A significantly off-centre 56Ni distribution for the low-luminosity type Ia supernova SN 2016brx from the 100IAS survey

Subo Dong; Boaz Katz; Juna A. Kollmeier; Doron Kushnir; N. Elias-Rosa; Subhash Bose; Nidia Morrell; J. L. Prieto; Ping Chen; C. S. Kochanek; G. M. Brandt; T. W-S Holoien; Avishay Gal-Yam; Antonia Morales-Garoffolo; Stuart Parker; M. M. Phillips; Anthony L. Piro; B. J. Shappee; Joshua D. Simon; K. Z. Stanek

doi:10.1093/mnrasl/sly098

A significantly off-centre ⁵⁶Ni distribution for the low-luminosity type Ia supernova SN 2016brx from the 100IAS survey

Subo Dong, Boaz Katz, Juna A. Kollmeier, Doron Kushnir, N. Elias-Rosa, Subhash Bose, Nidia Morrell, J. L. Prieto, Ping Chen, C. S. Kochanek, G. M. Brandt, T. W-S Holoien, Avishay Gal-Yam, Antonia Morales-Garoffolo, Stuart Parker, M. M. Phillips, Anthony L. Piro, B. J. Shappee, Joshua D. Simon, K. Z. Stanek

Department of Particle Physics and Astrophysics

Weizmann Institute of Science

Research output: Contribution to journal › Article › peer-review

Abstract

We present nebular-phase spectra of the Type Ia supernova (SN Ia) 2016brx, a member of the 1991bg-like subclass that lies at the faint end of the SN Ia luminosity function. Nebular spectra are available for only three other 1991bg-like SNe, and their Co line centres are all within ≲ 500 km s ^-1 of each other. In contrast, the nebular Co line centre of SN 2016brx is blue-shifted by > 1500 km s ^-1 compared to them and by ≈ 1200 km s ^-1 compared to the rest frame. This is a significant shift relative to the narrow nebular line velocity dispersion of ≲2000 km s ^-1 of these SNe. The large range of nebular line shifts implies that the ⁵⁶Ni in the ejecta of SN1991bg-like events is off-centre by~1000 km s ^-1 rather than universally centrally confined as previously suggested.With the addition of SN 2016brx, the Co nebular line shapes of 1991bg-like objects appear to connect with the brighter SNe Ia that show double-peaked profiles, hinting at a continuous distribution of line profiles among SNe Ia. One class of models to produce both off-centre and bimodal ⁵⁶Ni distributions is collisions of white dwarfs with unequal and equal masses.

Original language	English
Pages (from-to)	L70-L75
Number of pages	6
Journal	MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume	479
Issue number	1
Early online date	2 Jun 2018
DOIs	https://doi.org/10.1093/mnrasl/sly098
State	Published - Sep 2018

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1093/mnrasl/sly098

http://arxiv.org/pdf/1805.00010License: Other

Cite this

Dong, S., Katz, B., Kollmeier, J. A., Kushnir, D., Elias-Rosa, N., Bose, S., Morrell, N., Prieto, J. L., Chen, P., Kochanek, C. S., Brandt, G. M., Holoien, T. W.-S., Gal-Yam, A., Morales-Garoffolo, A., Parker, S., Phillips, M. M., Piro, A. L., Shappee, B. J., Simon, J. D., & Stanek, K. Z. (2018). A significantly off-centre ⁵⁶Ni distribution for the low-luminosity type Ia supernova SN 2016brx from the 100IAS survey. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 479(1), L70-L75. https://doi.org/10.1093/mnrasl/sly098

@article{8959994d677d4b9fbc1410338187f0b5,

title = "A significantly off-centre 56Ni distribution for the low-luminosity type Ia supernova SN 2016brx from the 100IAS survey",

abstract = "We present nebular-phase spectra of the Type Ia supernova (SN Ia) 2016brx, a member of the 1991bg-like subclass that lies at the faint end of the SN Ia luminosity function. Nebular spectra are available for only three other 1991bg-like SNe, and their Co line centres are all within ≲ 500 km s -1 of each other. In contrast, the nebular Co line centre of SN 2016brx is blue-shifted by > 1500 km s -1 compared to them and by ≈ 1200 km s -1 compared to the rest frame. This is a significant shift relative to the narrow nebular line velocity dispersion of ≲2000 km s -1 of these SNe. The large range of nebular line shifts implies that the 56Ni in the ejecta of SN1991bg-like events is off-centre by\textasciitilde{}1000 km s -1 rather than universally centrally confined as previously suggested.With the addition of SN 2016brx, the Co nebular line shapes of 1991bg-like objects appear to connect with the brighter SNe Ia that show double-peaked profiles, hinting at a continuous distribution of line profiles among SNe Ia. One class of models to produce both off-centre and bimodal 56Ni distributions is collisions of white dwarfs with unequal and equal masses. ",

author = "Subo Dong and Boaz Katz and Kollmeier, \{Juna A.\} and Doron Kushnir and N. Elias-Rosa and Subhash Bose and Nidia Morrell and Prieto, \{J. L.\} and Ping Chen and Kochanek, \{C. S.\} and Brandt, \{G. M.\} and Holoien, \{T. W-S\} and Avishay Gal-Yam and Antonia Morales-Garoffolo and Stuart Parker and Phillips, \{M. M.\} and Piro, \{Anthony L.\} and Shappee, \{B. J.\} and Simon, \{Joshua D.\} and Stanek, \{K. Z.\}",

