TY - JOUR
T1 - The Fast-evolving Type Ib Supernova SN 2015dj in NGC 7371
AU - Singh, Mridweeka
AU - Misra, Kuntal
AU - Valenti, Stefano
AU - Hosseinzadeh, Griffin
AU - Pastorello, Andrea
AU - Srivastav, Shubham
AU - Gangopadhyay, Anjasha
AU - Dastidar, Raya
AU - Tomasella, Lina
AU - Arcavi, Iair
AU - Benetti, Stefano
AU - Callis, Emma
AU - Cappellaro, Enrico
AU - Elias-Rosa, Nancy
AU - Howell, D. Andrew
AU - Kim, Sang Chul
AU - McCully, Curtis
AU - Tartaglia, Leonardo
AU - Terreran, Giacomo
AU - Turatto, Massimo
N1 - Publisher Copyright:
© 2021. The American Astronomical Society. All rights reserved.
PY - 2021/3/10
Y1 - 2021/3/10
N2 - We present the detailed optical evolution of a Type Ib SN 2015dj in NGC 7371, using data spanning up to ∼170 days after discovery. SN 2015dj shares similarity in light-curve shape with SN 2007gr and peaks at M V = -17.37 0.02 mag. Analytical modeling of the quasi bolometric light curve yields 0.06 0.01 M o˙ of 56Ni, ejecta mass M o˙, and kinetic energy erg. The spectral features show a fast evolution and resemble those of spherically symmetric ejecta. The analysis of nebular phase spectral lines indicates a progenitor mass between 13-20 M o˙, suggesting a binary scenario.
AB - We present the detailed optical evolution of a Type Ib SN 2015dj in NGC 7371, using data spanning up to ∼170 days after discovery. SN 2015dj shares similarity in light-curve shape with SN 2007gr and peaks at M V = -17.37 0.02 mag. Analytical modeling of the quasi bolometric light curve yields 0.06 0.01 M o˙ of 56Ni, ejecta mass M o˙, and kinetic energy erg. The spectral features show a fast evolution and resemble those of spherically symmetric ejecta. The analysis of nebular phase spectral lines indicates a progenitor mass between 13-20 M o˙, suggesting a binary scenario.
UR - http://www.scopus.com/inward/record.url?scp=85103237756&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/abdf5c
DO - 10.3847/1538-4357/abdf5c
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AN - SCOPUS:85103237756
SN - 0004-637X
VL - 909
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
ER -