ULTRA-BRIGHT OPTICAL TRANSIENTS ARE LINKED WITH TYPE Ic SUPERNOVAE

Pastorello, A.; Smartt, S. J.; Botticella, M. T.; Maguire, K.; Fraser, M.; Smith, Kenneth; Kotak, R.; Magill, L.; Valenti, S.; Young, D. R.; Gezari, Suvi; Bresolin, Fabio; Kudritzki, Rolf‐Peter; Howell, D. A.; Rest, A.; Metcalfe, N.; Mattila, S.; Kankare, E.; Huang, K. Y.; Urata, Y.; Burgett, W. S.; Chambers, K.; Dombeck, T.; Flewelling, H.; Grav, T.; Heasley, J. N.; Hodapp, Klaus W.; Kaiser, Nick; Luppino, Gerard A.; Lupton, R.; Magnier, E. A.; Monet, D. G.; Morgan, J. S.; Onaka, Peter M.; Price, P. A.; Rhoads, P. H.; Siegmund, Walter A.; Stubbs, C. W.; Sweeney, William E.; Tonry, J.; Wainscoat, R. J.; Waterson, M.; Waters, C.; Wynn‐Williams, C. G.

doi:10.1088/2041-8205/724/1/l16

Cited by 239 publications

(283 citation statements)

References 49 publications

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“…Various explanations have been considered by, e.g., Gänsicke et al (2009), Soker et al (2010, and Chatzopoulos et al (2009). It appears that SCP 06F6 may be a rare type of SN, with redshift z = 1.189 (Quimby et al 2009;Pastorello et al 2010). While its precise explanation is still uncertain, the important fact for this analysis is that SCP 06F6 is clearly not an SN Ia.…”

Section: Supernovaementioning

confidence: 79%

THEHUBBLE SPACE TELESCOPECLUSTER SUPERNOVA SURVEY. II. THE TYPE Ia SUPERNOVA RATE IN HIGH-REDSHIFT GALAXY CLUSTERS

Barbary

Aldering

Amanullah³

et al. 2011

ApJ

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We report a measurement of the Type Ia supernova (SN Ia) rate in galaxy clusters at 0.9 < z < 1.46 from the Hubble Space Telescope Cluster Supernova Survey. This is the first cluster SN Ia rate measurement with detected z > 0.9 SNe. Finding 8 ± 1 cluster SNe Ia, we determine an SN Ia rate of 0.50 ). This represents a factor of ≈5 ± 2 increase over measurements of the cluster rate at z < 0.2. We parameterize the late-time SN Ia delay time distribution (DTD) with a power law: Ψ(t) ∝ t s . Under the approximation of a single-burst cluster formation redshift of z f = 3, our rate measurement in combination with lower-redshift cluster SN Ia rates constrains s = −1.41 +0.47 −0.40 , consistent with measurements of the DTD in the field. This measurement is generally consistent with expectations for the "double degenerate" scenario and inconsistent with some models for the "single degenerate" scenario predicting a steeper DTD at large delay times. We check for environmental dependence and the influence of younger stellar populations by calculating the rate specifically in cluster red-sequence galaxies and in morphologically early-type galaxies, finding results similar to the full cluster rate. Finally, the upper limit of one hostless cluster SN Ia detected in the survey implies that the fraction of stars in the intra-cluster medium is less than 0.47 (95% confidence), consistent with measurements at lower redshifts.

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Section: Supernovaementioning

confidence: 79%

THEHUBBLE SPACE TELESCOPECLUSTER SUPERNOVA SURVEY. II. THE TYPE Ia SUPERNOVA RATE IN HIGH-REDSHIFT GALAXY CLUSTERS

Barbary

Aldering

Amanullah³

et al. 2011

ApJ

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“…Many supernovae with peculiar new properties, such as ultra bright SNe, have been 4 http://pan-starrs.ifa.hawaii.edu/public/home.html already found (e.g. Quimby et al 2007;Gezari et al 2009;Pastorello et al 2010;Chomiuk et al 2011). We expect that the untargeted surveys to produce an even larger richness in the SN variety that, in turn, will push for new explosion mechanism models.…”

Section: Modern and Future Sn Searchesmentioning

confidence: 98%

“…Different types of extremely luminous CC SNe have been recently discovered in dwarf, faint host galaxies Quimby et al 2007;Pastorello et al 2010) with an enormous luminosity at maximum that can not be powered by radioactive 56 Ni. Several scenarios have been proposed to explain these events: an explosion driven by black hole accretion (Utrobin et al 2010), the spin down of a rapidly rotating young magnetar (Kasen and Bildsten 2010;Woosley 2010), interaction of the SN ejecta with a dense CSM (Blinnikov and Sorokina 2010;Chevalier and Irwin 2011) or pulsational pair instability in which collisions between high velocity shells are the source of multiple, bright optical transients (Woosley et al 2007).…”

