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|Title:||Gaia16apd - a link between fast and slowly declining type I superluminous supernovae||Authors:||Kangas, T.
Carrasco Martínez, J. M.
ELIAS DE LA ROSA, NANCY DEL CARMEN
Hardy, L. K.
Hsiao, E. Y.
Nielsen, M. B.
Reynolds, T. M.
Stritzinger, M. D.
|Issue Date:||2017||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||469||Issue:||1||First Page:||1246||Abstract:||We present ultraviolet (UV), optical and infrared photometry and optical spectroscopy of the type Ic superluminous supernova (SLSN) Gaia16apd (=SN 2016eay), covering its evolution from 26 d before the g-band peak to 234.1 d after the peak. Gaia16apd was followed as a part of the NOT Unbiased Transient Survey (NUTS). It is one of the closest SLSNe known (z = 0.102 ± 0.001), with detailed optical and UV observations covering the peak. Gaia16apd is a spectroscopically typical type Ic SLSN, exhibiting the characteristic blue early spectra with O II absorption, and reaches a peak M<SUB>g</SUB> = -21.8 ± 0.1 mag. However, photometrically it exhibits an evolution intermediate between the fast and slowly declining type Ic SLSNe, with an early evolution closer to the fast-declining events. Together with LSQ12dlf, another SLSN with similar properties, it demonstrates a possible continuum between fast and slowly declining events. It is unusually UV-bright even for an SLSN, reaching a non-K-corrected M<SUB>uvm2</SUB> ≃ -23.3 mag, the only other type Ic SLSN with similar UV brightness being SN 2010gx. Assuming that Gaia16apd was powered by magnetar spin-down, we derive a period of P = 1.9 ± 0.2 ms and a magnetic field of B = 1.9 ± 0.2 × 10<SUP>14</SUP> G for the magnetar. The estimated ejecta mass is between 8 and 16 M<SUB>☉</SUB>, and the kinetic energy between 1.3 and 2.5 × 10<SUP>52</SUP> erg, depending on opacity and assuming that the entire ejecta is swept up into a thin shell. Despite the early photometric differences, the spectra at late times are similar to slowly declining type Ic SLSNe, implying that the two subclasses originate from similar progenitors.||URI:||http://hdl.handle.net/20.500.12386/28276||URL:||https://academic.oup.com/mnras/article/469/1/1246/3101034||ISSN:||0035-8711||DOI:||10.1093/mnras/stx833||Bibcode ADS:||2017MNRAS.469.1246K||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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checked on Jun 23, 2021
checked on Jun 23, 2021
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