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

Ofek, E. O.; Fox, D. B.; Cenko, S. Bradley; Sullivan, M.; Gnat, Orly; Frail, D. A.; Horesh, A.; Corsi, A.; Quimby, R.; Gehrels, N.; Kulkarni, S. R.; Gal‐Yam, A.; Nugent, P.; Yaron, O.; Filippenko, A. V.; Kasliwal, M. M.; Bildsten, Lars; Bloom, J.; Poznanski, D.; Arcavi, I.; Laher, Russ R.; Sesar, Branimir; Surace, J.

doi:10.1088/0004-637x/763/1/42

Cited by 73 publications

(76 citation statements)

References 85 publications

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“…We exclude from our sample objects for which the spectra evolve into those of normal SNe II a few weeks after explosion. Examples for such objects include PTF 11iqb and PTF 10uls (Ofek et al 2013a). In total we rejected five such SNe from our sample.…”

Section: Samplementioning

confidence: 99%

PRECURSORS PRIOR TO TYPE IIn SUPERNOVA EXPLOSIONS ARE COMMON: PRECURSOR RATES, PROPERTIES, AND CORRELATIONS

Ofek

Sullivan

Shaviv

et al. 2014

ApJ

237

264

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There is a growing number of Type IIn supernovae (SNe) which present an outburst prior to their presumably final explosion. These precursors may affect the SN display, and are likely related to poorly charted phenomena in the final stages of stellar evolution. By coadding Palomar Transient Factory (PTF) images taken prior to the explosion, here we present a search for precursors in a sample of 16 Type IIn SNe. We find five SNe IIn that likely have at least one possible precursor event (PTF 10bjb, SN 2010mc, PTF 10weh, SN 2011ht, and PTF 12cxj), three of which are reported here for the first time. For each SN we calculate the control time. We find that precursor events among SNe IIn are common: at the one-sided 99% confidence level, >50% of SNe IIn have at least one pre-explosion outburst that is brighter than 3 × 10 7 L taking place up to 1/3 yr prior to the SN explosion. The average rate of such precursor events during the year prior to the SN explosion is likely 1 yr −1 , and fainter precursors are possibly even more common. Ignoring the two weakest precursors in our sample, the precursors rate we find is still on the order of one per year. We also find possible correlations between the integrated luminosity of the precursor and the SN total radiated energy, peak luminosity, and rise time. These correlations are expected if the precursors are mass-ejection events, and the early-time light curve of these SNe is powered by interaction of the SN shock and ejecta with optically thick circumstellar material.

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Section: Samplementioning

confidence: 99%

PRECURSORS PRIOR TO TYPE IIn SUPERNOVA EXPLOSIONS ARE COMMON: PRECURSOR RATES, PROPERTIES, AND CORRELATIONS

Ofek

Sullivan

Shaviv

et al. 2014

ApJ

237

264

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“…Radio and X-ray emission from superluminous SNe may arise from interaction with the circumstellar medium (CSM; see, e.g., Ofek et al 2013). In an alternate model, SLSNs could be powered by the spin-down of a nascent magnetar inside the supernova ejecta (Kasen & Bildsten 2010), which may also produce X-ray emission .…”

Section: Radio and X-ray Follow-upmentioning

confidence: 99%

“…In dense CSM environments, free-free absorption can suppress the radio emission at early times. Thus, chances for a detection are maximized by observing after maximum light (Ofek et al 2013). Hence, we observed iPTF15cyk thrice between 1 month and 4 months after discovery.…”

Section: Radio and X-ray Follow-upmentioning

confidence: 99%

iPTF SEARCH FOR AN OPTICAL COUNTERPART TO GRAVITATIONAL-WAVE TRANSIENT GW150914

Kasliwal

Cenko

Singer

et al. 2016

ApJL

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The intermediate Palomar Transient Factory (iPTF) autonomously responded to and promptly tiled the error region of the first gravitational-wave event GW150914 to search for an optical counterpart. Only a small fraction of the total localized region was immediately visible in the northern night sky, due both to Sun-angle and elevation constraints. Here, we report on the transient candidates identified and rapid follow-up undertaken to determine the nature of each candidate. Even in the small area imaged of 126 deg 2 , after extensive filtering, eight candidates were deemed worthy of additional follow-up. Within two hours, all eight were spectroscopically classified by the Keck II telescope. Curiously, even though such events are rare, one of our candidates was a superluminous supernova. We obtained radio data with the Jansky Very Large Array and X-ray follow-up with the Swift satellite for this transient. None of our candidates appear to be associated with the gravitational-wave trigger, which is unsurprising given that GW150914 came from the merger of two stellar-mass black holes. This end-to-end discovery and follow-up campaign bodes well for future searches in this post-detection era of gravitational waves.

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“…The first few objects showed a striking diversity, e.g., SN2005ap (Quimby et al 2007), SN2006gy (Ofek et al 2007;Smith et al 2007), and SN2007bi (Gal-Yam et al 2009), leading to a natural division between H-rich events (SLSNe-II) and H-poor events (SLSNe-I). Most SLSNe-II show narrow lines (SLSN-IIn) and are powered by the interaction of the SN ejecta with the circumstellar medium (CSM; e.g., Chevalier & Fransson 1994;Chugai & Danziger 1994;Chevalier & Irwin 2011;Ofek et al 2013;Inserra et al 2018). SLSNe-I are less well-understood, and the physical processes that dominate these explosions are still under debate.…”

Section: Introductionmentioning

confidence: 99%

Light Curves of Hydrogen-poor Superluminous Supernovae from the Palomar Transient Factory

Gal‐Yam

Rubin

et al. 2018

ApJ

Self Cite

133

126

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We investigate the light-curve properties of a sample of 26 spectroscopically confirmed hydrogen-poor superluminous supernovae (SLSNe-I) in the Palomar Transient Factory survey. These events are brighter than SNe Ib/c and SNe Ic-BL, on average, by about 4 and 2mag, respectively. The peak absolute magnitudes of SLSNe-I in rest-frame g band span −22M g −20 mag, and these peaks are not powered by radioactive 56 Ni, unless strong asymmetries are at play. The rise timescales are longer for SLSNe than for normal SNe Ib/c, by roughly 10 days, for events with similar decay times. Thus, SLSNe-I can be considered as a separate population based on photometric properties. After peak, SLSNe-I decay with a wide range of slopes, with no obvious gap between rapidly declining and slowly declining events. The latter events show more irregularities (bumps) in the light curves at all times. At late times, the SLSN-I light curves slow down and cluster around the 56 Co radioactive decay rate. Powering the late-time light curves with radioactive decay would require between 1 and 10 M e of Ni masses. Alternatively, a simple magnetar model can reasonably fit the majority of SLSNe-I light curves, with four exceptions, and can mimic the radioactive decay of 56 Co, up to ∼400 days from explosion. The resulting spin values do not correlate with the host-galaxy metallicities. Finally, the analysis of our sample cannot strengthen the case for using SLSNe-I for cosmology.

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

Cited by 73 publications

References 85 publications

PRECURSORS PRIOR TO TYPE IIn SUPERNOVA EXPLOSIONS ARE COMMON: PRECURSOR RATES, PROPERTIES, AND CORRELATIONS

PRECURSORS PRIOR TO TYPE IIn SUPERNOVA EXPLOSIONS ARE COMMON: PRECURSOR RATES, PROPERTIES, AND CORRELATIONS

iPTF SEARCH FOR AN OPTICAL COUNTERPART TO GRAVITATIONAL-WAVE TRANSIENT GW150914

Light Curves of Hydrogen-poor Superluminous Supernovae from the Palomar Transient Factory

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