Luminous Type II supernovae for their low expansion velocities
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2020Metadata
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Rodríguez, Ó.
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Luminous Type II supernovae for their low expansion velocities
Author
- Rodríguez, Ó.;
- Pignata, G.;
- Anderson, J. P.;
- Moriya, T. J.;
- Clocchiatti, A.;
- Förster Burón, Francisco;
- Prieto, J.L.;
- Phillips, M. M.;
- Burns, C. R.;
- Contreras, C.;
- Folatelli, G.;
- Gutiérrez, C. P.;
- Hamuy Wackenhut, Mario;
- Morrell, N. I.;
- Stritzinger, M. D.;
- Suntzeff, N. B.;
- Benetti, S.;
- Cappellaro, E.;
- Elias Rosa, N.;
- Pastorello, A.;
- Turatto, M.;
- Maza Sancho, José María;
- Antezana, Roberto;
- Cartier, R.;
- González Muñoz, Luis;
- Haislip, J. B.;
- Kouprianov, V.;
- López, P.;
- Marchi Lasch, Sebastián;
- Reichart, D.;
Abstract
We present optical and near-infrared data of three Type II supernovae (SNe II), SN 2008bm, SN 2009aj, and SN 2009au. These SNe display the following common characteristics: signs of early interaction of the ejecta with circumstellar material (CSM), blue B - V colours, weakness of metal lines, low expansion velocities, and V-band absolute magnitudes 2-3 mag brighter than those expected for normal SNe II based on their expansion velocities. Two more SNe reported in the literature (SN 1983K and LSQ13fn) share properties similar to our sample. Analysing this set of five SNe II, which are luminous for their low expansion velocities (LLEV), we find that their properties can be reproduced assuming ejecta-CSM interaction that lasts between 4 and 11 weeks post-explosion. The contribution of this interaction to the radiation field seems to be the dominant component determining the observed weakness of metal lines in the spectra rather than the progenitor metallicity. Based on hydrodynamic simulations, we find that the interaction of the ejecta with a CSM of similar to 3.6 M-circle dot can reproduce the light curves and expansion velocities of SN 2009aj. Using data collected by the Chilean Automatic Supernova Search, we estimate an upper limit for the LLEV SNe II fraction to be 2-4 per cent of all normal SNe II. With the current data set, it is not clear whether the LLEV events are a separated class of SNe II with a different progenitor system, or whether they are the extreme of a continuum mediated by CSM interaction with the rest of the normal SN II population.
Patrocinador
CSP-I by NSF
AST-0306969
AST-0607438
AST-1008343
Ministry of Economy, Development, and Tourism's Millennium Science Initiative
IC120009
CONICYT PAI/INDUSTRIA
79090016
Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT)
Japan Society for the Promotion of Science
JP17H02864
JP18K13585
Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT)
Japan Society for the Promotion of Science
Comisión Nacional de Investigación Cientifica y Tecnológica (CONICYT)
CONICYT FONDECYT
1191038
EU/FP7-ERC grant
615929
Independent Research Fund Denmark
8021-00170B
VILLUM FONDEN
13261
National Science Foundation (NSF)
AST-1613455
NSF through Texas A&M University Mitchell/Heep/Munnerlyn Chair in Observational Astronomy
George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy
European Southern Observatory under ESO programmes
082.A0526
083.D-0970
Gemini Observatory, Cerro Pachon, Chile (Gemini Program)
GS-2009A-Q-43
Indexation
Artículo de publicación ISI Artículo de publicación SCOPUS
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MNRAS 494, 5882–5901 (2020)
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