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INVERSE COMPTON X-R...
INVERSE COMPTON X-RAY EMISSION FROM SUPERNOVAE WITH COMPACT PROGENITORS : APPLICATION TO SN2011fe
- Article/chapterEnglish2012
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Numbers
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LIBRIS-ID:oai:DiVA.org:su-79880
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https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-79880URI
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https://doi.org/10.1088/0004-637X/751/2/134DOI
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Language:English
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Summary in:English
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Subject category:ref swepub-contenttype
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Subject category:art swepub-publicationtype
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AuthorCount:42;
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We present a generalized analytic formalism for the inverse Compton X-ray emission from hydrogen-poor supernovae and apply this framework to SN 2011fe using Swift X-Ray Telescope (XRT), UVOT, and Chandra observations. We characterize the optical properties of SN 2011fe in the Swift bands and find them to be broadly consistent with a normal SN Ia, however, no X-ray source is detected by either XRT or Chandra. We constrain the progenitor system mass-loss rate (M) over dot < 2 x 10(-9) M-circle dot yr(-1) (3 sigma c.l.) for wind velocity v(w) = 100 km s(-1). Our result rules out symbiotic binary progenitors for SN 2011fe and argues against Roche lobe overflowing subgiants and main-sequence secondary stars if greater than or similar to 1% of the transferred mass is lost at the Lagrangian points. Regardless of the density profile, the X-ray non-detections are suggestive of a clean environment (n(CSM) < 150 cm(-3)) for 2 x 10(15) less than or similar to R less than or similar to 5 x 10(16) cm around the progenitor site. This is either consistent with the bulk of material being confined within the binary system or with a significant delay between mass loss and supernova explosion. We furthermore combine X-ray and radio limits from Chomiuk et al. to constrain the post-shock energy density in magnetic fields. Finally, we searched for the shock breakout pulse using gamma-ray observations from the Interplanetary Network and find no compelling evidence for a supernova-associated burst. Based on the compact radius of the progenitor star we estimate that the shock breakout pulse was likely not detectable by current satellites.
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Soderberg, A. M.
(author)
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Chomiuk, L.
(author)
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Chevalier, R.
(author)
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Hurley, K.
(author)
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Milisavljevic, D.
(author)
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Foley, R. J.
(author)
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Hughes, J. P.
(author)
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Slane, P.
(author)
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Fransson, ClaesStockholms universitet,Institutionen för astronomi(Swepub:su)frans
(author)
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Moe, M.
(author)
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Barthelmy, S.
(author)
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Boynton, W.
(author)
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Briggs, M.
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Connaughton, V.
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Costa, E.
(author)
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Cummings, J.
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Del Monte, E.
(author)
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Enos, H.
(author)
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Fellows, C.
(author)
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Feroci, M.
(author)
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Fukazawa, Y.
(author)
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Gehrels, N.
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Goldsten, J.
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Golovin, D.
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Hanabata, Y.
(author)
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Harshman, K.
(author)
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Krimm, H.
(author)
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Litvak, M. L.
(author)
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Makishima, K.
(author)
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Marisaldi, M.
(author)
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Mitrofanov, I. G.
(author)
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Murakami, T.
(author)
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Ohno, M.
(author)
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Palmer, D. M.
(author)
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Sanin, A. B.
(author)
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Starr, R.
(author)
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Svinkin, D.
(author)
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Takahashi, T.
(author)
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Tashiro, M.
(author)
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Terada, Y.
(author)
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Yamaoka, K.
(author)
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Stockholms universitetInstitutionen för astronomi
(creator_code:org_t)
Related titles
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In:Astrophysical Journal751:2, s. 134-0004-637X1538-4357
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- By the author/editor
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Margutti, R.
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Soderberg, A. M.
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Chomiuk, L.
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Chevalier, R.
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Hurley, K.
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Milisavljevic, D ...
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show more...
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Foley, R. J.
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Hughes, J. P.
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Slane, P.
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Fransson, Claes
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Moe, M.
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Barthelmy, S.
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Boynton, W.
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Briggs, M.
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Connaughton, V.
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Costa, E.
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Cummings, J.
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Del Monte, E.
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Enos, H.
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Fellows, C.
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Feroci, M.
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Fukazawa, Y.
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Gehrels, N.
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Goldsten, J.
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Golovin, D.
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Hanabata, Y.
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Harshman, K.
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Krimm, H.
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Litvak, M. L.
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Makishima, K.
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Marisaldi, M.
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Mitrofanov, I. G ...
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Murakami, T.
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Ohno, M.
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Palmer, D. M.
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Sanin, A. B.
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Starr, R.
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Svinkin, D.
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Takahashi, T.
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Tashiro, M.
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Terada, Y.
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Yamaoka, K.
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- NATURAL SCIENCES
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Stockholm University