STRONG EVOLUTION OF X-RAY ABSORPTION IN THE TYPE IIn SUPERNOVA SN 2010jl

Chandra, Poonam; Chevalier, Roger A.; Irwin, Christopher M.; Чугай, Н. Н.; Fransson, Claes; Söderberg, A. M.

doi:10.1088/2041-8205/750/1/l2

Cited by 52 publications

(67 citation statements)

References 17 publications

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“…The current null detection of hydrogen-poor luminous SNe in X-rays cannot be used to reject the CSM-interaction model proposed by Quimby et al (2011b). Chandra et al (2012b) reported on the discovery of X-ray emission from SN 2010jl. Its X-ray luminosity near optical 22 http://www.cbat.eps.harvard.edu/lists/Supernovae.html maximum light is about 6 × 10 40 erg s −1 , which is ∼10 −3…”

Section: Observations In Context Of the Modelmentioning

confidence: 84%

“…Moreover, Svirski et al (2012) assumed that the bound-free absorption can be neglected even at late times (i.e., the CSM is completely ionized). Chandra et al (2012b) reported on the analysis of the X-ray spectrum of SN 2010jl (including the proprietary data). They measured a column density at their latest epoch of ∼10 24 cm −2 , which is about 1000 times larger than the Galactic column density in the direction of SN 2010jl.…”

Section: Sn 2010jl (Ptf 10aaxf)mentioning

confidence: 99%

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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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Section: Observations In Context Of the Modelmentioning

confidence: 84%

Section: Sn 2010jl (Ptf 10aaxf)mentioning

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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“…In 2010, a bright type IIn supernova, SN 2010jl, was discovered in the western galaxy of UGC 5189 (Newton & Puckett 2010;Benetti et al 2010). The Chandra data of this supernovae was analyzed by Chandra et al (2012). In our analysis, the supernova is detected as a point source.…”

Section: Mrk 231 (Iras 12540+5708)mentioning

confidence: 99%

Diffuse X-Ray-emitting Gas in Major Mergers

Smith

Campbell

Struck

et al. 2018

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Using archived data from the Chandra X-ray telescope, we have extracted the diffuse Xray emission from 49 equal-mass interacting/merging galaxy pairs in a merger sequence, from widely separated pairs to merger remnants. After removal of contributions from unresolved point sources, we compared the diffuse thermal X-ray luminosity from hot gas (L X (gas)) with the global star formation rate (SFR). After correction for absorption within the target galaxy, we do not see strong trend of L X (gas)/SFR with SFR or merger stage for galaxies with SFR > 1 M ⊙ yr −1 . For these galaxies, the median L X (gas)/SFR is 5.5 × 10 39 ((erg s −1 )/M ⊙ yr −1 )), similar to that of normal spiral galaxies. These results suggest that stellar feedback in star forming galaxies reaches an approximately steady state condition, in which a relatively constant fraction of about 2% of the total energy output from supernovae and stellar winds is converted into X-ray flux. Three late-stage merger remnants with low SFRs and high K band luminosities (L K ) have enhanced L X (gas)/SFR; their UV/IR/optical colors suggest that they are post-starburst galaxies, perhaps in the process of becoming ellipticals. Systems with L K < 10 10 L ⊙ have lower L X (gas)/SFR ratios than the other galaxies in our sample, perhaps due to lower gravitational fields or lower metallicities. We see no relation between L X (gas)/SFR and Seyfert activity in this sample, suggesting that feedback from active galactic nuclei is not a major contributor to the hot gas in our sample galaxies.

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“…Ofek et al (2014b) combined visible and X-ray data to estimate the presence of > 10 M⊙ of CSM surrounding the progenitor of SN 2010jl. Because of its extreme brightness and relative proximity, SN 2010jl has been the focus of numerous further studies containing additional optical and X-ray observations (Roy et al 2011;Stoll et al 2011;Patat et al 2011;Andrews et al 2011;Smith et al 2012;Chandra et al 2012;Zhang et al 2012;Zoglauer et al 2013;Fransson et al 2013). The distance to UGC 5189A obtained from NED as described in §2.2 is 48.9 Mpc, consistent with the value adopted by Smith et al (2011b).…”

Section: Sn 2010jlmentioning

confidence: 99%

Constraints on Type IIn supernova progenitor outbursts from the Lick Observatory Supernova Search

Bilinski¹,

Smith²,

Li³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We searched through roughly 12 years of archival survey data acquired by the Katzman Automatic Imaging Telescope (KAIT) as part of the Lick Observatory Supernova Search (LOSS) in order to detect or place limits on possible progenitor outbursts of Type IIn supernovae (SNe IIn). The KAIT database contains multiple pre-SN images for 5 SNe IIn (plus one ambiguous case of a SN IIn/imposter) within 50 Mpc. No progenitor outbursts are found using the false discovery rate (FDR) statistical method in any of our targets. Instead, we derive limiting magnitudes (LMs) at the locations of the SNe. These limiting magnitudes (typically reaching m R ≈ 19.5 mag) are compared to outbursts of SN 2009ip and η Car, plus additional simulated outbursts. We find that the data for SN 1999el and SN 2003dv are of sufficient quality to rule out events ∼ 40 days before the main peak caused by initially faint SNe from blue supergiant (BSG) precursor stars, as in the cases of SN 2009ip and SN 2010mc. These SNe IIn may thus have arisen from red supergiant progenitors, or they may have had a more rapid onset of circumstellar matter interaction. We also estimate the probability of detecting at least one outburst in our dataset to be 60% for each type of the example outbursts, so the lack of any detections suggests that such outbursts are either typically less luminous (intrinsically or owing to dust) than ∼ −13 mag, or not very common among SNe IIn within a few years prior to explosion.

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STRONG EVOLUTION OF X-RAY ABSORPTION IN THE TYPE IIn SUPERNOVA SN 2010jl

Cited by 52 publications

References 17 publications

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

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

Diffuse X-Ray-emitting Gas in Major Mergers

Constraints on Type IIn supernova progenitor outbursts from the Lick Observatory Supernova Search

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