Volume 634, February 2020
|Number of page(s)||17|
|Published online||30 January 2020|
The Carnegie Supernova Project II
Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, Denmark
2 Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks, Rm 100, Norman, OK 73019-2061, USA
3 Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile
4 The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova 10691, Stockholm, Sweden
5 George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, Department of Physics and Astronomy, College Station, TX 77843, USA
6 Konkoly Observatory, CSFK, Konkoly-Thege M. ut 15-17, Budapest, Hungary
7 Department of Optics and Quantum Electronics, University of Szeged, Dom ter 9, Szeged, Hungary
8 Department of Astronomy, University of Texas, 1 University Station C1400, Austin, TX 78712, USA
9 Department of Physics, Florida State University, Tallahassee, FL 32306, USA
10 Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA
11 Instituto de Astrofısica de La Plata (IALP), CONICET, Paseo del bosque s/n, 1900 La Plata, Argentina
12 Facultad de Ciencias Astronómicas y Geofísicas (FCAG), Universidad Nacional de La Plata (UNLP), Paseo del bosque s/n, 1900 La Plata, Argentina
13 Kavli Institute for the Physics and Mathematics of the Universe, Todai Institutes for Advanced Study, University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan
14 Departamento de Física Teórica y del Cosmos, Universidad de Granada, 18071 Granada, Spain
Accepted: 12 November 2019
Supernova LSQ13abf was discovered soon after explosion by the La Silla-QUEST Survey and then followed by the Carnegie Supernova Project II at its optical and near-IR wavelengths. Our analysis indicates that LSQ13abf was discovered within two days of explosion and its first ≈10 days of evolution reveal a B-band light curve with an abrupt drop in luminosity. Contemporaneously, the V-band light curve exhibits a rise towards a first peak and the r- and i-band light curves show no early peak. The early light-curve evolution of LSQ13abf is reminiscent of the post-explosion cooling phase observed in the Type Ib SN 2008D, and the similarity between the two objects extends over weeks. Spectroscopically, LSQ13abf also resembles SN 2008D, with P Cygni He I features that strengthen over several weeks. Spectral energy distributions are constructed from the broad-bandphotometry, a UVOIR light curve is constructed by fitting black-body (BB) functions, and the underlying BB-temperature and BB-radius profiles are estimated. Explosion parameters are estimated by simultaneously fitting an Arnett model to the UVOIR light curve and the velocity evolution derived from spectral features, and an in addition to a post-shock breakout cooling model to the first two epochs of the bolometric evolution. This combined model suggests an explosion energy of 1.27 ± 0.23 × 1051 ergs, in addition to a relatively high ejecta mass of 5.94 ± 1.10 M⊙, a 56Ni mass of 0.16 ± 0.02 M⊙, and a progenitor-star radius of 28.0 ± 7.5 R⊙. The ejecta mass suggests the origins of LSQ13abf lie with a > 25 M⊙ zero-age-main-sequence mass progenitor and its estimated radius is three times larger compared to the result obtained from the same analysis applied to observations of SN 2008D, and nine times larger compared to SN 1999ex. Alternatively, a comparison of hydrodynamical simulations of ≳20−25 M⊙ zero-age-main-sequence progenitors that evolve to pre-supernova envelope masses of ≲10 M⊙ and extended (∼100 R⊙) envelopes also broadly match the observations of LSQ13abf.
Key words: supernovae: individual: LSQ13abf / supernovae: individual: SN 1999ex / supernovae: individual: SN 2008D / supernovae: individual: iPTF13bvn / supernovae: general
This paper includes data gathered with the Nordic Optical Telescope at the Observatorio del Roque de los Muchachos, La Palma, Spain, and the Magellan 6.5 m Telescopes located at Las Campanas Observatory, Chile.
Photometry and spectra presented in this paper are available on WISeREP.
© ESO 2020
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