SN 2010MB: Direct evidence for a supernova interacting with a large amount of hydrogen-free circumstellar material

Sagi Ben-Ami; Avishay Gal-Yam; Paolo A. Mazzali; Orly Gnat; Maryam Modjaz; Itay Rabinak; Mark Sullivan; Lars Bildsten; Dovi Poznanski; Ofer Yaron; Iair Arcavi; Joshua S. Bloom; Assaf Horesh; Mansi M. Kasliwal; Shrinivas R. Kulkarni; Peter E. Nugent; Eran O. Ofek; Daniel Perley; Robert Quimby; Dong Xu

doi:10.1088/0004-637X/785/1/37

SN 2010MB: Direct evidence for a supernova interacting with a large amount of hydrogen-free circumstellar material

Sagi Ben-Ami, Avishay Gal-Yam, Paolo A. Mazzali, Orly Gnat, Maryam Modjaz, Itay Rabinak, Mark Sullivan, Lars Bildsten, Dovi Poznanski, Ofer Yaron, Iair Arcavi, Joshua S. Bloom, Assaf Horesh, Mansi M. Kasliwal, Shrinivas R. Kulkarni, Peter E. Nugent, Eran O. Ofek, Daniel Perley, Robert Quimby, Dong Xu

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

Abstract

We present our observations of SN 2010mb, a Type Ic supernova (SN) lacking spectroscopic signatures of H and He. SN 2010mb has a slowly declining light curve (LC) (600 days) that cannot be powered by ⁵⁶Ni/⁵⁶Co radioactivity, the common energy source for Type Ic SNe. We detect signatures of interaction with hydrogen-free circumstellar material including a blue quasi-continuum and, uniquely, narrow oxygen emission lines that require high densities (10⁹ cm^-3). From the observed spectra and LC, we estimate that the amount of material involved in the interaction was 3 M . Our observations are in agreement with models of pulsational pair-instability SNe described in the literature.

Original language	English (US)
Article number	37
Journal	Astrophysical Journal
Volume	785
Issue number	1
DOIs	https://doi.org/10.1088/0004-637X/785/1/37
State	Published - Apr 10 2014

Keywords

stars: Population III
stars: mass-loss
supernovae: general

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1088/0004-637X/785/1/37

Cite this

Ben-Ami, S., Gal-Yam, A., Mazzali, P. A., Gnat, O., Modjaz, M., Rabinak, I., Sullivan, M., Bildsten, L., Poznanski, D., Yaron, O., Arcavi, I., Bloom, J. S., Horesh, A., Kasliwal, M. M., Kulkarni, S. R., Nugent, P. E., Ofek, E. O., Perley, D., Quimby, R., & Xu, D. (2014). SN 2010MB: Direct evidence for a supernova interacting with a large amount of hydrogen-free circumstellar material. Astrophysical Journal, 785(1), [37]. https://doi.org/10.1088/0004-637X/785/1/37

Ben-Ami, S, Gal-Yam, A, Mazzali, PA, Gnat, O, Modjaz, M, Rabinak, I, Sullivan, M, Bildsten, L, Poznanski, D, Yaron, O, Arcavi, I, Bloom, JS, Horesh, A, Kasliwal, MM, Kulkarni, SR, Nugent, PE, Ofek, EO, Perley, D, Quimby, R & Xu, D 2014, 'SN 2010MB: Direct evidence for a supernova interacting with a large amount of hydrogen-free circumstellar material', Astrophysical Journal, vol. 785, no. 1, 37. https://doi.org/10.1088/0004-637X/785/1/37

