41:56Z
dc.date.issued2014-11-07
dc.description.abstractThe Large Area Telescope on board the Fermi Gamma-ray Space Telescope detected a strong γ-ray flare on 2011 May 15 from a source identified as 4C +49.22, a flat spectrum radio quasar (FSRQ) also known as S4 1150+49. This blazar, characterized by a prominent radio–optical–X-ray jet, was in a low γ-ray activity state during the first years of Fermi observations. Simultaneous observations during the quiescent, outburst and post-flare γ-ray states were obtained by Swift, Planck and optical–IR–radio telescopes (Instituto Nacional de Astrofísica, Óptica y Electrónica, Catalina Sky Survey, Very Long Baseline Array [VLBA], Metsähovi). The flare is observed from microwave to X-ray bands with correlated variability and the Fermi, Swift and Planck data for this FSRQ show some features more typical of BL Lac objects, like the synchrotron peak in the optical band that outshines the thermal blue-bump emission, and the X-ray spectral softening. Multi-epoch VLBA observations show the ejection of a new component close in time with the GeV γ-ray flare. The radio-to-γ-ray spectral energy distribution is modelled and fitted successfully for the outburst and the post-flare epochs using either a single flaring blob with two emission processes (synchrotron self-Compton (SSC), and external-radiation Compton), and a two-zone model with SSC-only mechanism.en_US
dc.description.sponsorshipWe thank Benjamin Walter who helped in the English revision of the paper. This research has made with the use of the online tool for the SED modelling developed by Tramacere online at ISDC10 and ASDC11 The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l'Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France. We acknowledge the entire Swift mission team for the help and support and especially the Swift Observatory Duty Scientists, ODSs, for their invaluable help and professional support with the planning and execution of the repeated ToO observations of this target source. The NASA Swift γ-ray burst Explorer is a MIDEX Gamma Ray Burst mission led by NASA with participation of Italy and the UK. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal) and DEISA (EU). The Metsähovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, and others). JGN acknowledges financial support from the Spanish CSIC for a JAE-DOC fellowship, co-funded by the European Social Fund, and by the Spanish Ministerio de Ciencia e Innovacion, AYA2012-39475-C02-01, and Consolider-Ingenio 2010, CSD2010-00064, projects. This research has made use of observations from the MOJAVE data base that is maintained by the MOJAVE team. The MOJAVE project is supported under National Science Foundation grant 0807860-AST and NASA-Fermi grant NNX08AV67G. The National Radio Astronomy Observatory (NRAO VLBA) is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of observations from the CSS. CSS is funded by the NASA under Grant No. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Program. The CRTS survey is supported by the U.S. National Science Foundation under grants AST-0909182. This research has made use of observations obtained with the 2.1-m telescope of the Observatorio Astrofísico Guillermo Haro (OAGH), in the state of Sonora, Mexico, operated by the Instituto Nacional de Astrofísica, Óptica y Electrónica (INAOE), Mexico. OAGH thanks funding from the INAOE Astrophysics Department. This research has made use of data and software facilities from the ASI Science Data Center (ASDC), managed by the Italian Space Agency (ASI).en_US
dc.description.urihttps://academic.oup.com/mnras/article/445/4/4316/1751393en_US
dc.format.extent19 pagesen_US
dc.genrejournal articlesen_US
dc.identifierdoi:10.13016/m2bzb1-pfqf
dc.identifier.citationS. Cutini, S. Ciprini, M. Orienti, A. Tramacere, F. D'Ammando, F. Verrecchia, G. Polenta, L. Carrasco, V. D'Elia, P. Giommi, J. González-Nuevo, P. Grandi, D. Harrison, E. Hays, S. Larsson, A. Lähteenmäki, J. León-Tavares, M. López-Caniego, P. Natoli, R. Ojha, B. Partridge, A. Porras, L. Reyes, E. Recillas, E. Torresi, Radio–gamma-ray connection and spectral evolution in 4C +49.22 (S4 1150+49): the Fermi, Swift and Planck view, Monthly Notices of the Royal Astronomical Society, Volume 445, Issue 4, 21 December 2014, Pages 4316–4334, https://doi.org/10.1093/mnras/stu2011en_US
dc.identifier.urihttps://doi.org/10.1093/mnras/stu2011
dc.identifier.urihttp://hdl.handle.net/11603/18291
dc.identifier.urihttp://simbad.u-strasbg.fr/simbad/sim-ref?querymethod=bib&simbo=on&submit=submit+bibcode&bibcode=2014MNRAS.445.4316C
dc.identifier.urihttps://ned.ipac.caltech.edu/cgi-bin/objsearch?search_type=Search&refcode=2014MNRAS.445.4316C
dc.identifier.urihttps://heasarc.gsfc.nasa.gov/xamin/xamin.jsp?bibcode=2014MNRAS%2E445%2E4316C
dc.language.isoen_USen_US
dc.publisherOxford University Pressen_US
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Physics Department Collection
dc.relation.ispartofUMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
dc.relation.ispartofUMBC Faculty Collection
dc.rightsThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
dc.rightsThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2014 2020 Oxford University Press Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
dc.titleRadio–gamma-ray connection and spectral evolution in 4C +49.22 (S4 1150+49): the Fermi, Swift and Planck viewen_US
dc.typeTexten_US

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