Nebular spectra of 111 Type Ia supernovae disfavour single-degenerate progenitors

Tucker, M. A.; Shappee, B. J.; Vallely, P. J.; Stanek, K. Z.; Prieto, J. L.; Botyanszki, J.; Kochanek, C. S.; Anderson, J. P.; Brown, J.; Galbany, L.; Holoien, T. W-S; Hsiao, E. Y.; Kumar, S.; Kuncarayakti, H.; Morrell, N.; Phillips, M. M.; Stritzinger, M. D.; Thompson, Todd A.

doi:10.1093/mnras/stz3390

Title: Nebular spectra of 111 Type Ia supernovae disfavour single-degenerate progenitors

Journal Article · 04 December 2019 · Monthly Notices of the Royal Astronomical Society

DOI: https://doi.org/10.1093/mnras/stz3390 · OSTI ID:1601006

^[1]; Shappee, B. J. ^[1];

^[2]; Stanek, K. Z. ^[3]; Prieto, J. L. ^[4]; Botyanszki, J. ^[5]; Kochanek, C. S. ^[3]; Anderson, J. P. ^[6]; Brown, J. ^[2]; Galbany, L. ^[7];

^[8]; Hsiao, E. Y. ^[9]; Kumar, S. ^[9]; Kuncarayakti, H. ^[10]; Morrell, N. ^[11]; Phillips, M. M. ^[11]; Stritzinger, M. D. ^[12]; Thompson, Todd A. ^[3]

Univ. of Hawaii at Manoa, Honolulu, HI (United States)
The Ohio State Univ., Columbus, OH (United States)
The Ohio State Univ., Columbus, OH (United States). Center for Cosmology and AstroParticle Physics (CCAPP)
Núcleo de Astronomía de la Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Av. Ejército 441, Santiago, Chile; Millennium Institute of Astrophysics, Santiago, Chile
Univ. of California, Berkeley, CA (United States)
European Southern Observatory (Chile)
Univ. of Pittsburgh, PA (United States)
Carnegie Observatories, Pasadena, CA (United States)
Florida State Univ., Tallahassee, FL (United States)
University of Turku (Finland). Finnish Centre for Astronomy with ESO (FINCA). Tuorla Observatory
Carnegie Observatories, La Serena (Chile). Las Campanas Observatory
Aarhus Univ. (Denmark)

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 3σ upper limit on the fraction of SNe Ia that are produced through the classical H-rich non-degenerate companion scenario of $$\lt 5.5 {{\ \rm per\ cent}}$$. Additionally, we set a tentative 3σ upper limit otan He star progenitor scenarios of $$\lt 6.4 {{\ \rm per\ cent}}$$, 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 Δm15(B).

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Research Organization:: Krell Institute, Ames, IA (United States)

Sponsoring Organization:: USDOE Office of Science (SC)

Grant/Contract Number:: SC0019323

OSTI ID:: 1601006

Alternate ID(s):: OSTI ID: 1803687

Journal Information:: Monthly Notices of the Royal Astronomical Society, Vol. 493, Issue 1; ISSN 0035-8711

Publisher:: Royal Astronomical SocietyCopyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 38 works

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