The Prevalence and Influence of Circumstellar Material around Hydrogen-rich Supernova Progenitors

被引：60

作者：

Bruch, Rachel J. ^{[1
]}

Gal-Yam, Avishay ^{[1
]}

Yaron, Ofer ^{[1
]}

Chen, Ping ^{[1
]}

Strotjohann, Nora L. ^{[1
]}

Irani, Ido ^{[1
]}

Zimmerman, Erez ^{[1
]}

Schulze, Steve ^{[1
,2
]}

Yang, Yi ^{[1
]}

Kim, Young-Lo ^{[3
,4
]}

Bulla, Mattia ^{[2
]}

Sollerman, Jesper ^{[2
]}

Rigault, Mickael ^{[3
]}

Ofek, Eran ^{[1
]}

Soumagnac, Maayane ^{[1
,5
]}

Masci, Frank J. ^{[6
]}

Fremling, Christoffer ^{[7
]}

Perley, Daniel ^{[8
]}

Nordin, Jakob ^{[9
]}

Cenko, S. Bradley ^{[10
,11
]}

Ho, Anna Y. Q. ^{[12
]}

Adams, S. ^{[7
]}

Adreoni, Igor ^{[7
]}

Bellm, Eric C. ^{[13
]}

Blagorodnova, Nadia ^{[14
]}

Burdge, Kevin ^{[7
]}

De, Kishalay ^{[7
]}

Dekany, Richard G. ^{[15
]}

Dhawan, Suhail ^{[2
]}

Drake, Andrew J.

Duev, Dmitry A.

Graham, Matthew ^{[7
]}

Graham, Melissa L. ^{[17
]}

Jencson, Jacob ^{[7
]}

Karamehmetoglu, Emir ^{[2
,18
]}

Kasliwal, Mansi M. ^{[7
]}

Kulkarni, Shrinivas ^{[7
]}

Miller, A. A. ^{[19
,20
,21
]}

Neill, James D. ^{[7
]}

Prince, Thomas A. ^{[16
]}

Riddle, Reed ^{[15
]}

Rusholme, Benjamin ^{[6
]}

Sharma, Y. ^{[7
]}

Smith, Roger ^{[15
]}

Sravan, Niharika ^{[16
]}

Taggart, Kirsty ^{[8
]}

Walters, Richard ^{[15
]}

Yan, Lin ^{[7
]}

机构：

[1] Weizmann Inst Sci, Dept Particle Phys & Astrophys, 234 Herzl St, IL-76100 Rehovot, Israel

[2] Stockholm Univ, Oskar Klein Ctr, Dept Astron, AlbaNova, SE-10691 Stockholm, Sweden

[3] Univ Claude Bernard Lyon 1, Univ Lyon, CNRS IN2P3, IP2I Lyon, F-69622 Villeurbanne, France

[4] Univ Lancaster, Dept Phys, Lancaster LA1 4YB, Lancs, England

[5] Bar Ilan Univ, Phys Dept, Ramat Gan, Israel

[6] CALTECH, IPAC, 1200 E Calif Blvd, Pasadena, CA 91125 USA

[7] CALTECH, Cahill Ctr Astrophys, MC 249-17,1200 Calif Blvd, Pasadena, CA 91125 USA

[8] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, England

[9] Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany

[10] NASA Goddard Space Flight Ctr, Astrophys Sci Div, MC 661, Greenbelt, MD 20771 USA

[11] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA

[12] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA

[13] Univ Washington, DIRAC Inst, Dept Astron, 3910 15th Ave NE, Seattle, WA 98195 USA

[14] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, Nijmegen, Netherlands

[15] CALTECH, Caltech Opt Observ, MC 249-17,1200 E Calif Blvd, Pasadena, CA 91125 USA

[16] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA

[17] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA

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

[19] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys, 1800 Sherman Ave, Evanston, IL 60201 USA

[20] Northwestern Univ, Dept Phys & Astron, 1800 Sherman Ave, Evanston, IL 60201 USA

[21] Adler Planetarium, Chicago, IL 60605 USA

来源：

ASTROPHYSICAL JOURNAL | 2023年 / 952卷 / 02期

基金：

美国国家科学基金会; 欧洲研究理事会; 美国国家航空航天局;

关键词：

MASS-LOSS; LIGHT CURVES; RESOLUTION SPECTROGRAPH; EMISSION; ASTROPY; PERFORMANCE; PACKAGE; PROJECT;

D O I：

10.3847/1538-4357/acd8be

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Narrow transient emission lines (flash-ionization features) in early supernova (SN) spectra trace the presence of circumstellar material (CSM) around the massive progenitor stars of core-collapse SNe. The lines disappear within days after the SN explosion, suggesting that this material is spatially confined, and originates from enhanced mass loss shortly (months to a few years) prior to the explosion. We performed a systematic survey of H-rich (Type II) SNe discovered within less than 2 days from the explosion during the first phase of the Zwicky Transient Facility survey (2018-2020), finding 30 events for which a first spectrum was obtained within <2 days from the explosion. The measured fraction of events showing flash-ionization features (>36% at the 95% confidence level) confirms that elevated mass loss in massive stars prior to SN explosion is common. We find that SNe II showing flash-ionization features are not significantly brighter, nor bluer, nor more slowly rising than those without. This implies that CSM interaction does not contribute significantly to their early continuum emission, and that the CSM is likely optically thin. We measured the persistence duration of flash-ionization emission and find that most SNe show flash features for & AP;5 days. Rarer events, with persistence timescales >10 days, are brighter and rise longer, suggesting these may be intermediate between regular SNe II and strongly interacting SNe IIn.

引用

页数：23

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