THE EXCEPTIONALLY LUMINOUS TYPE II-LINEAR SUPERNOVA 2008es

Miller, A. A.; Chornock, R.; Perley, D. A.; Ganeshalingam, M.; Li, W.; Butler, N.; Bloom, J.; Smith, Nathan; Modjaz, M.; Poznanski, D.; Filippenko, A. V.; Griffith, C.; Shiode, J.; Silverman, J. M.

doi:10.1088/0004-637x/690/2/1303

Cited by 155 publications

(244 citation statements)

References 49 publications

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“…One possibility is that some of the SNe discovered may be brighter than SN Ia. There is increasing evidence for such rare types of bright SNe (Miller et al 2009). An example of such an event is 2006gy, that had a peak luminosity of M R ∼ −22 (Smith et al 2007).…”

Section: Supernovae With Faint Galaxy Hosts?mentioning

confidence: 99%

First Results From the Catalina Real-Time Transient Survey

Drake¹,

Djorgovski²,

Mahabal³

et al. 2009

ApJ

1,275

1,131

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We report on the results from the first six months of the Catalina Real-Time Transient Survey (CRTS). In order to search for optical transients (OTs) with timescales of minutes to years, the CRTS analyses data from the Catalina Sky Survey which repeatedly covers 26,000 of square degrees on the sky. The CRTS provides a public stream of transients that are bright enough to be followed up using small telescopes. Since the beginning of the survey, all CRTS transients have been made available to astronomers around the world in real time using HTML tables,RSS feeds, and VOEvents. As part of our public outreach program, the detections are now also available in Keyhole Markup Language through Google Sky. The initial discoveries include over 350 unique OTs rising more than 2 mag from past measurements. Sixty two of these are classified as supernovae (SNe), based on light curves, prior deep imaging and spectroscopic data. Seventy seven are due to cataclysmic variables (CVs; only 13 previously known), while an additional 100 transients were too infrequently sampled to distinguish between faint CVs and SNe. The remaining OTs include active galactic nucleus, blazars, high-proper-motions stars, highly variable stars (such as UV Ceti stars), and transients of an unknown nature. Our results suggest that there is a large population of SNe missed by many current SN surveys because of selection biases. These objects appear to be associated with faint host galaxies. We also discuss the unexpected discovery of white dwarf binary systems through dramatic eclipses.

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Section: Supernovae With Faint Galaxy Hosts?mentioning

confidence: 99%

First Results From the Catalina Real-Time Transient Survey

Drake¹,

Djorgovski²,

Mahabal³

et al. 2009

ApJ

1,275

1,131

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“…This scenario has been invoked to explain the overluminous type IIL SN 2008es (Gezari et al 2009;Miller et al 2009a).…”

Section: Sn 2007bi: Pair-instability or Massive Core Collapse?mentioning

confidence: 99%

“…the overluminous SNe 2005ap (Quimby et al 2007b) and 2008es (Gezari et al 2009;Miller et al 2009a). Here we report on the followup of two such objects discovered by non-targeted SN surveys, both hosted by low-luminosity, dwarf galaxies: Harutyunyan et al (2007) confirm the resemblance to other SNe Ic-BL.…”

Section: Introductionmentioning

confidence: 99%

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

Young¹,

Smartt²,

Valenti³

et al. 2010

A&A

137

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 majority of H-rich SLSNe (often dubbed SLSN-II) show narrow Balmer lines similar to SNe IIn and are likely powered by interaction with a dense circumstellar medium (CSM; e.g., Ofek et al 2007; Smith et al 2007Smith et al , 2010Chatzopoulos et al 2011;Drake et al 2011;Rest et al 2011). However, there are also examples of SLSN-II without clear spectroscopic interaction signatures (Gezari et al 2009;Miller et al 2009;Inserra et al 2016) as well as objects classified as SLSN-I based on their peak spectra but show hydrogen features at late times (Yan et al 2015(Yan et al , 2017a.…”

Section: Introductionmentioning

confidence: 99%

Hydrogen-poor Superluminous Supernovae from the Pan-STARRS1 Medium Deep Survey

Lunnan

Chornock

Berger

et al. 2018

ApJ

Self Cite

111

103

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe present light curves and classification spectra of 17 hydrogen-poor superluminous supernovae (SLSNe) from the Pan-STARRS1 Medium Deep Survey (PS1 MDS). Our sample contains all objects from the PS1MDS sample with spectroscopic classification that are similar to either of the prototypes SN 2005ap or SN 2007bi, without an explicit limit on luminosity. With a redshift range z 0.3 1.6 < < , PS1MDS is the first SLSN sample primarily probing the high-redshift population; our multifilter PS1 light curves probe the rest-frame UV emission, and hence the peak of the spectral energy distribution. We measure the temperature evolution and construct bolometric light curves, and find peak luminosities of 0.5 5 10 44 ( -) ergs −1 and lower limits on the total radiated energies of 0.3 2 10 51 ( -) erg. The light curve shapes are diverse, with both rise and decline times spanning a factor of ∼5 and several examples of double-peaked light curves. When correcting for the flux-limited nature of our survey, we find a median peak luminosity at 4000Å of M 21.1 mag 4000 = -and a spread of 0.7 mag s = .

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THE EXCEPTIONALLY LUMINOUS TYPE II-LINEAR SUPERNOVA 2008es

Cited by 155 publications

References 49 publications

First Results From the Catalina Real-Time Transient Survey

First Results From the Catalina Real-Time Transient Survey

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

Hydrogen-poor Superluminous Supernovae from the Pan-STARRS1 Medium Deep Survey

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