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The simultaneous low state spectral energy distribution of 1ES 2344+514 from radio to very high energies

Aleksić, J. and Moerbeck, W. Max and Readhead, A. C. S. (2013) The simultaneous low state spectral energy distribution of 1ES 2344+514 from radio to very high energies. Astronomy and Astrophysics, 556 . Art. No. A67. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20131004-102711113

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Abstract

Context. BL Lacertae objects are variable at all energy bands on time scales down to minutes. To construct and interpret their spectral energy distribution (SED), simultaneous broad-band observations are mandatory. Up to now, the number of objects studied during such campaigns is very limited and biased towards high flux states. Aims. We present the results of a dedicated multi-wavelength study of the high-frequency peaked BL Lacertae (HBL) object and known TeV emitter 1ES 2344+514 by means of a pre-organised campaign. Methods. The observations were conducted during simultaneous visibility windows of MAGIC and AGILE in late 2008. The measurements were complemented by Metsähovi, RATAN-600, KVA+Tuorla, Swift and VLBA pointings. Additional coverage was provided by the ongoing long-term F-GAMMA and MOJAVE programs, the OVRO 40-m and CrAO telescopes as well as the Fermi satellite. The obtained SEDs are modelled using a one-zone as well as a self-consistent two-zone synchrotron self-Compton model. Results. 1ES 2344+514 was found at very low flux states in both X-rays and very high energy gamma rays. Variability was detected in the low frequency radio and X-ray bands only, where for the latter a small flare was observed. The X-ray flare was possibly caused by shock acceleration characterised by similar cooling and acceleration time scales. MOJAVE VLBA monitoring reveals a static jet whose components are stable over time scales of eleven years, contrary to previous findings. There appears to be no significant correlation between the 15 GHz and R-band monitoring light curves. The observations presented here constitute the first multi-wavelength campaign on 1ES 2344+514 from radio to VHE energies and one of the few simultaneous SEDs during low activity states. The quasi-simultaneous Fermi-LAT data poses some challenges for SED modelling, but in general the SEDs are described well by both applied models. The resulting parameters are typical for TeV emitting HBLs. Consequently it remains unclear whether a so-called quiescent state was found in this campaign.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201220714DOIArticle
http://www.aanda.org/articles/aa/abs/2013/08/aa20714-12/aa20714-12.htmlPublisherArticle
http://arxiv.org/abs/1211.2608arXivDiscussion Paper
Additional Information:© 2013 ESO. Received 9 November 2012. Accepted 22 April 2013. Published online 31 July 2013. We would like to thank the anonymous referee for constructive comments. The MAGIC Collaboration would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence “Origin and Structure of the Universe”, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. The AGILE Mission is funded by the Italian Space Agency (ASI), with scientific and programmatic participation by the Italian Institute of Astrophysics (INAF) and the Italian Institute of Nuclear Physics (INFN). Research partially supported through the ASI grants no. I/089/06/2 and I/042/10/0. The Fermi-LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. We gratefully acknowledge the entire Swift team, the duty scientists and science planners for the dedicated support, making these observations possible. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. This research is partly based on observations with the 100-m telescope of the MPIfR (Max-Planck-Institut für Radioastronomie) at Effelsberg and has made use of observations with the IRAM 30-m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). The Metsähovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). This research has made use of data from the MOJAVE database that is maintained by the MOJAVE team (Lister et al. 2009a). The MOJAVE project is supported under NASA-Fermi grant NNX08AV67G. The VLBA is a facility of the National Science Foundation operated by the National Radio Astronomy Observatory under cooperative agreement with Associated Universities, Inc. This work made use of the Swinburne University of Technology software correlator, developed as part of the Australian Major National Research Facilities Programme and operated under licence. RATAN-600 operations were carried out with the financial support of the Ministry of Education and Science of the Russian Federation (contracts 16.518.11.7062 and 16.552.11.7028). This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of NASA’s Astrophysics Data System. Part of this work is based on archival data, software or on-line services provided by the ASI Science Data Center (ASDC). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of SAOImage DS9, developed by Smithsonian Astrophysical Observatory. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. Y.A.K., Y.Y.K., and K.V.S. were supported in part by the Russian Foundation for Basic Research (projects 11-02-00368, 12-02-33101), the basic research program “Active processes in galactic and extragalactic objects” of the Physical Sciences Division of the Russian Academy of Sciences, and the Ministry of Education and Science of the Russian Federation (agreement No. 8405). Y.Y.K. was also supported by the Dynasty Foundation.
Funders:
Funding AgencyGrant Number
Max-Planck-GesellschaftUNSPECIFIED
Istituto Nazionale di Fisica Nucleare (INFN)UNSPECIFIED
Swiss National Science Foundation (SNF)UNSPECIFIED
Ministerio de Ciencia e Innovación (MICINN)UNSPECIFIED
CPANCSD2007-00042
MultiDarkCSD2009-00064
Spanish Consolider-Ingenio 2010 programmeUNSPECIFIED
Academy of Finland127740
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Deutsche Forschungsgemeinschaft (DFG)SFB823/C4
Deutsche Forschungsgemeinschaft (DFG)SFB876/C3
MNiSW (Poland)745/N-HESS-MAGIC/2010/0
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)I/089/06/2
Agenzia Spaziale Italiana (ASI)I/042/10/0
NASAUNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
CEA/Irfu (France)UNSPECIFIED
IN2P3/CNRS (France)UNSPECIFIED
Ministry of Education, Culture, Sports, Science and Technology (MEXT)UNSPECIFIED
KEK (Japan)UNSPECIFIED
Japan Aerospace Exploration Agency (JAXA)UNSPECIFIED
K. A. Wallenberg FoundationUNSPECIFIED
Swedish Research Council and the National Space BoardUNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Institut national des sciences de l'Univers (INSU)UNSPECIFIED
Instituto Geográfico Nacional (IGN)UNSPECIFIED
Academy of Finland212656
Academy of Finland210338
Academy of Finland121148
NASANNX08AV67G
Ministry of Education and Science of the Russian Federation 16.518.11.7062
Ministry of Education and Science of the Russian Federation 16.552.11.7028
NASA/JPL/CaltechUNSPECIFIED
Russian Foundation for Basic Research 11-02-00368
Russian Foundation for Basic Research 12-02-33101
Russian Academy of SciencesUNSPECIFIED
Ministry of Education and Science of the Russian Federation agreement no.8405
Dynasty FoundationUNSPECIFIED
Bundesministerium für Bildung und Frauen (BMBF)UNSPECIFIED
Subject Keywords:galaxies: active; BL Lacertae objects: individual: 1ES 2344+514; gamma rays: galaxies; X-rays: individuals: 1ES 2344+514; radiation mechanisms: non-thermal
Record Number:CaltechAUTHORS:20131004-102711113
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20131004-102711113
Official Citation:The simultaneous low state spectral energy distribution of 1ES 2344+514 from radio to very high energies A67 J. Aleksić, L. A. Antonelli, P. Antoranz, M. Asensio, M. Backes, U. Barres de Almeida, J. A. Barrio, W. Bednarek, K. Berger, E. Bernardini, et al. (182 more) Published online: 31 July 2013 DOI: http://dx.doi.org/10.1051/0004-6361/201220714
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:41681
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:04 Oct 2013 18:26
Last Modified:03 Oct 2019 05:51

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