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Final Moments. II. Observational Properties and Physical Modeling of Circumstellar-material-interacting Type II Supernovae
Jacobson-Galán, W. V.1; Dessart, L.2; Davis, K. W.3; Kilpatrick, C. D.4,5; Margutti, R.1,6; Foley, R. J.3; Chornock, R.1; Terreran, G.7; Hiramatsu, D.8,9; Newsome, M.7,10; Gonzalez, E. Padilla7,10; Pellegrino, C.11; Howell, D. A.7,10; Filippenko, A. V.1; Anderson, J. P.12,13; Angus, C. R.14,15; Auchettl, K.3,16; Bostroem, K. A.17; Brink, T. G.1; Cartier, R.18; Coulter, D. A.19; Boer, T. de20; Drout, M. R.21; Earl, N.22; Ertini, K.23,24; Farah, J. R.7,10; Farias, D.14; Gall, C.14; Gao, H.20; Gerlach, M. A.25; Guo, F.26; Haynie, A.27,28; Hosseinzadeh, G.17; Ibik, A. L.21; Jha, S. W.29; Jones, D. O.30; Langeroodi, D.14; LeBaron, N1; Magnier, E. A.20; Piro, A. L.27; Raimundo, S. I.14,31; Rest, A.19,32; Rest, S.32; Rich, R. Michael33; Rojas-Bravo, C.3; Sears, H.4,5; Taggart, K.3; Villar, V. A.8; Wainscoat, R. J.20; Wang, X-F.26; Wasserman, A. R.34,35; Yan, S.26; Yang, Y.1; Zhang JJ(张居甲)36,37; Zheng, W.1
发表期刊ASTROPHYSICAL JOURNAL
2024-08-01
卷号970期号:2
DOI10.3847/1538-4357/ad4a2a
产权排序第36完成单位
收录类别SCI
摘要We present ultraviolet/optical/near-infrared observations and modeling of Type II supernovae (SNe II) whose early time (delta(t) < 2 days) spectra show transient, narrow emission lines from shock ionization of confined (r < 10(15) cm) circumstellar material (CSM). The observed electron-scattering broadened line profiles (i.e., IIn-like) of H i, He i/ii, C iv, and N iii/iv/v from the CSM persist on a characteristic timescale (t(IIn)) that marks a transition to a lower-density CSM and the emergence of Doppler-broadened features from the fast-moving SN ejecta. Our sample, the largest to date, consists of 39 SNe with early time IIn-like features in addition to 35 comparison SNe with no evidence of early time IIn-like features, all with ultraviolet observations. The total sample includes 50 unpublished objects with a total of 474 previously unpublished spectra and 50 multiband light curves, collected primarily through the Young Supernova Experiment and Global Supernova Project collaborations. For all sample objects, we find a significant correlation between peak ultraviolet brightness and both t(II)n and the rise time, as well as evidence for enhanced peak luminosities in SNe II with IIn-like features. We quantify mass-loss rates and CSM density for the sample through the matching of peak multiband absolute magnitudes, rise times, t(IIn), and optical SN spectra with a grid of radiation hydrodynamics and non-local thermodynamic equilibrium radiative-transfer simulations. For our grid of models, all with the same underlying explosion, there is a trend between the duration of the electron-scattering broadened line profiles and inferred mass-loss rate: t(IIn) approximate to 3.8[M/ (0.01 M-circle dot yr(-1))] days.
