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Sökning: WFRF:(Smith Geoffrey) > (2020-2024) > The slow demise of ...

LIBRIS Formathandbok  (Information om MARC21)
FältnamnIndikatorerMetadata
00003837naa a2200565 4500
001oai:DiVA.org:su-187872
003SwePub
008210107s2020 | |||||||||||000 ||eng|
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-1878722 URI
0247 a https://doi.org/10.1093/mnras/staa23242 DOI
040 a (SwePub)su
041 a engb eng
042 9 SwePub
072 7a ref2 swepub-contenttype
072 7a art2 swepub-publicationtype
1001 a Fox, Ori D.4 aut
2451 0a The slow demise of the long-lived SN 2005ip
264 c 2020-08-11
264 1b Oxford University Press (OUP),c 2020
338 a print2 rdacarrier
520 a The Type IIn supernova (SN IIn) 2005ip is one of the most well-studied and long-lasting examples of an SN interacting with its circumstellar environment. The optical light curve plateaued at a nearly constant level for more than five years, suggesting ongoing shock interaction with an extended and clumpy circumstellar medium (CSM). Here, we present continued observations of the SN from ∼1000 to 5000 d post-explosion at all wavelengths, including X-ray, ultraviolet, near-infrared (NIR), and mid-infrared. The UV spectra probe the pre-explosion mass loss and show evidence for CNO processing. From the bolometric light curve, we find that the total radiated energy is in excess of 1050 erg, the progenitor star’s pre-explosion mass-loss rate was ≳1×10−2M⊙ yr−1⁠, and the total mass lost shortly before explosion was ≳1M⊙⁠, though the mass lost could have been considerably larger depending on the efficiency for the conversion of kinetic energy to radiation. The ultraviolet through NIR spectrum is characterized by two high-density components, one with narrow high-ionization lines, and one with broader low-ionization H i, He i, [O i], Mg ii, and Fe ii lines. The rich Fe ii spectrum is strongly affected by Lyα fluorescence, consistent with spectral modelling. Both the Balmer and He i lines indicate a decreasing CSM density during the late interaction period. We find similarities to SN 1988Z, which shows a comparable change in spectrum at around the same time during its very slow decline. These results suggest that, at long last, the shock interaction in SN 2005ip may finally be on the decline.
650 7a NATURVETENSKAPx Fysik0 (SwePub)1032 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciences0 (SwePub)1032 hsv//eng
653 a circumstellar matter
653 a dust
653 a extinction
653 a infrared: stars
7001 a Fransson, Claesu Stockholms universitet,Oskar Klein-centrum för kosmopartikelfysik (OKC),Institutionen för astronomi4 aut0 (Swepub:su)frans
7001 a Smith, Nathan4 aut
7001 a Andrews, Jennifer4 aut
7001 a Bostroem, K. Azalee4 aut
7001 a Brink, Thomas G.4 aut
7001 a Cenko, S. Bradley4 aut
7001 a Clayton, Geoffrey C.4 aut
7001 a Filippenko, Alexei4 aut
7001 a Fong, Wen-fai4 aut
7001 a Gallagher, Joseph S.4 aut
7001 a Kelly, Patrick L.4 aut
7001 a Kilpatrick, Charles D.4 aut
7001 a Mauerhan, Jon C.4 aut
7001 a Miller, Adam M.4 aut
7001 a Montiel, Edward4 aut
7001 a Stritzinger, Maximilian D.4 aut
7001 a Szalai, Tamas4 aut
7001 a Van Dyk, Schuyler D.4 aut
7102 a Stockholms universitetb Oskar Klein-centrum för kosmopartikelfysik (OKC)4 org
7730 t Monthly notices of the Royal Astronomical Societyd : Oxford University Press (OUP)g 498:1, s. 517-531q 498:1<517-531x 0035-8711x 1365-2966
8564 u https://authors.library.caltech.edu/106998/1/staa2324.pdf
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-187872
8564 8u https://doi.org/10.1093/mnras/staa2324

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