note = "We thank S. Benetti and P. Garnavich for helping with archival spectra. SD, SB, and PC acknowledge Project 11573003 supported by National Science Foundation of China (NSFC). SB is partially supported by China postdoctoral science foundation grant no. 2016M600848. BK is supported by the I-CORE Program (1829/12) and the Beracha Foundation. JLP is supported in part by FONDECYT through grant no. 1151445 and by the Ministry of Economy, Development, and Tourism{\textquoteright}s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. AMG acknowledges financial support by the University of C{\'a}diz grant no. PR2017-64. Partly based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof{\'i}sica de Canarias, on the island of La Palma. ASAS-SN is supported by the Gordon and Betty Moore Foundation through grant no. GBMF5490 to the Ohio State University and NSF grant no. AST-1515927. Development of ASAS-SN has been supported by NSF grant no. AST-0908816, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics at the Ohio State University, the Chinese Academy of Sciences South America Center for Astronomy (CAS-SACA), the Villum Foundation, and George Skestos.",

year = "2018",

month = sep,

doi = "10.1093/mnrasl/sly098",

language = "الإنجليزيّة",

volume = "479",

pages = "L70--L75",

journal = "MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "1",

}

Dong, S, Katz, B, Kollmeier, JA, Kushnir, D, Elias-Rosa, N, Bose, S, Morrell, N, Prieto, JL, Chen, P, Kochanek, CS, Brandt, GM, Holoien, TW-S, Gal-Yam, A, Morales-Garoffolo, A, Parker, S, Phillips, MM, Piro, AL, Shappee, BJ, Simon, JD & Stanek, KZ 2018, 'A significantly off-centre ⁵⁶Ni distribution for the low-luminosity type Ia supernova SN 2016brx from the 100IAS survey', MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, vol. 479, no. 1, pp. L70-L75. https://doi.org/10.1093/mnrasl/sly098

TY - JOUR

T1 - A significantly off-centre 56Ni distribution for the low-luminosity type Ia supernova SN 2016brx from the 100IAS survey

AU - Dong, Subo

AU - Katz, Boaz

AU - Kollmeier, Juna A.

AU - Kushnir, Doron

AU - Elias-Rosa, N.

AU - Bose, Subhash

AU - Morrell, Nidia

AU - Prieto, J. L.

AU - Chen, Ping

AU - Kochanek, C. S.

AU - Brandt, G. M.

AU - Holoien, T. W-S

AU - Gal-Yam, Avishay

AU - Morales-Garoffolo, Antonia

AU - Parker, Stuart

AU - Phillips, M. M.

AU - Piro, Anthony L.

AU - Shappee, B. J.

AU - Simon, Joshua D.

AU - Stanek, K. Z.

N1 - We thank S. Benetti and P. Garnavich for helping with archival spectra. SD, SB, and PC acknowledge Project 11573003 supported by National Science Foundation of China (NSFC). SB is partially supported by China postdoctoral science foundation grant no. 2016M600848. BK is supported by the I-CORE Program (1829/12) and the Beracha Foundation. JLP is supported in part by FONDECYT through grant no. 1151445 and by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. AMG acknowledges financial support by the University of Cádiz grant no. PR2017-64. Partly based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma. ASAS-SN is supported by the Gordon and Betty Moore Foundation through grant no. GBMF5490 to the Ohio State University and NSF grant no. AST-1515927. Development of ASAS-SN has been supported by NSF grant no. AST-0908816, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics at the Ohio State University, the Chinese Academy of Sciences South America Center for Astronomy (CAS-SACA), the Villum Foundation, and George Skestos.

PY - 2018/9

Y1 - 2018/9

N2 - We present nebular-phase spectra of the Type Ia supernova (SN Ia) 2016brx, a member of the 1991bg-like subclass that lies at the faint end of the SN Ia luminosity function. Nebular spectra are available for only three other 1991bg-like SNe, and their Co line centres are all within ≲ 500 km s -1 of each other. In contrast, the nebular Co line centre of SN 2016brx is blue-shifted by > 1500 km s -1 compared to them and by ≈ 1200 km s -1 compared to the rest frame. This is a significant shift relative to the narrow nebular line velocity dispersion of ≲2000 km s -1 of these SNe. The large range of nebular line shifts implies that the 56Ni in the ejecta of SN1991bg-like events is off-centre by~1000 km s -1 rather than universally centrally confined as previously suggested.With the addition of SN 2016brx, the Co nebular line shapes of 1991bg-like objects appear to connect with the brighter SNe Ia that show double-peaked profiles, hinting at a continuous distribution of line profiles among SNe Ia. One class of models to produce both off-centre and bimodal 56Ni distributions is collisions of white dwarfs with unequal and equal masses.

AB - We present nebular-phase spectra of the Type Ia supernova (SN Ia) 2016brx, a member of the 1991bg-like subclass that lies at the faint end of the SN Ia luminosity function. Nebular spectra are available for only three other 1991bg-like SNe, and their Co line centres are all within ≲ 500 km s -1 of each other. In contrast, the nebular Co line centre of SN 2016brx is blue-shifted by > 1500 km s -1 compared to them and by ≈ 1200 km s -1 compared to the rest frame. This is a significant shift relative to the narrow nebular line velocity dispersion of ≲2000 km s -1 of these SNe. The large range of nebular line shifts implies that the 56Ni in the ejecta of SN1991bg-like events is off-centre by~1000 km s -1 rather than universally centrally confined as previously suggested.With the addition of SN 2016brx, the Co nebular line shapes of 1991bg-like objects appear to connect with the brighter SNe Ia that show double-peaked profiles, hinting at a continuous distribution of line profiles among SNe Ia. One class of models to produce both off-centre and bimodal 56Ni distributions is collisions of white dwarfs with unequal and equal masses.

U2 - 10.1093/mnrasl/sly098

DO - 10.1093/mnrasl/sly098

M3 - مقالة

SN - 0035-8711

VL - 479

SP - L70-L75

JO - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

JF - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

IS - 1