Early Spectroscopic Identification of Sn 2008d

Malesani, D.; Fynbo, J. P. U.; Hjorth, J.; Leloudas, G.; Sollerman, J.; Stritzinger, M. D.; Vreeswijk, P. M.; Watson, Derrick G.; Gorosabel, J.; Michałowski, M. J.; Thöne, C. C.; Augusteijn, T.; Bersier, D.; Jakobsson, P.; Jaunsen, A. O.; Ledoux, C.; Levan, A. J.; Milvang-Jensen, B.; Rol, E.; Tanvir, N. R.; Wiersema, K.; Xu, D.; Li, Albert; Bayliss, M.; Gall, C.; Grove, L. F.; Koester, Benjamin P.; Leitet, E.; Pursimo, T.; Skillen, I.

doi:10.1088/0004-637x/692/2/l84

Cited by 74 publications

(102 citation statements)

References 41 publications

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“…This seems consistent with the identification of intermediate cases such as SN 1999ex which was characterised by weak optical He I lines, and strong He I λλ 10830, 20581 lines in the near-IR (Hamuy et al 2002). Additionally, the transitional nature of SNe such as SN 2005bf (Folatelli et al 2006) and SN 2008D (Soderberg et al 2008;Mazzali et al 2008;Malesani et al 2009), both of which underwent a metamorphosis from a type Ic at early times to a type Ib at later epochs, may also provide an insight into the controversy of He. The current challenge lies in linking the observed variations of type Ib/c SNe to the physical properties of their progenitor systems.…”

Section: Introductionsupporting

confidence: 87%

Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415

Hunter

Valenti

Kotak

et al. 2009

A&A

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We present photometric and spectroscopic observations at optical and near-infrared wavelengths of the nearby type Ic supernova 2007gr. These represent the most extensive data-set to date of any supernova of this sub-type, with frequent coverage from shortly after discovery to more than one year post-explosion. We deduce a rise time to B-band maximum of 11.5 ± 2.7 d. We find a peak B-band magnitude of M B = −16.8, and light curves which are remarkably similar to the so-called "hypernova" SN 2002ap. In contrast, the spectra of SNe 2007gr and 2002ap show marked differences, not least in their respective expansion velocities. We attribute these differences primarily to the density profiles of their progenitor stars at the time of explosion i.e. a more compact star for SN 2007gr compared to SN 2002ap. From the quasi-bolometric light curve of SN 2007gr, we estimate that 0.076 ± 0.010 M of 56 Ni was produced in the explosion. Our near-infrared (IR) spectra clearly show the onset and disappearance of the first overtone of carbon monoxide (CO) between ∼70 to 175 d relative to B-band maximum. The detection of the CO molecule implies that ionised He was not microscopically mixed within the carbon/oxygen layers. From the optical spectra, near-IR light curves, and colour evolution, we find no evidence for dust condensation in the ejecta out to about +400 d. Given the combination of unprecedented temporal coverage, and high signal-to-noise data, we suggest that SN 2007gr could be used as a template object for supernovae of this sub-class.

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Section: Introductionsupporting

confidence: 87%

Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415

Hunter

Valenti

Kotak

et al. 2009

A&A

124

100

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“…Hereafter t exp denotes the epoch in observer's frame measured from the explosion date, MJD = 54474.56 (Malesani et al 2009;Modjaz et al 2009). …”

Section: Spectroscopymentioning

confidence: 99%

NEBULAR PHASE OBSERVATIONS OF THE TYPE Ib SUPERNOVA 2008D/X-RAY TRANSIENT 080109: SIDE-VIEWED BIPOLAR EXPLOSION

Tanaka

Yamanaka

Maeda

et al. 2009

ApJ

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We present optical spectroscopic and photometric observations of supernova (SN) 2008D, associated with the luminous X-ray transient 080109, at >300 days after the explosion (nebular phases). We also give flux measurements of emission lines from the H ii region at the site of the SN, and estimates of the local metallicity. The brightness of the SN at nebular phases is consistent with the prediction of the explosion models with an ejected 56

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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: 98%

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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Early Spectroscopic Identification of Sn 2008d

Cited by 74 publications

References 41 publications

Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415

Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415

NEBULAR PHASE OBSERVATIONS OF THE TYPE Ib SUPERNOVA 2008D/X-RAY TRANSIENT 080109: SIDE-VIEWED BIPOLAR EXPLOSION

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

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