SN 2004aw: confirming diversity of Type Ic supernovae

Taubenberger, S.; Pastorello, A.; Mazzali, P. A.; Valenti, S.; Pignata, G.; Sauer, Daniel; Arbey, Alexandre; Bärnbantner, O.; Benetti, S.; Valle, Antonio della; Deng, J. S.; Elias‐Rosa, N.; Filippenko, A. V.; Foley, R. J.; Goobar, A.; Kotak, R.; Li, W.; Meikle, P.; Méndez, J.; Patat, F.; Pian, E.; Ries, C.; Ruiz‐Lapuente, P.; Salvo, M.; Stanishev, V.; Turatto, M.; Hillebrandt, W.

doi:10.1111/j.1365-2966.2006.10776.x

Cited by 170 publications

(198 citation statements)

References 71 publications

(130 reference statements)

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“…This suggests that SNe Ic as a group span a range of peak luminosities and cannot be compartmentalised into two broad groups according only to their luminosities. Taubenberger et al (2006) compare the photometric and spectroscopic evolutions of SNe 1994I and 1997ef to illustrate that the decline rate of the light curves of SNe Ic may be related to the speed of spectral evolution, with a slower decline rate in the light curve related to a slower spectroscopic evolution (related to the photon diffusion time). SN 1990B (Clocchiatti et al 2001) presented a case clearly contrary to this line of thought with a slow decline in light curve evolution but a fast spectroscopic evolution.…”

Section: Confirming the Heterogeneity Of Sne Icmentioning

confidence: 99%

“…11). In the spectra of SNe Ic the absorption feature associated with Na ID (Valenti et al 2008a;Mazzali et al 2005) and SN 2004aw with E(B − V) = 0.37 (Taubenberger et al 2006). All spectra are shown in the rest-frame of the SN and are placed in order of increasing photospheric velocity from top to bottom.…”

Section: Spectroscopic Observations and Data Reductionmentioning

confidence: 99%

“…3). Comparison SNe Ic presented in this paper have been chosen to span this wide range of properties from the prototypical SN 1994I (Sauer et al 2006;Richmond et al 1996) to the very energetic SN 1998bw (Galama et al 1998;Patat et al 2001) and including intermediate SNe 2007gr (Valenti et al 2008b;Hunter et al 2009), 1997ef (Mazzali et al 2000Iwamoto et al 1998;Nakano et al 1997), 2002ap (Mazzali et al 2002Gal-Yam et al 2002;Foley et al 2003;Yoshii et al 2003;Hendry et al 2005), 2003jd (Valenti et al 2008a) and 2004aw (Taubenberger et al 2006). In both Figs.…”

Section: Light Curvesmentioning

confidence: 99%

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Two type Ic supernovae in low-metallicity, dwarf galaxies: diversity of explosions

Young¹,

Smartt²,

Valenti³

et al. 2010

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Aims. The aim of this paper is to discuss the nature of two type Ic supernovae SN 2007bg and SN 2007bi and their host galaxies. Both supernovae were discovered in wide-field, non-targeted surveys and are found to be associated with sub-luminous blue dwarf galaxies identified in SDSS images. Methods. We present BVRI photometry and optical spectroscopy of SN 2007bg and SN 2007bi and their host galaxies. Their lightcurves and spectra are compared to those of other type Ic SNe and analysis of these data provides estimates of the energetics, total ejected masses and synthesised mass of 56 Ni. Detection of the host galaxy emission lines allows for metallicity measurements. Results. Neither SNe 2007bg nor 2007bi were found in association with an observed GRB, but from estimates of the metallicities of their host-galaxies they are found to inhabit similar low-metallicity environments as GRB associated supernovae. The radio-bright SN 2007bg is hosted by an extremely sub-luminous galaxy of magnitude M B = −12.4 ± 0.6 mag and an estimated oxygen abundance of 12 + log(O/H) = 8.18 ± 0.17 (on the Pettini & Pagel 2004 scale). The early lightcurve evolution of SN 2007bg matches the fastpace decline of SN 1994I giving it one of the fastest post-maximum decline rates of all broad-lined type Ic supernovae known to date and, when combined with its high expansion velocities, a high kinetic energy to ejected mass ratio (E K /M ej ∼ 2.7). We also show that SN 2007bi is possibly the most luminous type Ic known, reaching a peak magnitude of M R ∼ −21.3 mag and displays a remarkably slow decline, following the radioactive decay rate of 56 Co to 56 Fe throughout the course of its observed lifetime. SN 2007bi also displays an extreme longevity in its spectral evolution and is still not fully nebular at approximately one year post-maximum brightness. From a simple model of the bolometric light curve of SN 2007bi we estimate a total ejected 56 Ni mass of M Ni = 3.5−4.5 M , the largest 56 Ni mass measured in the ejecta of a supernova to date. There are two models that could explain the high luminosity and large ejected 56 Ni mass. One is a pair-instability supernova (PISN) which has been predicted to occur for massive stars at low metallicities. We measure the host galaxy metallicity of SN 2007bi to be 12 + log(O/H) = 8.15 ± 0.15 (on the McGaugh 1991 scale) which is somewhat high to be consistent with the PISN model. An alternative is the core-collapse of a C+O star of 20−40 M which is the core of a star of originally 50−100 M .

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Section: Confirming the Heterogeneity Of Sne Icmentioning

confidence: 99%

Section: Spectroscopic Observations and Data Reductionmentioning

confidence: 99%

Section: Light Curvesmentioning

confidence: 99%

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Two type Ic supernovae in low-metallicity, dwarf galaxies: diversity of explosions

Young¹,

Smartt²,

Valenti³

et al. 2010

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“…The B − V colour of SN 2007gr is intermediate between these two objects, with strong similarity to SNe 1998bw and 2002ap. Uncertainties in the reddening estimates and possible contamination from nearby blue stars preclude a further discussion of the bluer colours of SN 1994I (Taubenberger et al 2006). …”

Section: Colour Evolution Of Sn 2007grmentioning

confidence: 99%

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

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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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“…Well observed SNe Ic include, among others, SN 1994I (Filippenko et al 1995), SN 2004aw (Taubenberger et al 2006) and SN 2007gr (Valenti et al 2008a). Drout et al (2011) present a first multi-band sample of SNe Ic, Taddia et al (2015a) present the sample of SNe Ic from SDSS and Bianco et al (2014) and Modjaz et al (2014) present the light curves and the spectra of 64/73 SE SNe obtained at the Harvard-Smithsonian Center for Astrophysics (CfA).…”

Section: Introductionmentioning

confidence: 99%

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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SN 2004aw: confirming diversity of Type Ic supernovae

Cited by 170 publications

References 71 publications

Two type Ic supernovae in low-metallicity, dwarf galaxies: diversity of explosions

Two type Ic supernovae in low-metallicity, dwarf galaxies: diversity of explosions

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

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

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