@article{6a96535773bb41e786a8a0c3f073c14a,

title = "SN 2010MB: Direct evidence for a supernova interacting with a large amount of hydrogen-free circumstellar material",

abstract = "We present our observations of SN 2010mb, a Type Ic supernova (SN) lacking spectroscopic signatures of H and He. SN 2010mb has a slowly declining light curve (LC) (600 days) that cannot be powered by 56Ni/56Co radioactivity, the common energy source for Type Ic SNe. We detect signatures of interaction with hydrogen-free circumstellar material including a blue quasi-continuum and, uniquely, narrow oxygen emission lines that require high densities (109 cm-3). From the observed spectra and LC, we estimate that the amount of material involved in the interaction was 3 M . Our observations are in agreement with models of pulsational pair-instability SNe described in the literature.",

keywords = "stars: Population III, stars: mass-loss, supernovae: general",

author = "Sagi Ben-Ami and Avishay Gal-Yam and Mazzali, {Paolo A.} and Orly Gnat and Maryam Modjaz and Itay Rabinak and Mark Sullivan and Lars Bildsten and Dovi Poznanski and Ofer Yaron and Iair Arcavi and Bloom, {Joshua S.} and Assaf Horesh and Kasliwal, {Mansi M.} and Kulkarni, {Shrinivas R.} and Nugent, {Peter E.} and Ofek, {Eran O.} and Daniel Perley and Robert Quimby and Dong Xu",

year = "2014",

month = apr,

day = "10",

doi = "10.1088/0004-637X/785/1/37",

language = "English (US)",

volume = "785",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing Ltd.",

number = "1",

}

TY - JOUR

T1 - SN 2010MB

T2 - Direct evidence for a supernova interacting with a large amount of hydrogen-free circumstellar material

AU - Ben-Ami, Sagi

AU - Gal-Yam, Avishay

AU - Mazzali, Paolo A.

AU - Gnat, Orly

AU - Modjaz, Maryam

AU - Rabinak, Itay

AU - Sullivan, Mark

AU - Bildsten, Lars

AU - Poznanski, Dovi

AU - Yaron, Ofer

AU - Arcavi, Iair

AU - Bloom, Joshua S.

AU - Horesh, Assaf

AU - Kasliwal, Mansi M.

AU - Kulkarni, Shrinivas R.

AU - Nugent, Peter E.

AU - Ofek, Eran O.

AU - Perley, Daniel

AU - Quimby, Robert

AU - Xu, Dong

PY - 2014/4/10

Y1 - 2014/4/10

N2 - We present our observations of SN 2010mb, a Type Ic supernova (SN) lacking spectroscopic signatures of H and He. SN 2010mb has a slowly declining light curve (LC) (600 days) that cannot be powered by 56Ni/56Co radioactivity, the common energy source for Type Ic SNe. We detect signatures of interaction with hydrogen-free circumstellar material including a blue quasi-continuum and, uniquely, narrow oxygen emission lines that require high densities (109 cm-3). From the observed spectra and LC, we estimate that the amount of material involved in the interaction was 3 M . Our observations are in agreement with models of pulsational pair-instability SNe described in the literature.

AB - We present our observations of SN 2010mb, a Type Ic supernova (SN) lacking spectroscopic signatures of H and He. SN 2010mb has a slowly declining light curve (LC) (600 days) that cannot be powered by 56Ni/56Co radioactivity, the common energy source for Type Ic SNe. We detect signatures of interaction with hydrogen-free circumstellar material including a blue quasi-continuum and, uniquely, narrow oxygen emission lines that require high densities (109 cm-3). From the observed spectra and LC, we estimate that the amount of material involved in the interaction was 3 M . Our observations are in agreement with models of pulsational pair-instability SNe described in the literature.

KW - stars: Population III

KW - stars: mass-loss

KW - supernovae: general

UR - http://www.scopus.com/inward/record.url?scp=84897435980&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84897435980&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/785/1/37

DO - 10.1088/0004-637X/785/1/37

M3 - Article

AN - SCOPUS:84897435980

SN - 0004-637X

VL - 785

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 37

ER -

SN 2010MB: Direct evidence for a supernova interacting with a large amount of hydrogen-free circumstellar material

Abstract

Keywords

ASJC Scopus subject areas

Access to Document

Other files and links

Fingerprint

Cite this