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|Title:||SN 2012ec: mass of the progenitor from PESSTO follow-up of the photospheric phase||Authors:||Barbarino, C.
BOTTICELLA, MARIA TERESA
DELLA VALLE, Massimo
Maund, J. R.
Pumo, M. L.
ELIAS DE LA ROSA, NANCY DEL CARMEN
LaCluyze, A. P.
Reichart, D. E.
Smartt, S. J.
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||448||Issue:||3||First Page:||2312||Abstract:||We present the results of a photometric and spectroscopic monitoring campaign of SN 2012ec, which exploded in the spiral galaxy NGC 1084, during the photospheric phase. The photometric light curve exhibits a plateau with luminosity L = 0.9 × 10<SUP>42</SUP> erg s<SUP>-1</SUP> and duration ̃90 d, which is somewhat shorter than standard Type II-P supernovae (SNe). We estimate the nickel mass M(<SUP>56</SUP>Ni) = 0.040 ± 0.015 M<SUB>☉</SUB> from the luminosity at the beginning of the radioactive tail of the light curve. The explosion parameters of SN 2012ec were estimated from the comparison of the bolometric light curve and the observed temperature and velocity evolution of the ejecta with predictions from hydrodynamical models. We derived an envelope mass of 12.6 M<SUB>☉</SUB>, an initial progenitor radius of 1.6 × 10<SUP>13</SUP> cm and an explosion energy of 1.2 foe. These estimates agree with an independent study of the progenitor star identified in pre-explosion images, for which an initial mass of M = 14-22 M<SUB>☉</SUB> was determined. We have applied the same analysis to two other Type II-P SNe (SNe 2012aw and 2012A), and carried out a comparison with the properties of SN 2012ec derived in this paper. We find a reasonable agreement between the masses of the progenitors obtained from pre-explosion images and masses derived from hydrodynamical models. We estimate the distance to SN 2012ec with the standardized candle method (SCM) and compare it with other estimates based on other primary and secondary indicators. SNe 2012A, 2012aw and 2012ec all follow the standard relations for the SCM for the use of Type II-P SNe as distance indicators.||Acknowledgments:||We warmly thank our referee, Dovi Poznanski, for his helpful comments, which significantly improved the content and the readability of our manuscript. We thank E. Cappellaro for the useful discussions. CB thanks the IRAP PhD programme for the financial support. The research of JRM is supported through a Royal Society Research Fellowship. AG-Y is supported by an EU/FP7-ERC grant no , ‘The Quantum Universe’ I-Core programme by the Israeli Committee for planning and budgeting and the ISF, GIF, Minerva, ISF and Weizmann-UK grants, and the Kimmel award. GP acknowledges partial support by proyecto interno UNAB DI-303-13/R. GP and MH acknowledge support provided by the Millennium Institute of Astrophysics (MAS) through grant IC120009 of the ‘Programa Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo de Chile’. MDV, MLP, SB, AP, LT and MT are partially supported by the PRIN-INAF 2011 with the project ‘Transient Universe: from ESO Large to PESSTO’. This work was partly supported by the European Union FP7 programme through ERC grant number 320360. This work is based (in part) on observations collected at the European Organization for Astronomical Research in the Southern hemisphere, Chile as part of PESSTO, ESO programme 188.D-3003, 191.D-0935. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement no.  (PI: S. J. Smartt) and STFC grants ST/I001123/1 and ST/L000709/1. The early SN 2012ec data have been collected via the ESO-NTT Large Programme Supernova Variety and Nuclesosynthesis Yelds (184.D-1140), a European SN collaboration led by Stefano Benetti ( http://sngroup.oapd.inaf.it/esolarge.html ). This paper is partially based on observations collected at Copernico telescope (Asiago, Italy) of the INAF – Osservatorio Astronomico di Padova; at the Galileo 1.22m telescope operated by Department of Physics and Astronomy of the University of Padova at Asiago; at the 2.56m NOT operated by The Nordic Optical Telescope Scientific Association (NOTSA); at the 4.3m WHT operated by the Isaac Newton Group of Telescopes; on observations obtained through the CNTAC proposal CN2012B-73 and on observations made with the LT (programme OL12B) operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council.||URI:||http://hdl.handle.net/20.500.12386/23891||URL:||https://academic.oup.com/mnras/article/448/3/2312/1093173||ISSN:||0035-8711||DOI:||10.1093/mnras/stv106||Bibcode ADS:||2015MNRAS.448.2312B||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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