Massive stars exploding in a He-rich circumstellar medium X. Flash spectral features in the Type Ibn SN 2019cj and observations of SN2018jmt

被引：0

作者：

Wang, Z. -Y. ^{[1
,2
]}

Pastorello, A. ^{[3
]}

Maeda, K. ^{[4
]}

Reguitti, A. ^{[3
,5
]}

Cai, Y. -Z. ^{[6
,7
,8
]}

Howell, D. Andrew ^{[9
,10
]}

Benetti, S. ^{[3
]}

Buckley, D. A. H. ^{[11
,12
,13
]}

Cappellaro, E. ^{[3
]}

Carini, R. ^{[14
]}

Cartier, R. ^{[15
]}

Chen, T. -W. ^{[16
]}

Elias-Rosa, N. ^{[3
,17
]}

Fang, Q. -L. ^{[4
]}

Gal-Yam, A. ^{[18
]}

Gangopadhyay, A. ^{[19
]}

Gromadzki, M. ^{[20
]}

Gan, W-P. ^{[21
]}

Hiramatsu, D. ^{[22
,23
]}

Hu, M. -K. ^{[24
]}

Inserra, C. ^{[25
]}

McCully, C. ^{[9
]}

Nicholl, M. ^{[26
]}

Olivares, F. E. ^{[27
]}

Pignata, G. ^{[28
]}

Pineda-Garcia, J. ^{[29
]}

Pursiainen, M. ^{[30
]}

Ragosta, F. ^{[14
,31
]}

Rau, A. ^{[32
]}

Roy, R. ^{[33
]}

Sollerman, J. ^{[19
]}

Tartaglia, L. ^{[34
]}

Terreran, G. ^{[9
,10
]}

Valerin, G. ^{[3
]}

Wang, Q. ^{[35
]}

Wang, S. -Q. ^{[21
]}

Young, D. R. ^{[26
]}

Aryan, A. ^{[16
]}

Bronikowski, M. ^{[36
]}

Concepcion, E. ^{[36
]}

Galbany, L. ^{[17
,37
]}

Lin, H. ^{[6
,7
,8
]}

Melandri, A. ^{[14
]}

Petrushevska, T. ^{[36
]}

Ramirez, M. ^{[29
,38
]}

Shi, D. -D. ^{[39
,40
]}

Warwick, B. ^{[30
]}

Zhang, J-J. ^{[6
,7
,8
]}

Wang, B. ^{[6
,7
,8
]}

Wang, X-F. ^{[24
]}

机构：

[1] Beijing Normal Univ, Sch Phys & Astron, Beijing 100875, Peoples R China

[2] Beijing Normal Univ, Fac Arts & Sci, Dept Phys, Zhuhai 519087, Peoples R China

[3] INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[4] Kyoto Univ, Dept Astron, Kitashirakawa Oiwake Cho,Sakyo Ku, Kyoto 6068502, Japan

[5] INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, LC, Italy

[6] Chinese Acad Sci, Yunnan Observ, Kunming 650216, Yunnan, Peoples R China

[7] Yunnan Key Lab, Int Ctr Supernovae, Kunming 650216, Yunnan, Peoples R China

[8] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650216, Yunnan, Peoples R China

[9] Las Cumbres Observ, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA

[10] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[11] South African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa

[12] Univ Cape Town, Dept Astron, Private Bag X3, ZA-7701 Rondebosch, South Africa

[13] Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa

[14] INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy

[15] Univ Diego Port, Fac Ingn & Ciencias, Inst Estudios Astrofis, Ave Ejercito Libertador 441, Santiago, Chile

[16] Natl Cent Univ, Grad Inst Astron, 300 Jhongda Rd, Jhongli 32001, Taiwan

[17] CSIC, Inst Space Sci ICE, Carrer Can Magrans S-N, E-08193 Barcelona, Spain

[18] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel

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

[20] Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland

[21] Guangxi Univ, Sch Phys Sci & Technol, Guangxi Key Lab Relativist Astrophys, Nanning 530004, Peoples R China

[22] Ctr Astrophys Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138 USA

[23] NSF Inst Artificial Intelligence & Fundamental In, Cambridge, MA USA

[24] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China

[25] Cardiff Univ, Sch Phys & Astron, Cardiff Hub Astrophys Res & Technol, Queens Bldg, Cardiff CF24 3AA, Wales

