Probing Shock Breakout with Serendipitous
                    <i>GALEX</i>
                    Detections of Two SNLS Type II-P Supernovae

Gezari, Suvi; Dessart, Luc; Basa, S.; Martin, D. Christopher; Neill, James D.; Woosley, S. E.; Hillier, D. J.; Bazin, G.; Forster, Karl; Friedman, Peter G.; Du, J. Le; Mazure, A.; Morrissey, Patrick; Neff, Susan G.; Schiminovich, David; Wyder, Ted K.

doi:10.1086/591647

Cited by 113 publications

(155 citation statements)

References 31 publications

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“…The first phase is the shock breakout phase, where the internal energy of the shock diffuses out to give an X-ray (extended progenitor) or gamma-ray (compact progenitor) burst. This phase lasts only for minutes or hours (Falk & Arnett 1977) and only been observed for two Type II-P SNe (SNLS04D2dc and SNLS-06D1jd Gezari et al 2008;Schawinski et al 2008) and once for a Type I SN (SN 2008D, Soderberg et al 2008.…”

Section: Appendix A: Light Curve Modelsmentioning

confidence: 98%

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

Gáll

Polshaw

Kotak

et al. 2015

A&A

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We report on our findings based on the analysis of observations of the Type II-L supernova LSQ13cuw within the framework of currently accepted physical predictions of core-collapse supernova explosions. LSQ13cuw was discovered within a day of explosion, hitherto unprecedented for Type II-L supernovae. This motivated a comparative study of Type II-P and II-L supernovae with relatively well-constrained explosion epochs and rise times to maximum (optical) light. From our sample of twenty such events, we find evidence of a positive correlation between the duration of the rise and the peak brightness. On average, SNe II-L tend to have brighter peak magnitudes and longer rise times than SNe II-P. However, this difference is clearest only at the extreme ends of the rise time versus peak brightness relation. Using two different analytical models, we performed a parameter study to investigate the physical parameters that control the rise time behaviour. In general, the models qualitatively reproduce aspects of the observed trends. We find that the brightness of the optical peak increases for larger progenitor radii and explosion energies, and decreases for larger masses. The dependence of the rise time on mass and explosion energy is smaller than the dependence on the progenitor radius. We find no evidence that the progenitors of SNe II-L have significantly smaller radii than those of SNe II-P.

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Section: Appendix A: Light Curve Modelsmentioning

confidence: 98%

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

Gáll

Polshaw

Kotak

et al. 2015

A&A

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show abstract

“…Closer to the VLE SNe regime, UV observations using the GALEX satellite in 2008 detected two CCSNe very close to the time of explosion (Gezari et al 2008): one with fading and one with rapidly rising UV emission, suggesting that the latter had been caught during its breakout phase. KEPLER hydrodynamic models combined with the CMFGEN radiation transport code were used to model the observed UV light curve of these events as breakout in a 15 M red supergiant exploding with a final kinetic energy 1.2 B.…”

Section: Candidate Shock Breakout Eventsmentioning

confidence: 99%

Very Low-energy Supernovae: Light Curves and Spectra of Shock Breakout

Lovegrove

Woosley

Zhang

2017

ApJ

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The brief transient emitted as a shock wave erupts through the surface of a presupernova star carries information about the stellar radius and explosion energy. Here the CASTRO code, which treats radiation transport using multigroup flux-limited diffusion, is used to simulate the light curves and spectra of shock breakout in very low-energy supernovae (VLE SNe), explosions in giant stars with final kinetic energy much less than 10 51 erg. VLE SNe light curves, computed here with the KEPLER code, are distinctively faint, red, and long-lived, making them challenging to find with transient surveys. The accompanying shock breakouts are brighter, though briefer, and potentially easier to detect. Previous analytic work provides general guidance, but numerical simulations are challenging due to the range of conditions and lack of equilibration between color and effective temperatures. We consider previous analytic work and extend discussions of color temperature and opacity to the lower energy range explored by these events. Since this is the first application of the CASTRO code to shock breakout, test simulations of normal energy shock breakout of SN1987A are carried out and compared with the literature. A set of breakout light curves and spectra are then calculated for VLE SNe with final kinetic energies in the range 10 47 − 10 50 ergs for red supergiants with main sequence masses 15 M and 25 M . The importance of uncertainties in stellar atmosphere model, opacity, and ambient medium is discussed, as are observational prospects with current and forthcoming missions.