资助项目European Research Council under the European Union[101002652]; Heising-Simons Foundation[2018-0913]; Heising-Simons Foundation[2018-0911]; Heising-Simons Foundation[2021-3248]; NASA[NNG17PX03C]; NASA[GO-16075]; NASA[GO-16500]; NASA[80NSSC22K0946]; NASA[80NSSC20K0953]; NASA[NNX08AR22G]; NSF[AST-1720756]; NSF[AST-1815935]; NSF[PHY-1748958]; NSF[AST-2221789]; NSF[AST-2224255]; NSF[AST-2108676]; NSF[AST-1440341]; NSF[AST-1238877]; NSF[AST-1911225]; NSF[AST-1911151]; David & Lucille Packard Foundation; VILLUM FONDEN[16599]; VILLUM FONDEN[25501]; Center for AstroPhysical Surveys (CAPS) at NCSA; University of Illinois Urbana-Champaign; National Science Foundation (NSF)[DGE-1842165]; CIERA postdoctoral fellowship; USC-Carnegie Graduate Fellowship; ANID, Millennium Science Initiative[ANID]; ANID, Millennium Science Initiative[Millennium Science Initiative]; National Natural Science Foundation of China (NSFC)[12288102]; National Natural Science Foundation of China (NSFC)[12033003]; New Cornerstone Science Foundation; Munich Institute for Astro-, Particle and BioPhysics (MIAPbP); Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany's Excellence Strategy[EXC-2094 390783311]; LSSTC Catalyst Fellowship; John Templeton Foundation[62192]; NSERC[RGPIN-2019-06186]; Canada Research Chairs Program; Dunlap Institute at the University of Toronto; Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)[EXC-2094 - 390783311]; Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)[CE170100013]; Gordon & Betty Moore Foundation; David and Lucile Packard Foundation; Instituto de Astrofisica de Canarias[P62-507]; W.M. Keck Foundation; University of Maryland; Eotvos Lorand University (ELTE); Los Alamos National Laboratory; Gordon and Betty Moore Foundation; Rutgers University program[2022-1-MLT-004]; CAS; People's Government of Yunnan Province
项目资助者European Research Council under the European Union[101002652] ; Heising-Simons Foundation[2018-0913, 2018-0911, 2021-3248] ; NASA[NNG17PX03C, GO-16075, GO-16500, 80NSSC22K0946, 80NSSC20K0953, NNX08AR22G] ; NSF[AST-1720756, AST-1815935, PHY-1748958, AST-2221789, AST-2224255, AST-2108676, AST-1440341, AST-1238877, AST-1911225, AST-1911151] ; David & Lucille Packard Foundation ; VILLUM FONDEN[16599, 25501] ; Center for AstroPhysical Surveys (CAPS) at NCSA ; University of Illinois Urbana-Champaign ; National Science Foundation (NSF)[DGE-1842165] ; CIERA postdoctoral fellowship ; USC-Carnegie Graduate Fellowship ; ANID, Millennium Science Initiative[ANID, Millennium Science Initiative] ; National Natural Science Foundation of China (NSFC)[12288102, 12033003] ; New Cornerstone Science Foundation ; Munich Institute for Astro-, Particle and BioPhysics (MIAPbP) ; Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany's Excellence Strategy[EXC-2094 390783311] ; LSSTC Catalyst Fellowship ; John Templeton Foundation[62192] ; NSERC[RGPIN-2019-06186] ; Canada Research Chairs Program ; Dunlap Institute at the University of Toronto ; Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)[EXC-2094 - 390783311] ; Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)[CE170100013] ; Gordon & Betty Moore Foundation ; David and Lucile Packard Foundation ; Instituto de Astrofisica de Canarias[P62-507] ; W.M. Keck Foundation ; University of Maryland ; Eotvos Lorand University (ELTE) ; Los Alamos National Laboratory ; Gordon and Betty Moore Foundation ; Rutgers University program[2022-1-MLT-004] ; CAS ; People's Government of Yunnan Province
语种英语
学科领域天文学 ; 恒星与银河系
文章类型Article
出版者IOP Publishing Ltd
出版地TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-637X
URL查看原文
WOS记录号WOS:001281458400001
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]CORE-COLLAPSE SUPERNOVA ; X-RAY-EMISSION ; MASS-LOSS ; SHOCK BREAKOUT ; P SUPERNOVA ; PAN-STARRS ; SN 2020JFO ; PRECURSOR EMISSION ; RADIO-EMISSION ; IA SUPERNOVAE
引用统计
文献类型期刊论文
版本出版稿
条目标识符http://ir.ynao.ac.cn/handle/114a53/27510
专题南方基地
中国科学院天体结构与演化重点实验室
