期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 493, 期 1, 页码 1044-1062出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz3390
关键词
supernovae; general; galaxies; distances and redshifts
资金
- United States Department of Energy through the Computational Sciences Graduate Fellowship (DOE CSGF) [DE-SC0019323]
- NSF [AST-1108693]
- Independent Research Fund Denmark
- FONDECYT [1191038]
- Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC120009]
- National Science Foundation Graduate Research Fellowship Program [DGE-1343012]
- Radcliffe Institute for Advanced Study at Harvard University
- European Organisation for Astronomical Research in the Southern hemisphere under ESO [0100.D-0191, 0101.D-0173, 0102.D-0287(A), 096.D-0296(A)]
- National Science Foundation [AST-1238877]
- National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project [NCC5-626]
- Max-Planck Society
- Max Planck Institute for Extraterrestrial Physics
- Queen's University Belfast
- Harvard Smithsonian Center forAstrophysics
- National Central University of Taiwan
- Space Telescope Science Institute
- National Aeronautics and Space Administration [NNX08AR22G]
- NASA Science Mission Directorate
- University of Maryland, Eotvos Lorand University (ELTE)
- Los Alamos National Laboratory
- Gordon and Betty Moore Foundation
We place statistical constraints on Type Ia supernova (SN Ia) progenitors using 227 nebular-phase spectra of 111 SNe Ia. We find no evidence of stripped companion emission in any of the nebular-phase spectra. Upper limits are placed on the amount of mass that could go undetected in each spectrum using recent hydrodynamic simulations. With these null detections, we place an observational 3 sigma upper limit on the fraction of SNe Ia that are produced through the classical H-rich non-degenerate companion scenario of < 5.5 per cent. Additionally, we set a tentative 3 sigma upper limit otan He star progenitor scenarios of < 6.4 per cent, although further theoretical modelling is required. These limits refer to our most representative sample including normal, 91bg-like, 91T-like, and 'super-Chandrasekhar' SNe Ia but excluding SNe Iax and SNe Ia-CSM. As part of our analysis, we also derive a Nebular Phase Phillips Relation, which approximates the brightness of an SN Ia from 150 to 500 d after maximum using the peak magnitude and decline rate parameter Delta m(15)(B).
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