Section: Snementioning

confidence: 99%

Supernovae and Gaia

Altavilla

Botticella²,

Turatto³

2012

Astrophys Space Sci

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Despite decades of dedicated efforts there are still basic questions to answer with regard to Supernova progenitor systems and explosion mechanisms. In particular, in the last years a number of exceptionally bright objects and extremely faint events have demonstrated an unexpected large Supernova variety.The large number of Supernovae candidates at different redshifts provided by the next generation surveys, from ground and space, will allow to reach a better insight of the Supernova events in all their flavours. In particular it will be the possible to assess the systematics of type Ia Supernovae as distance indicator at any redshift.The Gaia astrometric mission is expected to discover a huge number of transient events, including Supernovae, which will be immediately disseminated to the astronomical community by a transients alert system for a suitable follow up.

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“…If the optical depth at R w is c/v s , then the SN light curve will have a slow decay (e.g., SN 2006gy; Ofek et al 2007;Smith et al 2007). If the optical depth at R w is c/v s , then it will have a faster decay (e.g., SN 2010gx; Pastorello et al 2010a;Quimby et al 2011b). Moriya & Tominaga (2012) investigated shock breakouts in general wind-density profiles of the form ρ ∝ r −w .…”

Section: Introductionmentioning

confidence: 99%

X-Ray Emission From Supernovae in Dense Circumstellar Matter Environments: A Search for Collisionless Shocks

Ofek

Fox

Cenko

et al. 2013

ApJ

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The optical light curve of some supernovae (SNe) may be powered by the outward diffusion of the energy deposited by the explosion shock (the so-called shock breakout) in optically thick (τ 30) circumstellar matter (CSM). Recently, it was shown that the radiation-mediated and radiation-dominated shock in an optically thick wind must transform into a collisionless shock and can produce hard X-rays. The X-rays are expected to peak at late times, relative to maximum visible light. Here we report on a search, using Swift/XRT and Chandra, for X-ray emission from 28 SNe that belong to classes whose progenitors are suspected to be embedded in dense CSM. Our sample includes 19 Type IIn SNe, one Type Ibn SN, and eight hydrogen-poor superluminous SNe (SLSN-I such as SN 2005ap). Two SNe (SN 2006jc and SN 2010jl) have X-ray properties that are roughly consistent with the expectation for X-rays from a collisionless shock in optically thick CSM. However, the X-ray emission from SN 2006jc can also be explained as originating in an optically thin region. Thus, we propose that the optical light curve of SN 2010jl is powered by shock breakout in CSM. We suggest that two other events (SN 2010al and SN 2011ht) were too X-ray bright during the SN maximum optical light to be explained by the shock-breakout model. We conclude that the light curves of some, but not all, SNe IIn/Ibn are powered by shock breakout in CSM. For the rest of the SNe in our sample, including all of the SLSN-I events, our X-ray limits are not deep enough and were typically obtained too early (i.e., near the SN maximum light) for definitive conclusions about their nature. Late-time X-ray observations are required in order to further test whether these SNe are indeed embedded in dense CSM. We review the conditions required for a shock breakout in a wind profile. We argue that the timescale, relative to maximum light, for the SN to peak in X-rays is a probe of the column density and the density profile above the shock region. In SNe whose X-ray emission slowly rises, and peaks at late times, the optical light curve is likely powered by the diffusion of shock energy in a dense CSM. We note that if the CSM density profile falls faster than a constant-rate wind-density profile, then X-rays may escape at earlier times than estimated for the wind-profile case. Furthermore, if the CSM has a region in which the density profile is very steep relative to a steady wind-density profile, or if the CSM is neutral, then the radio free-free absorption may be sufficiently low for radio emission to be detected.

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ULTRA-BRIGHT OPTICAL TRANSIENTS ARE LINKED WITH TYPE Ic SUPERNOVAE

Cited by 239 publications

References 49 publications

THEHUBBLE SPACE TELESCOPECLUSTER SUPERNOVA SURVEY. II. THE TYPE Ia SUPERNOVA RATE IN HIGH-REDSHIFT GALAXY CLUSTERS

THEHUBBLE SPACE TELESCOPECLUSTER SUPERNOVA SURVEY. II. THE TYPE Ia SUPERNOVA RATE IN HIGH-REDSHIFT GALAXY CLUSTERS

Supernovae and Gaia

X-Ray Emission From Supernovae in Dense Circumstellar Matter Environments: A Search for Collisionless Shocks

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