The Optical/Near‐Infrared Light Curves of SN 2002ap for the First 140 Days after Discovery

Yoshii, Yuzuru; Tomita, Hiroyuki; Kobayashi, Yukiyasu; Deng, J. S.; Maeda, Keiichi; Nomoto, Ken’ichi; Mazzali, P. A.; Umeda, Hideyuki; Aoki, Tsutomu; Doi, M.; Enya, Keigo; Minezaki, Takeo; Suganuma, Masahiro; Peterson, B. A.

doi:10.1086/375572

Cited by 72 publications

(83 citation statements)

References 29 publications

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“…Even stranger, the light curve was very different from any known SN ): a fairly rapid rise to a first peak was followed by a period of stalling or slow decline and by a new rise to a later, brighter peak at ∼ 40 days after explosion (Fig. 1) Modjaz et al 2005c) at FLWO, BV RI bands at the Himalayan Chandra Telescope (HCT; Anupama et al 2005), and BV RIJHK bands at the MAGNUM Telescope (Yoshii et al 2003;Inada et al 2005) (Fig. 1).…”

Section: Introductionmentioning

confidence: 94%

The Unique Type Ib Supernova 2005bf: A WN Star Explosion Model for Peculiar Light Curves and Spectra

Tominaga

Tanaka

Nomoto

et al. 2005

ApJ

105

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Observations and modeling for the light curve (LC) and spectra of supernova (SN) 2005bf are reported. This SN showed unique features: the LC had two maxima, and declined rapidly after the second maximum, while the spectra showed strengthening He lines whose velocity increased with time. The double-peaked LC can be reproduced by a double-peaked 56 Ni distribution, with most 56 Ni at low velocity and a small amount at high velocity. The rapid post-maximum decline requires a large fraction of the γ-rays to escape from the 56 Ni-dominated region, possibly because of low-density "holes". The presence of Balmer lines in the spectrum suggests that the He layer of the progenitor was substantially intact. Increasing γ-ray deposition in the He layer due to enhanced γ-ray escape from the 56 Ni-dominated region may explain both the delayed strengthening and the increasing velocity of the He lines. The SN has massive ejecta (∼ 6−7M ⊙ ), normal kinetic energy (∼ 1.0 − 1.5 × 10 51 ergs), high peak bolometric luminosity (∼ 5 × 10 42 erg s −1 ) for an epoch as late as ∼ 40 days, and a large 56 Ni mass (∼ 0.32M ⊙ ). These properties, and the presence of a small amount of H suggest that the progenitor was initially massive (M∼ 25 − 30M ⊙ ) and had lost most of its H envelope, and was possibly a WN star. The double-peaked 56 Ni distribution suggests that the explosion may have formed jets that did not reach the He layer. The properties of SN 2005bf resemble those of the explosion of Cassiopeia A.

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Section: Introductionmentioning

confidence: 94%

The Unique Type Ib Supernova 2005bf: A WN Star Explosion Model for Peculiar Light Curves and Spectra

Tominaga

Tanaka

Nomoto

et al. 2005

ApJ

105

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“…Being one of the nearest SNe in the last decades, SN 2002ap triggered an observational campaign since its discovery on 2002 January 29 (Gal-Yam et al 2002;Mazzali et al 2002;Foley et al 2003;Yoshii et al 2003;Tomita et al 2006). Thanks to its proximity, only 9.4 Mpc in distance, high quality observational data were acquired until 580 days after explosion, which is prerequisite for the identification of late excess over the exponential 56 Co decay.…”

Section: Data Preparation and Modelingmentioning

confidence: 99%

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Wang

Liu

et al. 2017

ApJ

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Broad-lined type Ic supernovae (SNe Ic-BL) are peculiar stellar explosions that distinguish themselves from ordinary SNe. Some SNe Ic-BL are associated with long-duration ( 2 s) gamma-ray bursts (GRBs). Black holes and magnetars are two types of compact objects that are hypothesized to be central engines of GRBs. In spite of decades of investigations, no direct evidence for the formation of black holes or magnetars has been found for GRBs so far. Here we report the finding that the early peak (t 50 days) and late-time (t 300 days) slow decay displayed in the light curves of both SNe 1998bw (associated with GRB 980425) and 2002ap (not GRB-associated) can be attributed to magnetar spin-down with initial rotation period P 0 ∼ 20 ms, while the intermediate-time (50 t 300 days) exponential decline is caused by radioactive decay of 56 Ni. The connection between the early peak and late-time slow decline in the light curves is unexpected in alternative models. We thus suggest that GRB 980425 and SN 2002ap were powered by magnetars.

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“…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%

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

Young¹,

Smartt²,

Valenti³

et al. 2010

A&A

139

132

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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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The Optical/Near‐Infrared Light Curves of SN 2002ap for the First 140 Days after Discovery

Cited by 72 publications

References 29 publications

The Unique Type Ib Supernova 2005bf: A WN Star Explosion Model for Peculiar Light Curves and Spectra

The Unique Type Ib Supernova 2005bf: A WN Star Explosion Model for Peculiar Light Curves and Spectra

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

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

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