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dc.contributor.authorRani, B.en_US
dc.contributor.authorJorstad, Svetlana G.en_US
dc.contributor.authorMarscher, Alan P.en_US
dc.contributor.authorAgudo, I.en_US
dc.contributor.authorSokolovsky, K. V.en_US
dc.contributor.authorLarionov, V. M.en_US
dc.contributor.authorSmith, P.en_US
dc.contributor.authorMosunova, D. A.en_US
dc.contributor.authorBorman, G. A.en_US
dc.contributor.authorGrishina, T. S.en_US
dc.contributor.authorKopatskaya, E. N.en_US
dc.contributor.authorMokrushina, A. A.en_US
dc.contributor.authorMorozova, D. A.en_US
dc.contributor.authorSavchenko, S. S.en_US
dc.contributor.authorTroitskaya, Yu. V.en_US
dc.contributor.authorTroitsky, I. S.en_US
dc.contributor.authorThum, C.en_US
dc.contributor.authorMolina, S. N.en_US
dc.contributor.authorCasadio, C.en_US
dc.date.accessioned2019-02-15T14:36:03Z
dc.date.available2019-02-15T14:36:03Z
dc.date.issued2018-05-10
dc.identifierhttp://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000431818800008&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=6e74115fe3da270499c3d65c9b17d654
dc.identifier.citationB Rani, SG Jorstad, AP Marscher, I Agudo, KV Sokolovsky, VM Larionov, P Smith, DA Mosunova, GA Borman, TS Grishina, EN Kopatskaya, AA Mokrushina, DA Morozova, SS Savchenko, Yu V Troitskaya, IS Troitsky, C Thum, SN Molina, C Casadio. 2018. "Exploring the Connection between Parsec-scale Jet Activity and Broadband Outbursts in 3C 279." ASTROPHYSICAL JOURNAL, Volume 858, Issue 2, pp. ? - ? (15). https://doi.org/10.3847/1538-4357/aab785
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttps://hdl.handle.net/2144/33332
dc.description.abstractWe use a combination of high-resolution very long baseline interferometry (VLBI) radio and multiwavelength flux density and polarization observations to constrain the physics of the dissipation mechanism powering the broadband flares in 3C 279 during an episode of extreme flaring activity in 2013–2014. Six bright flares superimposed on a long-term outburst are detected at γ-ray energies. Four of the flares have optical and radio counterparts. The two modes of flaring activity (faster flares sitting on top of a long-term outburst) present at radio, optical, and γ-ray frequencies are missing in X-rays. X-ray counterparts are only observed for two flares. The first three flares are accompanied by ejection of a new VLBI component (NC2), suggesting the 43 GHz VLBI core as the site of energy dissipation. Another new component, NC3, is ejected after the last three flares, which suggests that the emission is produced upstream from the core (closer to the black hole). The study therefore indicates multiple sites of energy dissipation in the source. An anticorrelation is detected between the optical percentage polarization (PP) and optical/γ-ray flux variations, while the PP has a positive correlation with optical/γ-ray spectral indices. Given that the mean polarization is inversely proportional to the number of cells in the emission region, the PP versus optical/γ-ray anticorrelation could be due to more active cells during the outburst than at other times. In addition to the turbulent component, our analysis suggests the presence of a combined turbulent and ordered magnetic field, with the ordered component transverse to the jet axis.en_US
