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|Title:||Ten years of INTEGRAL observations of the hard X-ray emission from SGR 1900+14||Authors:||Ducci, L.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||583||First Page:||A113||Abstract:||We exploited the high sensitivity of the INTEGRAL IBIS/ISGRI instrument to study the persistent hard X-ray emission of the soft gamma-ray repeater SGR 1900+14, based on ~11.6 Ms of archival data. The 22-150 keV INTEGRAL spectrum can be well fitted by a power law with photon index 1.9 ± 0.3 and flux F<SUB>x</SUB> = (1.11 ± 0.17) × 10<SUP>-11</SUP> erg cm<SUP>-2</SUP> s<SUP>-1</SUP> (20-100 keV). A comparison with the 20-100 keV flux measured in 1997 with BeppoSAX, and possibly associated with SGR 1900+14, shows a luminosity decrease by a factor of ~5. The slope of the power law above 20 keV is consistent within the uncertainties with that of SGR 1806-20, the other persistent soft gamma-ray repeater for which a hard X-ray emission extending up to 150 keV has been reported.||Acknowledgments:||We thank the anonymous referee for constructive comments that helped to improve the paper. This work is partially supported by the Bundesministerium für Wirtschaft und Technologie through the Deutsches Zentrum für Luft und Raumfahrt (grant FKZ 50 OG 1301). This work has been partially supported through financial contribution from the agreement ASI/INAF I/037/12/0 and from PRIN INAF 2014. This paper is based on data from observations with INTEGRAL, and XMM-Newton . INTEGRAL is an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Spain, and Switzerland), Czech Republic and Poland, and with the participation of Russia and the USA. XMM-Newton is an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. This research has made use of SAOImage DS9, developed by Smithsonian Astrophysical Observatory.||URI:||http://hdl.handle.net/20.500.12386/23661||URL:||https://www.aanda.org/articles/aa/abs/2015/11/aa27029-15/aa27029-15.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201527029||Bibcode ADS:||2015A&A...583A.113D||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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