<i>Swift</i>
                    and
                    <i>Chandra</i>
                    Detections of Supernova 2006jc: Evidence for Interaction of the Supernova Shock with a Circumstellar Shell

Immler, S.; Modjaz, M.; Landsman, W. B.; Bufano, F.; Brown, P. J.; Milne, Peter; Dessart, Luc; Holland, S. T.; Koss, Michael; Pooley, David; Kirshner, R.; Filippenko, A. V.; Panagia, N.; Chevalier, Roger A.; Mazzali, P. A.; Gehrels, N.; Petre, Robert; Burrows, D. N.; Nousek, J. A.; Roming, P. W. A.; Pian, E.; Söderberg, A. M.; Greiner, J.

doi:10.1086/529373

Cited by 90 publications

(122 citation statements)

References 12 publications

(20 reference statements)

Supporting

Mentioning

115

Contrasting

Order By: Relevance

“…Whether the dust formed in the postshock gas, as convincingly proposed by Smith et al (2008), or in the ejecta can be assessed only through detailed modeling of all the spectral and photometric data available. A brightening of X-ray emission from $20 to $100 days after discovery has been interpreted by Immler et al (2008) as the result of the SN shock with a dense shell of material, consistent with that believed to be released by an outburst of the progenitor. The X-ray brightening occurred during the NIR rebrightening; hence, the interaction between ejecta and outer shell arose at the same epoch as dust formation.…”

Section: Discussionmentioning

confidence: 70%

Near‐Infrared Observations of the Type Ib Supernova SN 2006jc: Evidence of Interactions with Dust

Carlo

Corsi

Arkharov

et al. 2008

Astrophysical Journal

View full text Add to dashboard Cite

In the framework of a program for the monitoring of supernovae in the near-infrared (NIR) carried out by the Teramo, Rome, and Pulkovo observatories with the AZT-24 telescope, we observed the supernova SN 2006jc in the J, H, and K photometric bands during a period of 7 months, starting $36 days after its discovery. Our observations evidence a NIR rebrightening, peaking $70 days after discovery, along with a reddening of (H À K) and (J À H) colors until 120 days after discovery. After that date, (J À H) seems to evolve toward bluer colors. Our data, complemented with IR and optical observations found in the literature, show that the rebrightening is produced by hot, newly formed dust surrounding the supernova.

show abstract

Section: Discussionmentioning

confidence: 70%

Near‐Infrared Observations of the Type Ib Supernova SN 2006jc: Evidence of Interactions with Dust

Carlo

Corsi

Arkharov

et al. 2008

Astrophysical Journal

View full text Add to dashboard Cite

show abstract

“…SN 2006jc has a large number of Swift/XRT and Chandra observations. The SN is detected on multiple epochs and its X-ray light curve is presented in Figure 2 (see also Immler et al 2008). It was detected in X-rays soon after maximum optical light and reached a maximum X-ray luminosity of about 1.5×10 40 erg s…”

Section: Where N (E) Has Units Of Photons CMmentioning

confidence: 96%

“…However, X-rays can also be generated in optically thin environments. Following Immler et al (2008), the X-ray emission from an optically thin region is given by…”

Section: X-ray Emission From Collisionless Shocksmentioning

confidence: 99%

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

Ofek

Fox

Cenko

et al. 2013

ApJ

Self Cite

View full text Add to dashboard Cite

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.

show abstract

“…A precursor to the SN explosion has been identified in the H-stripped type-Ibn SN 2006jc, which showed signs of interaction with a He-rich medium (e.g., Foley et al 2007;Pastorello et al 2007;Immler et al 2008). Evidence for significantly enhanced mass loss timed with the explosion has been found for the H-poor progenitors of both type-IIb SNe (GalYam et al 2014;Kamble et al 2015;Maeda et al 2015) and type-Ib SNe (Svirski & Nakar 2014), as well as for the H-and He-poor progenitors of type-Ic SNe associated with some nearby gamma-ray bursts (Margutti et al 2015;Nakar 2015).…”

Section: Introductionmentioning

confidence: 99%

Ejection of the Massive Hydrogen-rich Envelope Timed with the Collapse of the Stripped SN 2014C

Margutti

Kamble

Milisavljevic

et al. 2017

ApJ

Self Cite

166

269

View full text Add to dashboard Cite

We present multi-wavelength observations of SN 2014C during the first 500 days. These observations represent the first solid detection of a young extragalactic stripped-envelope SN out to high-energy X-rays ∼40 keV. SN 2014C shows ordinary explosion parameters (E k ∼1.8×10 51 erg and M ej ∼1.7 M e ). However, over an ∼1 year timescale, SN 2014C evolved from an ordinary hydrogen-poor supernova into a strongly interacting, hydrogen-rich supernova, violating the traditional classification scheme of type-I versus type-II SNe. Signatures of the SN shock interaction with a dense medium are observed across the spectrum, from radio to hard X-rays, and revealed the presence of a massive shell of ∼1 M e of hydrogen-rich material at ∼6×10 16 cm. The shell was ejected by the progenitor star in the decades to centuries before collapse. This result challenges current theories of massive star evolution, as it requires a physical mechanism responsible for the ejection of the deepest hydrogen layer of H-poor SN progenitors synchronized with the onset of stellar collapse. Theoretical investigations point at binary interactions and/or instabilities during the last nuclear burning stages as potential triggers of the highly time-dependent mass loss. We constrain these scenarios utilizing the sample of 183 SNe Ib/c with public radio observations. Our analysis identifies SN 2014C-like signatures in ∼10% of SNe. This fraction is reasonably consistent with the expectation from the theory of recent envelope ejection due to binary evolution if the ejected material can survive in the close environment for 10 3 -10 4 years. Alternatively, nuclear burning instabilities extending to core C-burning might play a critical role.

show abstract

Swift and Chandra Detections of Supernova 2006jc: Evidence for Interaction of the Supernova Shock with a Circumstellar Shell

Cited by 90 publications

References 12 publications

Near‐Infrared Observations of the Type Ib Supernova SN 2006jc: Evidence of Interactions with Dust

Near‐Infrared Observations of the Type Ib Supernova SN 2006jc: Evidence of Interactions with Dust

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

Ejection of the Massive Hydrogen-rich Envelope Timed with the Collapse of the Stripped SN 2014C

Contact Info

Product

Resources

About