dc.description.sponsorshipThe 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 a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire 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, Swedish Research Council, and 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'Etudes Spatiales in France. This work was performed in part under DOE Contract DE-AC02-76SF00515.This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by the Universities Space Research Association through a contract with NASA. This study makes use of 43 GHz VLBA data from the VLBA-BU Blazar Monitoring Program (VLBA-BU-BLAZAR;. http://www.bu.edu/blazars/VLBAproject.html), funded by NASA through the Fermi Guest Investigator Program. The VLBA is an instrument of the Long Baseline Observatory. The Long Baseline Observatory is a facility of the National Science Foundation operated by Associated Universities, Inc. The BU group acknowledges support from US National Science Foundation grant AST-1615796. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This research was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by the Universities Space Research Association through a contract with NASA. KS is supported by the Russian Science Foundation grant 16-12-10481. The St. Petersburg University team acknowledges support from Russian Science Foundation grant 17-12-01029. This research has made use of data from the OVRO 40 m monitoring program (Richards et al. 2011), which is supported in part by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G and NSF grants AST-0808050 and AST-1109911. IA acknowledges support by a Ramon y Cajal grant of the Ministerio de Economia, Industria, y Competitividad (MINECO) of Spain. Acquisition and reduction of the POLAMI data was supported in part by MINECO through grants AYA2010-14844, AYA2013-40825-P, and AYA2016-80889-P and by the Regional Government of Andalucia through grant P09-FQM-4784. The POLAMI observations were carried out at the IRAM 30 m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). BR acknowledges the help of Roopesh Ojha, Marcello Giroletti, and Dave Thompson for fruitful discussions and comments that improved the manuscript. (Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; DE-AC02-76SF00515 - DOE; NASA Postdoctoral Program at the Goddard Space Flight Center; NASA through the Fermi Guest Investigator Program; AST-1615796 - US National Science Foundation; Smithsonian Institution; Academia Sinica; 16-12-10481 - Russian Science Foundation; 17-12-01029 - Russian Science Foundation; NNX08AW31G - NASA; NNX11A043G - NASA; NNX14AQ89G - NASA; AST-0808050 - NSF; AST-1109911 - NSF; Ramon y Cajal grant of the Ministerio de Economia, Industria, y Competitividad (MINECO) of Spain; AYA2010-14844 - MINECO; AYA2013-40825-P - MINECO; AYA2016-80889-P - MINECO; P09-FQM-4784 - Regional Government of Andalucia; INSU/CNRS (France); MPG (Germany); GN (Spain))en_US
dc.format.extentp. 15en_US
dc.languageEnglish
dc.language.isoen_US
dc.publisherIOP Publishing LTDen_US
dc.relation.ispartofAstrophysical Journal
dc.subjectScience & technologyen_US
dc.subjectPhysical sciencesen_US
dc.subjectAstronomy & astrophysicsen_US
dc.subjectGalaxies: activeen_US
dc.subjectQuasars: individual (3C 279)en_US
dc.subjectRadio continuum: galaxiesen_US
dc.subjectGalaxies: jetsen_US
dc.subjectGamma rays: galaxiesen_US
dc.subjectGamma-rayen_US
dc.subjectGalactic nucleien_US
dc.subjectMillimeter wavelengthsen_US
dc.subjectEnergy-distributionen_US
dc.subjectQuasar 3C 279en_US
dc.subjectLight curvesen_US
dc.subjectRadioen_US
dc.subjectTelescopeen_US
dc.subjectVariabilityen_US
dc.subjectPolarizationen_US
dc.subjectAstronomical and space sciencesen_US
dc.subjectOrganic chemistryen_US
dc.subjectPhysical chemistry (incl. structural)en_US
dc.titleExploring the connection between Parsec-scale jet activity and broadband outbursts in 3C 279en_US
dc.typeArticleen_US
dc.description.versionAccepted manuscripten_US
dc.identifier.doi10.3847/1538-4357/aab785
pubs.elements-sourceweb-of-scienceen_US
pubs.notesEmbargo: No embargoen_US
pubs.organisational-groupBoston Universityen_US
pubs.organisational-groupBoston University, College of Arts & Sciencesen_US
pubs.organisational-groupBoston University, College of Arts & Sciences, Department of Astronomyen_US
pubs.publication-statusPublisheden_US
dc.identifier.orcid0000-0001-7396-3332 (Marscher, AP)


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