Optical and near-infrared observations of SN 2011dh – The first 100 days

Ergon, M.; Sollerman, J.; Fraser, M.; Pastorello, A.; Taubenberger, S.; Elias‐Rosa, N.; Bersten, Melina C.; Jerkstrand, A.; Benetti, S.; Botticella, M. T.; Fransson, Claes; Harutyunyan, A.; Kotak, R.; Smartt, S. J.; Valenti, S.; Bufano, F.; Cappellaro, E.; Fiaschi, M.; Howell, A.; Kankare, E.; Magill, L.; Mattila, S.; Maund, Justyn R.; Naves, R.; Ochner, P.; Ruíz, José Rafael; Smith, K.; Tomasella, L.; Turatto, M.

doi:10.1051/0004-6361/201321850

Cited by 111 publications

(139 citation statements)

References 87 publications

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“…Some SNe IIb show a distinct primary peak, but most do not (e.g. SN 2008ax, Pastorello et al 2008;Tsvetkov et al 2009Ergon et al 2014). As LSQ13cuw was discovered early, it is unlikely that a primary peak was missed.…”

Section: Photometrymentioning

confidence: 99%

“…Table B.1 lists the local sequence stars from the SDSS DR9 catalogue that were used to calibrate the LT and LCOGT g r i -band Ripero et al (1993); g) Corwin et al (1993); h) Centurion et al (1993); i) Hanzl et al (1993); j) Tweedy et al (1993); k) Dumont et al (1993); l) Pressberger et al (1993); m) Lewis et al (1994); n) Barbon et al (1995); o) Pastorello et al (2008); p) Tsvetkov et al (2009); q) Ergon et al (2014).…”

Section: A31 Radiusmentioning

confidence: 99%

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A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

Gáll

Polshaw

Kotak

et al. 2015

A&A

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We report on our findings based on the analysis of observations of the Type II-L supernova LSQ13cuw within the framework of currently accepted physical predictions of core-collapse supernova explosions. LSQ13cuw was discovered within a day of explosion, hitherto unprecedented for Type II-L supernovae. This motivated a comparative study of Type II-P and II-L supernovae with relatively well-constrained explosion epochs and rise times to maximum (optical) light. From our sample of twenty such events, we find evidence of a positive correlation between the duration of the rise and the peak brightness. On average, SNe II-L tend to have brighter peak magnitudes and longer rise times than SNe II-P. However, this difference is clearest only at the extreme ends of the rise time versus peak brightness relation. Using two different analytical models, we performed a parameter study to investigate the physical parameters that control the rise time behaviour. In general, the models qualitatively reproduce aspects of the observed trends. We find that the brightness of the optical peak increases for larger progenitor radii and explosion energies, and decreases for larger masses. The dependence of the rise time on mass and explosion energy is smaller than the dependence on the progenitor radius. We find no evidence that the progenitors of SNe II-L have significantly smaller radii than those of SNe II-P.

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Section: Photometrymentioning

confidence: 99%

Section: A31 Radiusmentioning

confidence: 99%

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

Gáll

Polshaw

Kotak

et al. 2015

A&A

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“…In Fig. 3 we also display the quasi-bolometric BVRI LC of the Type IIb SN 2011dh (Ergon et al 2014a), as well as a scaled and stretched quasi-bolometric BVRI LC of SN 1998bw (SN Ic-BL; Clocchiatti et al 2011). We find that the peak BVRI luminosity of iPTF13bvn is somewhat lower than that of SN 2011dh, indicating a slightly lower 56 Ni mass 7 .…”

Section: Light Curvesmentioning

confidence: 99%

The rise and fall of the Type Ib supernova iPTF13bvn

Fremling

Sollerman

Taddia

et al. 2014

A&A

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Context. We investigate iPTF13bvn, a core-collapse (CC) supernova (SN) in the nearby spiral galaxy NGC 5806. This object was discovered by the intermediate Palomar Transient Factory (iPTF) very close to the estimated explosion date and was classified as a stripped-envelope CC SN, likely of Type Ib. Furthermore, a possible progenitor detection in pre-explosion Hubble Space Telescope (HST) images was reported, making this the only SN Ib with such an identification. Based on the luminosity and color of the progenitor candidate, as well as on early-time spectra and photometry of the SN, it was argued that the progenitor candidate is consistent with a single, massive Wolf-Rayet (WR) star. Aims. We aim to confirm the progenitor detection, to robustly classify the SN using additional spectroscopy, and to investigate if our follow-up photometric and spectroscopic data on iPTF13bvn are consistent with a single-star WR progenitor scenario. Methods. We present a large set of observational data, consisting of multi-band light curves (UBVRI, g r i z ) and optical spectra. We perform standard spectral line analysis to track the evolution of the SN ejecta. We also construct a bolometric light curve and perform hydrodynamical calculations to model this light curve to constrain the synthesized radioactive nickel mass and the total ejecta mass of the SN. Late-time photometry is analyzed to constrain the amount of oxygen. Furthermore, image registration of pre-and postexplosion HST images is performed. Results. Our HST astrometry confirms the location of the progenitor candidate of iPTF13bvn, and follow-up spectra securely classify this as a SN Ib. We use our hydrodynamical model to fit the observed bolometric light curve, estimating the total ejecta mass to be 1.9 M and the radioactive nickel mass to be 0.05 M . The model fit requires the nickel synthesized in the explosion to be highly mixed out in the ejecta. We also find that the late-time nebular r -band luminosity is not consistent with predictions based on the expected oxygen nucleosynthesis in very massive stars. Conclusions. We find that our bolometric light curve of iPTF13bvn is not consistent with the previously proposed single massive WR-star progenitor scenario. The total ejecta mass and, in particular, the late-time oxygen emission are both significantly lower than what would be expected from a single WR progenitor with a main-sequence mass of at least 30 M .

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“…The detection of an early peak can bring important information on the radius of the progenitor star (Piro & Nakar 2013), but also on the outer structure of the star, the degree of 56 Ni mixing, as well as the presence of a companion or a dense circumstellar material (CSM). Some SE SNe, such as SN Ib 1999ex (Stritzinger et al 2002), SN Ib 2008D (Soderberg et al 2008Malesani et al 2009;Modjaz et al 2009), SN Ib/IIb iPTF13bvn (Fremling et al 2016), and many SNe IIb (e.g., SN 1993J, Richmond et al 1994SN 2011dh, Arcavi et al 2011Ergon et al 2014), do show this kind of early emission. The type Ib/c SN 2013ge showed an early peak but only in the ultra-violet (UV) light curves (Drout et al 2016).…”

Section: Introductionmentioning

confidence: 97%

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

Taddia

Fremling

Sollerman

et al. 2016

A&A

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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.

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Optical and near-infrared observations of SN 2011dh – The first 100 days

Cited by 111 publications

References 87 publications

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

The rise and fall of the Type Ib supernova iPTF13bvn

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

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