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Title: The bumpy light curve of Type IIn supernova iPTF13z over 3 years

Abstract

A core-collapse (CC) supernova (SN) of Type IIn is dominated by the interaction of SN ejecta with the circumstellar medium (CSM). Some SNe IIn (e.g. SN 2006jd) have episodes of re-brightening ("bumps") in their light curves. We present iPTF13z, a Type IIn SN discovered on 2013 February 1 by the intermediate Palomar Transient Factory (iPTF). This SN showed at least five bumps in its declining light curve between 130 and 750 days after discovery. We analyse this peculiar behaviour and try to infer the properties of the CSM, of the SN explosion, and the nature of the progenitor star. We obtained multi-band optical photometry for over 1000 days after discovery with the P48 and P60 telescopes at Palomar Observatory. We obtained low-resolution optical spectra during the same period. We did an archival search for progenitor outbursts. We analyse the photometry and the spectra, and compare iPTF13z to other SNe IIn. In particular we derive absolute magnitudes, colours, a pseudo-bolometric light curve, and the velocities of the different components of the spectral lines. A simple analytical model is used to estimate the properties of the CSM. iPTF13z had a light curve peaking at M r ≤ 18.3 mag. The five bumpsmore » during its decline phase had amplitudes ranging from 0.4 to 0.9 mag and durations between 20 and 120 days. The most prominent bumps appeared in all the different optical bands, when covered. The spectra of this SN showed typical SN IIn characteristics, with emission lines of Hα (with broad component FWHM ~ 10 3 - 10 4 km s -1 and narrow component FWHM ~ 10 2 km s -1 ) and He i, but also with Fe ii, Ca ii, Na i D and Hβ P Cygni profiles (with velocities of ~ 10 3 km s -1). A pre-explosion outburst was identified lasting ≳ 50 days, with M r ≤ 15 mag around 210 days before discovery. Large, variable progenitor mass-loss rates (≳ 0.01M yr -1) and CSM densities (10 -16 g cm -3) are derived. The SN was hosted by a metal-poor dwarf galaxy at redshift z = 0.0328. We suggest that the light curve bumps of iPTF13z arose from SN ejecta interacting with denser regions in the CSM, possibly produced by the eruptions of a luminous blue variable progenitor star.« less

Authors:
; ; ; ; ; ; ; ; ; ; ; ;
Publication Date:
Research Org.:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States); Lawrence Berkeley National Laboratory-National Energy Research Scientific Computing Center
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1437968
DOE Contract Number:  
AC02-05CH11231
Resource Type:
Journal Article
Journal Name:
Astronomy and Astrophysics
Additional Journal Information:
Journal Volume: 605; Journal ID: ISSN 0004-6361
Publisher:
EDP Sciences
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS

Citation Formats

Nyholm, A., Sollerman, J., Taddia, F., Fremling, C., Moriya, T. J., Ofek, E. O., Gal-Yam, A., De Cia, A., Roy, R., Kasliwal, M. M., Cao, Y., Nugent, P. E., and Masci, F. J. The bumpy light curve of Type IIn supernova iPTF13z over 3 years. United States: N. p., 2017. Web. doi:10.1051/0004-6361/201629906.
Nyholm, A., Sollerman, J., Taddia, F., Fremling, C., Moriya, T. J., Ofek, E. O., Gal-Yam, A., De Cia, A., Roy, R., Kasliwal, M. M., Cao, Y., Nugent, P. E., & Masci, F. J. The bumpy light curve of Type IIn supernova iPTF13z over 3 years. United States. doi:10.1051/0004-6361/201629906.
Nyholm, A., Sollerman, J., Taddia, F., Fremling, C., Moriya, T. J., Ofek, E. O., Gal-Yam, A., De Cia, A., Roy, R., Kasliwal, M. M., Cao, Y., Nugent, P. E., and Masci, F. J. Tue . "The bumpy light curve of Type IIn supernova iPTF13z over 3 years". United States. doi:10.1051/0004-6361/201629906.
@article{osti_1437968,
title = {The bumpy light curve of Type IIn supernova iPTF13z over 3 years},
author = {Nyholm, A. and Sollerman, J. and Taddia, F. and Fremling, C. and Moriya, T. J. and Ofek, E. O. and Gal-Yam, A. and De Cia, A. and Roy, R. and Kasliwal, M. M. and Cao, Y. and Nugent, P. E. and Masci, F. J.},
abstractNote = {A core-collapse (CC) supernova (SN) of Type IIn is dominated by the interaction of SN ejecta with the circumstellar medium (CSM). Some SNe IIn (e.g. SN 2006jd) have episodes of re-brightening ("bumps") in their light curves. We present iPTF13z, a Type IIn SN discovered on 2013 February 1 by the intermediate Palomar Transient Factory (iPTF). This SN showed at least five bumps in its declining light curve between 130 and 750 days after discovery. We analyse this peculiar behaviour and try to infer the properties of the CSM, of the SN explosion, and the nature of the progenitor star. We obtained multi-band optical photometry for over 1000 days after discovery with the P48 and P60 telescopes at Palomar Observatory. We obtained low-resolution optical spectra during the same period. We did an archival search for progenitor outbursts. We analyse the photometry and the spectra, and compare iPTF13z to other SNe IIn. In particular we derive absolute magnitudes, colours, a pseudo-bolometric light curve, and the velocities of the different components of the spectral lines. A simple analytical model is used to estimate the properties of the CSM. iPTF13z had a light curve peaking at Mr ≤ 18.3 mag. The five bumps during its decline phase had amplitudes ranging from 0.4 to 0.9 mag and durations between 20 and 120 days. The most prominent bumps appeared in all the different optical bands, when covered. The spectra of this SN showed typical SN IIn characteristics, with emission lines of Hα (with broad component FWHM ~ 103 - 104 km s-1 and narrow component FWHM ~ 102 km s-1 ) and He i, but also with Fe ii, Ca ii, Na i D and Hβ P Cygni profiles (with velocities of ~ 103 km s-1). A pre-explosion outburst was identified lasting ≳ 50 days, with Mr ≤ 15 mag around 210 days before discovery. Large, variable progenitor mass-loss rates (≳ 0.01M⊙ yr-1) and CSM densities (10-16 g cm-3) are derived. The SN was hosted by a metal-poor dwarf galaxy at redshift z = 0.0328. We suggest that the light curve bumps of iPTF13z arose from SN ejecta interacting with denser regions in the CSM, possibly produced by the eruptions of a luminous blue variable progenitor star.},
doi = {10.1051/0004-6361/201629906},
journal = {Astronomy and Astrophysics},
issn = {0004-6361},
number = ,
volume = 605,
place = {United States},
year = {2017},
month = {8}
}