The Type I[CLC]c[/CLC] Hypernova SN 2002[CLC]ap[/CLC]

Mazzali, P. A.; Deng, J.; Maeda, Keiichi; Nomoto, Ken’ichi; Umeda, Hideyuki; Hatano, K.; Iwamoto, K.; Yoshii, Yuzuru; Kobayashi, Yukiyasu; Minezaki, Takeo; Doi, Mamoru; Enya, Keigo; Tomita, Hiroyuki; Smartt, S. J.; Kinugasa, K.; Kawakita, Hideyo; Ayani, K.; Kawabata, Tetsuya; Yamaoka, H.; Qiu, Y.; Motohara, Kentaro; Gerardy, C.; Fesen, Robert A.; Kawabata, Koji S.; Iye, Masanori; Kashikawa, Nobunari; Kosugi, George; Ohyama, Youichi; Takada-Hidai, Masahide; Zhao, Gang; Chornock, R.; Filippenko, A. V.; Benetti, S.; Turatto, M.

doi:10.1086/341504

Cited by 273 publications

(205 citation statements)

References 26 publications

(15 reference statements)

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“…For comparison, lines showing expansion with apparent speeds of 0.1 and 1.0 c area also plotted. (Mazzali et al 2002) and 2003jd (Mazzali et al 2005) were both suggested to possibly harbor off-axis GRB jets due to their spectral resemblance to GRB-SNe (e.g., SNe 1998bw, 2003dh, and 2003lw). In neither case, however, was the expected latetime radio emission seen up to an age of ∼2 years (Soderberg et al 2006).…”

Section: Discussionmentioning

confidence: 99%

Very-Long-Baseline Interferometry Observations of Sn 2008d

Bietenholz

Söderberg

Bartel

2009

ApJ

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We report on two epochs of very-long-baseline interferometry (VLBI) observations of the Type Ib/c supernova, SN 2008D, which was associated with the X-ray outburst XRF 080109. At our first epoch, at t = 30 days after the explosion, we observed at 22 and 8.4 GHz, and at our second, at t = 133 days, at 8.4 and 5.0 GHz. The VLBI observations allow us to accurately measure the source's size and position at each epoch, and thus constrain its expansion velocity and proper motion. We find the source at best marginally resolved at both epochs, allowing us to place a 3σ upper limit of ∼ 0.75 c on the expansion velocity of a circular source. For an elongated source, our measurements are compatible with mildly relativistic expansion. However, our 3σ upper limit on the proper motion is 4 μas day −1 , corresponding to an apparent velocity of less than 0.6 c, and is consistent with a stationary flux centroid. This limit rules out a relativistic jet such as a gamma-ray burst jet away from the line of sight, which would be expected to show apparent proper motion of greater than c. Taken together, our measurements argue against the presence of any long-lived relativistic outflow in SN 2008D. On the other hand, our measurements are consistent with the nonrelativistic expansion velocities of less than 30,000 km s −1 and small proper motions (< 500 km s −1 ) seen in typical supernovae.

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Section: Discussionmentioning

confidence: 99%

Very-Long-Baseline Interferometry Observations of Sn 2008d

Bietenholz

Söderberg

Bartel

2009

ApJ

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“…Specific cases include Type Ic supernovae SN 1997ef, 1997dq and SN 2002ap (Mazzali et al, 2002;Yoshii et al, 2003). All show evidence for peculiarity and high energy.…”

Section: Unusual Supernovae and Transition Objectsmentioning

confidence: 99%

The Supernova Gamma-Ray Burst Connection

Woosley

Bloom

2006

AIP Conference Proceedings

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ABSTRACT:Observations show that at least some gamma-ray bursts (GRBs) happen simultaneously with core-collapse supernovae (SNe), thus linking by a common thread nature's two grandest explosions. We review here the growing evidence for and theoretical implications of this association, and conclude that most long-duration soft-spectrum GRBs are accompanied by massive stellar explosions (GRB-SNe). The kinetic energy and luminosity of well-studied GRBSNe appear to be greater than those of ordinary SNe, but evidence exists, even in a limited sample, for considerable diversity. The existing sample also suggests that most of the energy in the explosion is contained in nonrelativistic ejecta (producing the supernova) rather than in the relativistic jets responsible for making the burst and its afterglow.

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“…2). Its rapid photometric evolution is very similar to that of a dimmer, non-GRB SN 2002ap, 35 but it is somewhat faster. Although its spectrum is characterized by broader absorption lines as in SN 1998bw and other GRB/SN, they are not as broad as those of SN 1998bw, and it is much more similar to that of SN 2002ap (Fig.…”

Section: Xrf-supernovaementioning

confidence: 80%

First stars, hypernovae, and superluminous supernovae

Nomoto

2017

The Fourteenth Marcel Grossmann Meeting

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After the big bang, production of heavy elements in the early universe takes place starting from the formation of the first (Pop III) stars, their evolution, and explosion. The Pop III supernova (SN) explosions have strong dynamical, thermal, and chemical feedback on the formation of subsequent stars and evolution of galaxies. However, the nature of Pop III stars/supernovae (SNe) have not been well-understood. The signature of nucleosynthesis yields of the first SN can be seen in the elemental abundance patterns observed in extremely metal-poor (EMP) stars. We show that the abundance patterns of EMP stars, e.g. the excess of C, Co, Zn relative to Fe, are in better agreement with the yields of hyper-energetic explosions (Hypernovae, (HNe)) rather than normal supernovae. We note the large variation of the abundance patterns of EMP stars propose that such a variation is related to the diversity of the GRB-SNe and posssibly superluminous supernovae (SLSNe). For example, the carbon-enhanced metal-poor (CEMP) stars may be related to the faint SNe (or dark HNe), which could be the explosions induced by relativistic jets. Finally, we examine the various mechanisms of SLSNe.

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The Type I[CLC]c[/CLC] Hypernova SN 2002[CLC]ap[/CLC]

Cited by 273 publications

References 26 publications

Very-Long-Baseline Interferometry Observations of Sn 2008d

Very-Long-Baseline Interferometry Observations of Sn 2008d

The Supernova Gamma-Ray Burst Connection

First stars, hypernovae, and superluminous supernovae

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