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“…However, the Swift/XRT and UVOT provided evidence of their existence by detecting the early X-ray/UV emission a few days before SNe 2006aj associated with the GRB 060218 (Campana et al 2006) and before SNe 2008D (Soderberg et al 2008). The GALEX satellite detected serendipitous early UV events associated with SNe SNLS-04D2dc (Schawinski et al 2008;Gezari et al 2008), SNLS-06D1jd (Gezari et al 2008), and 2010aq (Gezari et al 2010).…”

Section: Supernova Shock Breakoutsmentioning

confidence: 99%

“…For red supergiant progenitors (radius ∼10 13 cm, then Type II-P SNe), T 0 was estimated with 0.75 day accuracy for SNLS-06D1jd and 0.35 days for SNLS-04D2dc (Gezari et al 2008), while Schawinski et al (2008) was able to estimate it with a precision of ∼1 h. A 0.02 day accuracy was reached for SN 2010aq (Gezari et al 2010) by fitting the data with theoretical models (Rabinak & Waxman 2011). For WolfRayet star progenitors (radius ∼10 11 cm, then Type Ibc SNe), the onset of the X-ray SBO associated with SN 2008D (Soderberg et al 2008) was determined with an accuracy of 9 +8 −20 s. A precise determination of the (T 0 ), achieved with SBO observations and accurate theoretical models describing how the shock wave propagates through the exploding star, is fundamental in the multi-messenger studies, which use SBOs as triggers to search for GWs and neutrinos (see Sect.…”

Section: Supernova Shock Breakoutsmentioning

confidence: 99%

“…Longer duration (days) shock breakouts (SBOs) have been observed with GALEX by type II SNe related to larger (red giant) progenitors (e.g. Gezari et al 2008;Schawinski et al 2008). This is an important tool, since the direct detection of SN progenitors is incredibly difficult and has only been possible for a small number of nearby corecollapse SNe with pre-explosion high-resolution imaging.…”

Section: Introductionmentioning

confidence: 99%

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A time domain experiment withSwift: monitoring of seven nearby galaxies

Andreoni¹,

D’Avanzo²,

Campana³

et al. 2016

A&A

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Context. Focused on the study of transient sources, time domain astronomy today is one of the most active and growing areas of research in astronomy. Most of the present and planned surveys aimed at carrying out time domain studies work in the optical band and founded their searching strategies on fixed cadences. Although nothing similar currently exists in the X-ray and ultraviolet (UV) bands, the Swift satellite is certainly the most appropriate available instrument to carry out such surveys. Aims. We aimed to detect a supernova (SN) shock breakout (SBO) in nearby galaxies. The SBO marks the first escape of radiation from the blast wave that breaks through the photosphere of the star and launches the SN ejecta. The detection of an SBO is a diagnostic for the radius of the progenitor star and the ratio of explosion energy to ejecta mass. It also allows us to determine the onset of the explosion with an accuracy of a few hours to a few seconds. Methods. Using the XRT and UVOT instruments onboard the Swift satellite, we carried out a weekly cadenced, six-month monitoring of seven nearby galaxies: NGC 1084, NGC 2207/IC 2163, NGC 2770, NGC 4303/M 61, NGC 3147, NGC 3690, and NGC 6754. We searched for variable or transient sources in the collected data. These galaxies were selected because they are close (distance ≤50 Mpc), small enough to fit in the Swift/UVOT field of view, and are hosts of at least three SNe in the past 20 yr. Results. We found no evidence for an SN SBO event. Five objects located within the light of the sample galaxies were found to be variable in the X-ray and/or in the UV. These include mainly background active galactic nucleus and unresolved ULX in NGC 3690. In addition to these objects, we found two variable Galactic sources: the known nova CP Draconis (which experienced an outburst during our monitoring) and an uncatalogued eclipsing binary. Conclusions. Despite the lack of SBO detections, the results of our explorative study encourage the use of Swift in further time domain studies. Moreover, since our sample galaxies are within the Universe volume that will be reached by the forthcoming advanced gravitational wave (GW) detectors (a-LIGO and a-Virgo), this work provides an example on how to carry out Swift surveys from which the GW signal from SNe can be detected, and to detect counterparts to GW triggers.

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Probing Shock Breakout with Serendipitous GALEX Detections of Two SNLS Type II-P Supernovae

Cited by 113 publications

References 31 publications

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

A comparative study of Type II-P and II-L supernova rise times as exemplified by the case of LSQ13cuw

Very Low-energy Supernovae: Light Curves and Spectra of Shock Breakout

A time domain experiment withSwift: monitoring of seven nearby galaxies

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