Nebular-phase spectra of nearby Type Ia Supernovae

被引：0

作者：

Graham M.L. ^{[1
,2
]}

Kumar S. ^{[2
]}

Hosseinzadeh G. ^{[3
,4
]}

Hiramatsu D. ^{[3
,4
]}

Arcavi I. ^{[3
,4
]}

Howell D.A. ^{[3
,4
]}

Valenti S. ^{[5
]}

Sand D.J. ^{[6
]}

Parrent J.T. ^{[7
]}

McCully C. ^{[3
,4
]}

Filippenko A.V. ^{[2
,8
]}

机构：

[1] Department of Astronomy, University of Washington, Box 351580, Seattle, 98195, WA

[2] Department of Astronomy, University of California, Berkeley, 94720, CA

[3] Las Cumbres Observatory, Goleta, 93117, CA

[4] Physics Department, University of California, Santa Barbara, 93106, CA

[5] Department of Physics, University of California, Davis, 1 Shields Ave, Davis, 95616, CA

[6] Department of Astronomy and Steward Observatory, University of Arizona, 933 N Cherry Ave, Tucson, 85719, AZ

[7] Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, 02138, MA

[8] Senior Miller Fellow, Miller Institute for Basic Research in Science, University of California, Berkeley, 94720, CA

来源：

Graham, M.L. (mlg3k@uw.edu) | 1600年 / Oxford University Press卷 / 472期

基金：

美国国家航空航天局;

关键词：

ASASSN-14jg; SN2012hr; SN2013aa; SN2013cs; SN2013dy; SN2013gy; SN2015F; Supernovae: general; Supernovae: individual: SN2012fr;

D O I：

10.1093/MNRAS/STX2224

中图分类号：

学科分类号：

摘要：

We present late-time spectra of eight Type Ia supernovae (SNe Ia) obtained at > 200 d after peak brightness using the Gemini South and Keck telescopes. All of the SNe Ia in our sample were nearby, well separated from their host galaxy's light, and have early-time photometry and spectroscopy from the Las Cumbres Observatory. Parameters are derived from the light curves and spectra such as peak brightness, decline rate, photospheric velocity and the widths and velocities of the forbidden nebular emission lines. We discuss the physical interpretations of these parameters for the individual SNe Ia and the sample in general, including comparisons to well-observed SNe Ia from the literature. There are possible correlations between early-time and late-time spectral features that may indicate an asymmetric explosion, so we discuss our sample of SNe within the context ofmodels for an offset ignition and/or white dwarf collisions. A subset of our late-time spectra are uncontaminated by host emission, and we statistically evaluate our non-detections of Hα emission to limit the amount of hydrogen in these systems. Finally, we consider the late-time evolution of the iron emission lines, finding that not all of our SNe follow the established trend of a redward migration at > 200 d after maximum brightness. © 2018 The Author(s).

引用

页码：3437 / 3454

页数：17

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