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  • Bose, Subhash (author)

ASASSN-15nx : A Luminous Type II Supernova with a Perfect Linear Decline

  • Article/chapterEnglish2018

Publisher, publication year, extent ...

  • 2018-07-27
  • American Astronomical Society,2018
  • printrdacarrier

Numbers

  • LIBRIS-ID:oai:DiVA.org:su-159008
  • https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-159008URI
  • https://doi.org/10.3847/1538-4357/aacb35DOI

Supplementary language notes

  • Language:English
  • Summary in:English

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Classification

  • Subject category:ref swepub-contenttype
  • Subject category:art swepub-publicationtype

Notes

  • We report a luminous Type II supernova, ASASSN-15nx, with a peak luminosity of M-v = -20 mag that is between those of typical core-collapse supernovae and super-luminous supernovae. The post-peak optical light curves show a long, linear decline with a steep slope of 2.5 mag (100 day)(-1) (i.e., an exponential decline in flux) through the end of observations at phase approximate to 260 day. In contrast, the light curves of hydrogen-rich supernovae (SNe II-P/L) always show breaks in their light curves at phase similar to 100 day, before settling onto Co-56 radioactive decay tails with a decline rate of about 1 mag (100 day)(-1). The spectra of ASASSN-15nx do not exhibit the narrow emission-line features characteristic of Type IIn SNe, which can have a wide variety of light-curve shapes usually attributed to strong interactions with a dense circumstellar medium (CSM). ASASSN-15nx has a number of spectroscopic peculiarities, including a relatively weak and triangular-shaped H alpha emission profile with no absorption component. The physical origin of these peculiarities is unclear, but the long and linear post-peak light curve without a break suggests a single dominant powering mechanism. Decay of a large amount of Ni-56 (M-Ni = 1.6 +/- 0.2 M-circle dot) can power the light curve of ASASSN-15nx, and the steep light-curve slope requires substantial gamma-ray escape from the ejecta, which is possible given a low-mass hydrogen envelope for the progenitor. Another possibility is strong CSM interactions powering the light curve, but the CSM needs to be sculpted to produce the unique light-curve shape and avoid producing SN IIn-like narrow emission lines.

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Added entries (persons, corporate bodies, meetings, titles ...)

  • Dong, Subo (author)
  • Kochanek, C. S. (author)
  • Pastorello, Andrea (author)
  • Katz, Boaz (author)
  • Bersier, David (author)
  • Andrews, Jennifer E. (author)
  • Prieto, J. L. (author)
  • Stanek, K. Z. (author)
  • Shappee, B. J. (author)
  • Smith, Nathan (author)
  • Kollmeier, Juna (author)
  • Benetti, Stefano (author)
  • Cappellaro, E. (author)
  • Chen, Ping (author)
  • Elias-Rosa, N. (author)
  • Milne, Peter (author)
  • Morales-Garoffolo, Antonia (author)
  • Tartaglia, LeonardoStockholms universitet,Institutionen för astronomi,Oskar Klein-centrum för kosmopartikelfysik (OKC)(Swepub:su)leta1160 (author)
  • Tomasella, L. (author)
  • Bilinski, Christopher (author)
  • Brimacombe, Joseph (author)
  • Frank, Stephan (author)
  • Holoien, T. W. -S. (author)
  • Kilpatrick, Charles D. (author)
  • Kiyota, Seiichiro (author)
  • Madore, Barry F. (author)
  • Rich, Jeffrey A. (author)
  • Stockholms universitetInstitutionen för astronomi (creator_code:org_t)

Related titles

  • In:Astrophysical Journal: American Astronomical Society862:20004-637X1538-4357

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