التفاصيل البيبلوغرافية
| العنوان: |
PS1-14bj: A HYDROGEN-POOR SUPERLUMINOUS SUPERNOVA WITH A LONG RISE AND SLOW DECAY. |
| المؤلفون: |
R. Lunnan, R. Chornock, E. Berger, D. Milisavljevic, D. O. Jones, A. Rest, W. Fong, C. Fransson, R. Margutti, M. R. Drout, P. K. Blanchard, P. Challis, P. S. Cowperthwaite, R. J. Foley, R. P. Kirshner, N. Morrell, A. G. Riess, K. C. Roth, D. Scolnic, S. J. Smartt |
| المصدر: |
Astrophysical Journal; 11/10/2016, Vol. 831 Issue 2, p1-1, 1p |
| مصطلحات موضوعية: |
HYDROGEN, SUPERNOVAE, PHOTOMETRY, LUMINOSITY, CIRCUMSTELLAR matter |
| مستخلص: |
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 rest-frame days, and exponential decline out to ∼250 days past peak at a measured rate of , consistent with fully trapped 56Co 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 () and with a flatter peak than previous events. PS1-14bj shows a number of peculiar properties, including a near-constant color temperature for days past peak, and strong emission lines from [O iii] λ5007 and [O iii] λ4363 with a velocity width of ∼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 56Ni-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. [ABSTRACT FROM AUTHOR] |
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