A SPECTROSCOPICALLY NORMAL TYPE Ic SUPERNOVA FROM A VERY MASSIVE PROGENITOR

Valenti, S.; Taubenberger, S.; Pastorello, A.; Aramyan, L. S.; Botticella, M. T.; Fraser, M.; Benetti, S.; Smartt, S. J.; Cappellaro, E.; Elias‐Rosa, N.; Ergon, M.; Magill, L.; Magnier, E. A.; Kotak, R.; Price, P. A.; Sollerman, J.; Tomasella, L.; Turatto, M.; Wright, D. E.

doi:10.1088/2041-8205/749/2/l28

Cited by 81 publications

(78 citation statements)

References 47 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This is also true for other values of binary separation. We also emphasise that the last spectrum of iPTF15dtg reveals a strong [O i] λ6300 line that is similar to that of SN 2011bm, for which a massive, and thus probably single progenitor system, was suggested (Valenti et al 2012). …”

Section: The Companion-interaction Scenariomentioning

confidence: 63%

“…In Fig. 14, we combine the data from Valenti et al (2012) and PTF in r-band (and also in g-band), and it appears that the first r-band point of SN 2011bm displays an excess compared to the expected power-law (PL) rise (red dashed lines) obtained by fitting the early PTF r-band data points. Also in the case of SN 2011bm we thus have an early emission similar to that of iPTF15dtg, although with higher contrast with respect to the main peak.…”

Section: Discussionmentioning

confidence: 97%

“…Another caveat concerning the hydrodynamical model is that SNEC is a 1D code and therefore we cannot take into account geometries that are different from spherical symmetry. Maeda et al (2008), Modjaz et al (2008), Taubenberger et al (2009), andValenti et al (2012) indicate that a signature of bipolar explosions, typical of SNe with central engines, is a double peak in the profile of the nebular oxygen lines (even though the absence of a double peak does not rule out asphericity). We inspected the [O i] λλ6300, 6364 line in our last spectrum (which is not fully nebular) and the double peak is not visible.…”

Section: Discussionmentioning

confidence: 99%

See 2 more Smart Citations

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

Taddia

Fremling

Sollerman

et al. 2016

A&A

View full text Add to dashboard Cite

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 (∼10−15 d), 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 (∼30 d) 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 (∼10 M ) and strong 56 Ni mixing. The luminous early emission can be reproduced if we account for the presence of an extended ( 500 R ), low-mass ( 0.045 M ) 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 ( 35 M ) WR star that experienced strong mass loss.

show abstract

Section: The Companion-interaction Scenariomentioning

confidence: 63%

Section: Discussionmentioning

confidence: 97%

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

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

Taddia

Fremling

Sollerman

et al. 2016

A&A

View full text Add to dashboard Cite

show abstract

“…They span an order of magnitude in peak luminosity and significantly increase the number of known transients with short characteristic times. Other events from the literature are shown as colored circles/squares: Type Ia SNe (Nugent et al 2002;Taubenberger et al 2008;Scalzo et al 2012), Type Iax & "calcium-rich" Ia Kasliwal et al 2012;Perets et al 2010), Type Ib/Ic (Drout et al 2011;Valenti et al 2008;Campana et al 2006;Taubenberger et al 2006;Bersten et al 2012;Cobb et al 2010;Valenti et al 2012), Type IIP/IIL Hamuy 2003;Andrews et al 2011;Botticella et al 2009), Type IIn (Kiewe et al 2012;Margutti et al 2014), Type I SLSNe (Quimby et al 2011;Chomiuk et al 2011;Lunnan et al 2013), and other rapidly evolving events (red; Drout et al 2013;Kasliwal et al 2010;Poznanski et al 2010;Ofek et al 2010;Matheson et al 2000). (A color version of this figure is available in the online journal.)…”

