2016A&A...592A..89T


Query : 2016A&A...592A..89T

2016A&A...592A..89T - Astronomy and Astrophysics, volume 592A, 89-89 (2016/8-1)

iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor.

TADDIA F., FREMLING C., SOLLERMAN J., CORSI A., GAL-YAM A., KARAMEHMETOGLU E., LUNNAN R., BUE B., ERGON M., KASLIWAL M., VREESWIJK P.M. and WOZNIAK P.R.

Abstract (from CDS):

Context. Type Ic supernovae (SNe Ic) arise from the core-collapse of H- (and He-) poor stars, which could either be single Wolf-Rayet (WR) stars or lower-mass stars stripped of their envelope by a companion. Their light curves are radioactively powered and usually show a fast rise to peak (∼10-15d), without any early (in the first few days) emission bumps (with the exception of broad-lined SNe Ic) as sometimes seen for other types of stripped-envelope SNe (e.g., Type IIb SN 1993J and Type Ib SN 2008D).
Aims. We have studied iPTF15dtg, a spectroscopically normal SN Ic with an early excess in the optical light curves followed by a long (∼30d) rise to the main peak. It is the first spectroscopically-normal double-peaked SN Ic to be observed. Our aim is to determine the properties of this explosion and of its progenitor star.
Methods. Optical photometry and spectroscopy of iPTF15dtg was obtained with multiple telescopes. The resulting light curves and spectral sequence are analyzed and modeled with hydrodynamical and analytical models, with particular focus on the early emission.
Results. iPTF15dtg is a slow rising SN Ic, similar to SN 2011bm. Hydrodynamical modeling of the bolometric properties reveals a large ejecta mass (∼10M) and strong 56Ni mixing. The luminous early emission can be reproduced if we account for the presence of an extended (≥500R), low-mass (≥0.045M) envelope around the progenitor star. Alternative scenarios for the early peak, such as the interaction with a companion, a shock-breakout (SBO) cooling tail from the progenitor surface, or a magnetar-driven SBO are not favored.
Conclusions. The large ejecta mass and the presence of H- and He-free extended material around the star suggest that the progenitor of iPTF15dtg was a massive (≥35M) WR star that experienced strong mass loss.

Abstract Copyright: © ESO, 2016

Journal keyword(s): supernovae: general - supernovae: general

Simbad objects: 22

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Number of rows : 22
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 iPTF 15dtg SN* 02 30 20.05 +37 14 06.7           SNIc 35 0
2 SN 2007gr SN* 02 43 27.98 +37 20 44.7       12.77   SNIc 217 1
3 SN 2013ez SN* 02 53 56.70 +13 23 13.6           ~ 86 0
4 SN 2006aj SN* 03 21 39.670 +16 52 02.27 17.96 19.11 17.40     SNIc-BL 902 1
5 SN 2010bh SN* 07 10 30.63 -56 15 19.7           SNIc 267 1
6 SN 2008D SN* 09 09 30.625 +33 08 20.16     17.5     SNIb 387 1
7 SN 2006jc SN* 09 17 20.78 +41 54 32.7     13.8     SNIbn 319 1
8 SN 1993J SN* 09 55 24.77476 +69 01 13.7026   10.8 12.0     SNIIb 1364 1
9 SN 2005bf SN* 10 23 56.99 -03 11 29.3     18.0     SNIb 191 1
10 SN 2013ge SN* 10 34 48.46 +21 39 41.9           SNIc 43 1
11 SN 2004aw SN* 11 57 50.24 +25 15 55.1   18.06       SNIc 188 1
12 SN 2011bm SN* 12 56 53.89 +22 22 28.2           SNIc 57 1
13 PTF 11bov SN* 12 56 53.94 +22 22 28.1           SNIc 7 0
14 PTF 11qcj SN* 13 13 41.51 +47 17 57.0           SNIb 48 0
15 SN 1994I SN* 13 29 54.072 +47 11 30.50     12.9     SNIc 610 1
16 SN 2011dh SN* 13 30 05.10555 +47 10 10.9227           SNIIb 353 1
17 SN 2013dx SN* 14 29 14.77 +15 46 26.6           ~ 136 0
18 SN 2013cu SN* 14 33 58.97 +40 14 20.7           SNII: 79 1
19 iPTF 13bvn SN* 15 00 00.152 +01 52 53.17           SNIb 152 0
20 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1764 2
21 SN 2006oz SN* 22 08 53.56 +00 53 50.4           SLSNIc 80 1
22 PTF 10vgv SN* 22 16 01.17 +40 52 03.3           SNIc 25 0

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2023.02.02-20:04:27

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