SN 2013ab: a normal Type IIP supernova in NGC 5669
Date Issued
2015
Author(s)
Bose, Subhash
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Valenti, Stefano
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Misra, Kuntal
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•
•
Sand, David
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Kumar, Brijesh
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•
Sutaria, Firoza
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Maccarone, Thomas J.
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Kumar, Brajesh
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Graham, M. L.
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Howell, D. Andrew
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•
Chandola, H. C.
•
Pandey, Shashi B.
Description
This work makes use of observations from the LCOGT network. We are thankful to the observing and technical staffs of LCOGT, ARIES, HCT and Asiago telescopes for their kind cooperation in observation of SN 2013ab. We gratefully acknowledge the services of the NASA ADS and NED data bases and also the online supernova spectrum archive (SUSPECT) which are used to access data and references in this paper. We acknowledge the TriGrid VL project and the INAF-Astronomical Observatory of Padua for the use of computer facilities. MLP and AP acknowledge the financial support from CSFNSM and from the PRIN-INAF 2011 ‘Transient Universe: from ESO Large to PESSTO’ (P.I. S. Benetti). We are also thankful to the anonymous referee, whose comments and suggestions has helped in significant improvement of the manuscript.
Abstract
We present densely sampled ultraviolet/optical photometric and low-resolution optical spectroscopic observations of the Type IIP supernova 2013ab in the nearby (̃24 Mpc) galaxy NGC 5669, from 2 to 190 d after explosion. Continuous photometric observations, with the cadence of typically a day to one week, were acquired with the 1-2 m class telescopes in the Las Cumbres Observatory Global Telescope network, ARIES telescopes in India and various other telescopes around the globe. The light curve and spectra suggest that the supernova (SN) is a normal Type IIP event with a plateau duration of ̃80 d with mid-plateau absolute visual magnitude of -16.7, although with a steeper decline during the plateau (0.92 mag 100 d-1 in V band) relative to other archetypal SNe of similar brightness. The velocity profile of SN 2013ab shows striking resemblance with those of SNe 1999em and 2012aw. Following the Rabinak & Waxman prescription, the initial temperature evolution of the SN emission allows us to estimate the progenitor radius to be ̃800 R☉, indicating that the SN originated from a red supergiant star. The distance to the SN host galaxy is estimated to be 24.3 Mpc from expanding photosphere method. From our observations, we estimate that 0.064 M☉ of 56Ni was synthesized in the explosion. General relativistic, radiation hydrodynamical modelling of the SN infers an explosion energy of 0.35 × 1051 erg, a progenitor mass (at the time of explosion) of ̃9 M☉ and an initial radius of ̃600 R☉.
Volume
450
Issue
3
Start page
2373
Issn Identifier
0035-8711
Ads BibCode
2015MNRAS.450.2373B
Rights
open.access
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