Section: Colors and Sedsmentioning

confidence: 99%

Rapidly Evolving and Luminous Transients From Pan-Starrs1

Drout

Chornock

Söderberg

et al. 2014

ApJ

326

444

View full text Add to dashboard Cite

In the past decade, several rapidly evolving transients have been discovered whose timescales and luminosities are not easily explained by traditional supernovae (SNe) models. The sample size of these objects has remained small due, at least in part, to the challenges of detecting short timescale transients with traditional survey cadences. Here we present the results from a search within the Pan-STARRS1 Medium Deep Survey (PS1-MDS) for rapidly evolving and luminous transients. We identify 10 new transients with a time above half-maximum (t 1/2 ) of less than 12 days and −16.5 > M > −20 mag. This increases the number of known events in this region of SN phase space by roughly a factor of three. The median redshift of the PS1-MDS sample is z = 0.275 and they all exploded in star-forming galaxies. In general, the transients possess faster rise than decline timescale and blue colors at maximum light (g P1 − r P1 −0.2). Best-fit blackbodies reveal photospheric temperatures/radii that expand/cool with time and explosion spectra taken near maximum light are dominated by a blue continuum, consistent with a hot, optically thick, ejecta. We find it difficult to reconcile the short timescale, high peak luminosity (L > 10 43 erg s −1 ), and lack of UV line blanketing observed in many of these transients with an explosion powered mainly by the radioactive decay of 56 Ni. Rather, we find that many are consistent with either (1) cooling envelope emission from the explosion of a star with a low-mass extended envelope that ejected very little (<0.03 M ) radioactive material, or (2) a shock breakout within a dense, optically thick, wind surrounding the progenitor star. After calculating the detection efficiency for objects with rapid timescales in the PS1-MDS we find a volumetric rate of 4800-8000 events yr −1 Gpc −3 (4%-7% of the core-collapse SN rate at z = 0.2).

show abstract

“…Most SNe Ib/c and Ic-BL also tend to decay faster than SLSNe, although there are a few exceptions of slow-decaying, long-lived SNe Ib/c (e.g., PTF 11bov, also known as SN 2011bm; Valenti et al 2012).…”

Section: Rise and Decay Timesmentioning

confidence: 99%

Light Curves of Hydrogen-poor Superluminous Supernovae from the Palomar Transient Factory

Gal‐Yam

Rubin

et al. 2018

ApJ

139

126

View full text Add to dashboard Cite

We investigate the light-curve properties of a sample of 26 spectroscopically confirmed hydrogen-poor superluminous supernovae (SLSNe-I) in the Palomar Transient Factory survey. These events are brighter than SNe Ib/c and SNe Ic-BL, on average, by about 4 and 2mag, respectively. The peak absolute magnitudes of SLSNe-I in rest-frame g band span −22M g −20 mag, and these peaks are not powered by radioactive 56 Ni, unless strong asymmetries are at play. The rise timescales are longer for SLSNe than for normal SNe Ib/c, by roughly 10 days, for events with similar decay times. Thus, SLSNe-I can be considered as a separate population based on photometric properties. After peak, SLSNe-I decay with a wide range of slopes, with no obvious gap between rapidly declining and slowly declining events. The latter events show more irregularities (bumps) in the light curves at all times. At late times, the SLSN-I light curves slow down and cluster around the 56 Co radioactive decay rate. Powering the late-time light curves with radioactive decay would require between 1 and 10 M e of Ni masses. Alternatively, a simple magnetar model can reasonably fit the majority of SLSNe-I light curves, with four exceptions, and can mimic the radioactive decay of 56 Co, up to ∼400 days from explosion. The resulting spin values do not correlate with the host-galaxy metallicities. Finally, the analysis of our sample cannot strengthen the case for using SLSNe-I for cosmology.

show abstract

A SPECTROSCOPICALLY NORMAL TYPE Ic SUPERNOVA FROM A VERY MASSIVE PROGENITOR

Cited by 81 publications

References 47 publications

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

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

Rapidly Evolving and Luminous Transients From Pan-Starrs1

Light Curves of Hydrogen-poor Superluminous Supernovae from the Palomar Transient Factory

Contact Info

Product

Resources

About