WFRF:(Cowperthwaite P. S.)
Sökning: WFRF:(Cowperthwaite P. S.) > (2016) > PS1-14bj :
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| Fältnamn | Indikatorer | Metadata |
|---|---|---|
| 000 | 04038naa a2200661 4500 | |
| 001 | oai:DiVA.org:su-143863 | |
| 003 | SwePub | |
| 008 | 170605s2016 | |||||||||||000 ||eng| | |
| 024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-1438632 URI |
| 024 | 7 | a https://doi.org/10.3847/0004-637X/831/2/1442 DOI |
| 040 | a (SwePub)su | |
| 041 | a engb eng | |
| 042 | 9 SwePub | |
| 072 | 7 | a ref2 swepub-contenttype |
| 072 | 7 | a art2 swepub-publicationtype |
| 100 | 1 | a Lunnan, R.4 aut |
| 245 | 1 0 | a PS1-14bj :b A HYDROGEN-POOR SUPERLUMINOUS SUPERNOVA WITH A LONG RISE AND SLOW DECAY |
| 264 | 1 | c 2016 |
| 338 | a print2 rdacarrier | |
| 520 | a We present photometry and spectroscopy of PS1-14bj, a hydrogen-poor superluminous supernova (SLSN) at redshift z = 0.5215 discovered in the last months of the Pan-STARRS1 Medium Deep Survey. PS1-14bj stands out because of its extremely slow evolution, with an observed rise of greater than or similar to 125 rest-frame days, and exponential decline out to similar to 250 days past peak at a measured rate of 0.01 mag day(-1), consistent with fully trapped Co-56 decay. This is the longest rise time measured in an SLSN to date, and the first SLSN to show a rise time consistent with pair-instability supernova (PISN) models. Compared to other slowly evolving SLSNe, it is spectroscopically similar to the prototype SN 2007bi at maximum light, although lower in luminosity (L-peak similar or equal to 4.6 x 10(43) erg s(-1) ) and with a flatter peak than previous events. PS1-14bj shows a number of peculiar properties, including a near-constant color temperature for > 200 days past peak, and strong emission lines from [O III] lambda 5007 and [O III] lambda 4363 with a velocity width of similar to 3400 km s(-1) in its late-time spectra. These both suggest there is a sustained source of heating over very long timescales, and are incompatible with a simple Ni-56-powered/PISN interpretation. A modified magnetar model including emission leakage at late times can reproduce the light curve, in which case the blue continuum and [O III] features are interpreted as material heated and ionized by the inner pulsar wind nebula becoming visible at late times. Alternatively, the late-time heating could be due to interaction with a shell of H-poor circumstellar material. | |
| 650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
| 653 | a supernovae: general | |
| 653 | a supernovae: individual (PS1-14bj | |
| 653 | a LSQ14an) | |
| 700 | 1 | a Chornock, R.4 aut |
| 700 | 1 | a Berger, E.4 aut |
| 700 | 1 | a Milisavljevic, D.4 aut |
| 700 | 1 | a Jones, D. O.4 aut |
| 700 | 1 | a Rest, A.4 aut |
| 700 | 1 | a Fong, W.4 aut |
| 700 | 1 | a Fransson, Claesu Stockholms universitet,Institutionen för astronomi,Oskar Klein-centrum för kosmopartikelfysik (OKC)4 aut0 (Swepub:su)frans |
| 700 | 1 | a Margutti, R.4 aut |
| 700 | 1 | a Drout, M. R.4 aut |
| 700 | 1 | a Blanchard, P. K.4 aut |
| 700 | 1 | a Challis, P.4 aut |
| 700 | 1 | a Cowperthwaite, P. S.4 aut |
| 700 | 1 | a Foley, R. J.4 aut |
| 700 | 1 | a Kirshner, R. P.4 aut |
| 700 | 1 | a Morrell, N.4 aut |
| 700 | 1 | a Riess, A. G.4 aut |
| 700 | 1 | a Roth, K. C.4 aut |
| 700 | 1 | a Scolnic, D.4 aut |
| 700 | 1 | a Smartt, S. J.4 aut |
| 700 | 1 | a Smith, K. W.4 aut |
| 700 | 1 | a Villar, V. A.4 aut |
| 700 | 1 | a Chambers, K. C.4 aut |
| 700 | 1 | a Draper, P. W.4 aut |
| 700 | 1 | a Huber, M. E.4 aut |
| 700 | 1 | a Kaiser, N.4 aut |
| 700 | 1 | a Kudritzki, R. -P.4 aut |
| 700 | 1 | a Magnier, E. A.4 aut |
| 700 | 1 | a Metcalfe, N.4 aut |
| 700 | 1 | a Waters, C.4 aut |
| 710 | 2 | a Stockholms universitetb Institutionen för astronomi4 org |
| 773 | 0 | t Astrophysical Journalg 831:2q 831:2x 0004-637Xx 1538-4357 |
| 856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-143863 |
| 856 | 4 8 | u https://doi.org/10.3847/0004-637X/831/2/144 |
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