[26] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland

[27] UKIRT Observ, Inst Astron, 640 N Aohoku Pl,Univ Pk, Hilo, HI 96720 USA

[28] Univ Tarapaca, Inst Alta Invest, Casilla 7D, Arica, Chile

[29] Univ Andres Bello, Fac Ciencias Exactas, Inst Astrofis, Ave Fernandez Concha 700, Santiago, Chile

[30] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England

[31] Space Sci Data Ctr ASI, Via Politecn SNC, I-00133 Rome, Italy

[32] Max Planck Inst Extraterr Phys, Giessenbach Str 1, D-85748 Garching, Germany

[33] Manipal Acad Higher Educ, Manipal Ctr Nat Sci, Manipal 576104, Karnataka, India

[34] INAF, Osservatorio Astron Abruzzo, Via M Maggini Snc, I-64100 Teramo, Italy

[35] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[36] Univ Nova Gorica, Ctr Astrophys & Cosmol, Vipavska 11c, Ajdovscina 5270, Slovenia

[37] Inst Estud Espacials Catalunya IEEC, Castelldefels 08860, Barcelona, Spain

[38] Millennium Inst Astrophys, Nuncio Monsenor Sotero Sanz 100,Of 104, Santiago, Chile

[39] Anhui Univ Sci & Technol, Ctr Fundamental Phys, Sch Mech & Opt Elect Phys, Huainan 232001, Anhui, Peoples R China

[40] Chinese Acad Sci, Purple Mt Observ, 10 Yuan Hua Rd, Nanjing 210023, Jiangsu, Peoples R China

[41] Beijing Normal Univ, Inst Frontier Astron & Astrophys, Beijing 102206, Peoples R China

[42] Beijing Normal Univ, Adv Inst Nat Sci, Zhuhai 519087, Peoples R China

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 691卷

基金：

国家重点研发计划; 美国国家科学基金会; 英国科学技术设施理事会; 英国科研创新办公室; 美国国家航空航天局; 欧洲研究理事会; 中国国家自然科学基金; 美国安德鲁·梅隆基金会;

关键词：

circumstellar matter; supernovae: general; supernovae: individual: SN 2018jmt; supernovae: individual: SN 2019cj; PULSATIONAL PAIR-INSTABILITY; PRE-SUPERNOVA OUTBURSTS; CORE-COLLAPSE; DIVERSE PROPERTIES; EXPLOSION SITES; DUST FORMATION; IC SUPERNOVA; LIGHT-CURVE; PROGENITOR; SPECTROSCOPY;

D O I：

10.1051/0004-6361/202451131

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present optical and near-infrared observations of two Type Ibn supernovae (SNe), SN 2018jmt and SN 2019cj. Their light curves have rise times of about ten days, reaching an absolute peak magnitude of M-g (SN 2018jmt) = -19.07 +/- 0.37 and M-V(SN 2019cj) = -18.94 +/- 0.19 mag, respectively. The early-time spectra of SN 2018jmt are dominated by a blue continuum, accompanied by narrow (600 1000 km s(-1)) He i lines with the P-Cygni profile. At later epochs, the spectra become more similar to those of the prototypical SN Ibn 2006jc. At early phases, the spectra of SN 2019cj show flash ionisation emission lines of C iii, N iii, and He ii superposed on a blue continuum. These features disappear after a few days, and then the spectra of SN 2019cj evolve similarly to those of SN 2018jmt. The spectra indicate that the two SNe exploded within a He-rich circumstellar medium (CSM) lost by the progenitors a short time before the explosion. We modelled the light curves of the two SNe Ibn to constrain the progenitor and the explosion parameters. The ejecta masses are consistent with either what is expected for a canonical SN Ib (similar to 2M(circle dot)) or for a massive Wolf Rayet star (>similar to 4M(circle dot)), with the kinetic energy on the order of 1051 erg. The lower limit on the ejecta mass (>similar to 2M(circle dot)) argues against a scenario involving a relatively low-mass progenitor (e.g. M-ZAMS similar to 10M(circle dot)). We set a conservative upper limit of similar to 0.1M(circle dot) for the Ni-56 masses in both SNe. From the light curve modelling, we determined a two-zone CSM distribution, with an inner, flat CSM component and an outer CSM with a steeper density profile. The physical properties of SN 2018jmt and SN 2019cj are consistent with those expected from the core collapse of relatively massive envelope-stripped stars.

引用

页数：21

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