Luminous Type II supernovae for their low expansion velocities

被引：16

作者：

Rodriguez, O. ^{[1
,2
,3
]}

Pignata, G. ^{[1
,2
]}

Anderson, J. P. ^{[4
]}

Moriya, T. J. ^{[5
,6
]}

Clocchiatti, A. ^{[2
,7
]}

Forster, F. ^{[2
,8
]}

Prieto, J. L. ^{[2
,9
]}

Phillips, M. M. ^{[10
]}

Burns, C. R. ^{[11
]}

Contreras, C. ^{[10
]}

Folatelli, G. ^{[12
,13
,14
]}

Gutierrez, C. P. ^{[15
]}

Hamuy, M. ^{[2
,16
]}

Morrell, N., I ^{[10
]}

Stritzinger, M. D. ^{[17
]}

Suntzeff, N. B. ^{[18
]}

Benetti, S. ^{[19
]}

Cappellaro, E. ^{[19
]}

Elias-Rosa, N. ^{[19
]}

Pastorello, A. ^{[19
]}

Turatto, M. ^{[19
]}

Maza, J. ^{[16
]}

Antezana, R. ^{[16
]}

Cartier, R. ^{[20
]}

Gonzalez, L. ^{[16
]}

Haislip, J. B. ^{[21
]}

Kouprianov, V ^{[21
]}

Lopez, P. ^{[14
]}

Marchi-Lasch, S. ^{[16
]}

Reichart, D. ^{[21
]}

机构：

[1] Univ Andres Bello, Dept Ciencias Fis, Avda Republ 252, Santiago, Chile

[2] Millennium Inst Astrophys MAS, Nuncio Monsenor Sotero Sanz 100, Santiago, Chile

[3] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel

[4] European Southern Observ, Alonso Cordova 3107,Casilla 19, Santiago, Chile

[5] Natl Inst Nat Sci, Natl Astron Observ Japan, Div Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[6] Monash Univ, Fac Sci, Sch Phys & Astron, Clayton, Vic 3800, Australia

[7] Pontificia Univ Catolica Chile, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile

[8] Univ Chile, Ctr Math Modeling, Beaucheff 851,7th Floor, Santiago, Chile

[9] Univ Diego Portales, Nucleo Astron, Fac Ingn & Ciencias, Av Ejercito 441, Santiago, Chile

[10] Las Campanas Observ, Carnegie Observ, Casilla 60, La Serena, Chile

[11] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA

[12] Consejo Nacl Invest Cient & Tecn, Inst Astrofis La Plata IALP, Paseo Bosque S-N,B1900FWA, La Plata, Argentina

[13] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, Paseo Bosque,B1900FWA, La Plata, Argentina

[14] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan

[15] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England

[16] Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile

[17] Aarhus Univ, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark

[18] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA

[19] INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[20] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile

[21] Univ N Carolina, Dept Phys & Astron, Campus Box 325, Chapel Hill, NC 27599 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2020年 / 494卷 / 04期

基金：

日本学术振兴会;

关键词：

circumstellar matter; supernovae: general; supernovae: individual: SN1983K; supernovae: individual: SN 2008bm; supernovae: individual: SN 2009aj; supernovae: individual: SN 2009au; supernovae: individual: LSQ13fn; LIGHT CURVES; SN; 2005CS; PLATEAU SUPERNOVAE; SHOCK BREAKOUT; P SUPERNOVA; NOVA; 1979C; PHOTOMETRY; EVOLUTION; DISTANCE; EMISSION;

D O I：

10.1093/mnras/staa1133

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页码：5882 / 5901

页数：20

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