作者单位1.Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA; [email protected];
2.Institut d'Astrophysique de Paris, CNRS-Sorbonne Université, 98 bis boulevard Arago, F-75014 Paris, France;
3.Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA;
4.Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, IL 60202, USA;
5.Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USA;
6.Department of Physics, University of California, Berkeley, CA 94720-7300, USA;
7.Las Cumbres Observatory, 6740 Cortona Drive Suite 102, Goleta, CA 93117, USA;
8.Center for Astrophysics ∣ Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138-1516, USA;
9.The NSF AI Institute for Artificial Intelligence and Fundamental Interactions, USA;
10.Department of Physics, University of California, Santa Barbara, Santa Barbara, CA, 93111, USA;
11.Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA;
12.European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile;
13.Millennium Institute of Astrophysics MAS, Nuncio Monsenor Sotero Sanz 100, Off. 104, Providencia, Santiago, Chile;
14.DARK, Niels Bohr Institute, University of Copenhagen, Jagtvej 128, 2200 Copenhagen, Denmark;
15.Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, UK;
16.School of Physics, The University of Melbourne, VIC 3010, Australia;
17.Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA;
18.Gemini Observatory, NSF's National Optical-Infrared Astronomy Research Laboratory, Casilla 603, La Serena, Chile;
19.Space Telescope Science Institute, Baltimore, MD 21218, USA;
20.Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA;
21.David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario, M5S 3H4, Canada;
22.Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 W. Green Street, Urbana, IL 61801, USA;
23.Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, B1900FWA, La Plata, Argentina;
24.Instituto de Astrofisica de La Plata (IALP), CCT-CONICET-UNLP, Paseo del Bosque S/N, B1900FWA, La Plata, Argentina;
25.Department of Astrophysics, Pontificia Universidad Catolica de Chile, Santiago, Chile;
26.Department of Physics, Tsinghua University, Shuangqing Road, Beijing, People's Republic of China;
27.The Observatories of the Carnegie Institute for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA;
28.Department of Physics & Astronomy, University of Southern California, Los Angeles, CA 90089, USA;
29.Department of Physics and Astronomy, Rutgers, the State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854, USA;
30.Institute for Astronomy, University of Hawai'i, 640 N. A'ohoku Pl., Hilo, HI 96720, USA;
31.Department of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ, UK;
32.Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA;
33.Department Physics and Astronomy, University of California, Los Angeles, Los Angeles, CA 90095-1547, USA;
34.Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 W. Green Street, IL 61801, USA;
35.Center for Astrophysical Surveys, National Center for Supercomputing Applications, Urbana, IL 61801, USA;
36.Yunnan Observatories (YNAO), Chinese Academy of Sciences, Kunming 650216, People's Republic of China;
37.Key Laboratory for the Structure and Evolution of Celestial Objects, CAS, Kunming, 650216, People's Republic of China
推荐引用方式
GB/T 7714		 Jacobson-Galán, W. V.,Dessart, L.,Davis, K. W.,et al. Final Moments. II. Observational Properties and Physical Modeling of Circumstellar-material-interacting Type II Supernovae[J]. ASTROPHYSICAL JOURNAL,2024,970(2).
APA Jacobson-Galán, W. V..,Dessart, L..,Davis, K. W..,Kilpatrick, C. D..,Margutti, R..,...&Zheng, W..(2024).Final Moments. II. Observational Properties and Physical Modeling of Circumstellar-material-interacting Type II Supernovae.ASTROPHYSICAL JOURNAL,970(2).
MLA Jacobson-Galán, W. V.,et al."Final Moments. II. Observational Properties and Physical Modeling of Circumstellar-material-interacting Type II Supernovae".ASTROPHYSICAL JOURNAL 970.2(2024).
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