Ultraviolet Observations of SN 1987A with the IUE Satellite

Pun, C. S. J.; Kirshner, R.; Sonneborn, G.; Challis, Peter; Nassiopoulos, G. E.; Arquilla, R.; Crenshaw, D. Michael; Shrader, C. R.; Teays, T. J.; Cassatella, A.; Gilmozzi, R.; Talavera, A.; Wamsteker, W.; Fransson, Claes; Panagia, N.

doi:10.1086/192185

Cited by 77 publications

(99 citation statements)

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“…(Fransson & Kozma 2002;Seitenzahl et al 2014). To compare the SLSNe light curves with SN 1987A, we assume an explosion date for the SLSNe and shift the bolometric light curves to that of SN 1987A (taken from Pun et al 1995), using the same method as Gal-Yam et al (2009). We shifted the light curve of SN 1987A to match the potential transition from the diffusive phase to the radioactive decay in the SLSN light curves or to the late-time decay.…”

Section: Ni Massesmentioning

confidence: 99%

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

Gal‐Yam

Rubin

et al. 2018

ApJ

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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Section: Ni Massesmentioning

confidence: 99%

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

Gal‐Yam

Rubin

et al. 2018

ApJ

133

126

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“…Whether testing a benchmark model or tracing observed features with a prescription of candidate lines, the interpretation of the observed spectral features and the related empirical (Pun et al 1995); SN1984L at approximately day+8 relative to B-band maximum light (Doggett & Branch 1985;Wheeler & Levreault 1985;Tsvetkov 1987); SN1987M on UT 1987 September 28 and UT 1987 October 2, approximately days+9 and +13, respectively, relative to B-band maximum light (Filippenko et al 1990;Jeffery et al 1991); and SN2011fe near maximum light (Pereira et al 2013 measurements depend on the quality of the full fit from the supporting model. Moreover, if a model spectrum produces all but a single (or few) observed feature(s), the model is judged to be significantly incomplete.…”

Section: Spectral Line Identificationmentioning

confidence: 99%

LINE IDENTIFICATIONS OF TYPE I SUPERNOVAE: ON THE DETECTION OF Si II FOR THESE HYDROGEN-POOR EVENTS

Parrent

Milisavljević

Söderberg

et al. 2016

ApJ

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Here we revisit line identifications of type I supernovae (SNe I) and highlight trace amounts of unburned hydrogen as an important free parameter for the composition of the progenitor. Most one-dimensional stripped-envelope models of supernovae indicate that observed features near 6000-6400 Å in typeI spectra are due to more than Si IIλ6355. However, while an interpretation of conspicuous Si IIλ6355 can approximate 6150 Å absorption features for all SNe Ia during the first month of free expansion, similar identifications applied to 6250 Å features of SNe Ib and Ic have not been as successful. When the corresponding synthetic spectra are compared with highquality timeseries observations, the computed spectra are frequently too blue in wavelength. Some improvement can be achieved with Fe II lines that contribute redward of 6150 Å; however, the computed spectra either remain too blue or the spectrum only reaches a fair agreement when the rise-time to peak brightness of the model conflicts with observations by a factor of two. This degree of disagreement brings into question the proposed explosion scenario. Similarly, a detection of strong Si IIλ6355 in the spectra of broadlined Ic and super-luminous events of type I/R is less convincing despite numerous model spectra used to show otherwise. Alternatively, we suggest 6000-6400 Å features are possibly influenced by either trace amounts of hydrogen or blueshifted absorption and emission in Hα, the latter being an effect which is frequently observed in the spectra of hydrogen-rich, SNe II.

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“…The gamma-ray transfer was modeled by the transfer equation (10) (Humphreys and McElroy 1984). At the distance modulus m − M = 18.5 for the LMC, the color excess E(B-V ) = 0.15, and the interstellar extinction A V = 3.1E(B-V ) (Pun et al 1995), the radius of the blue supergiant is about 46.8R . We take this value as the presupernova radius R 0 .…”

Section: The Mean Opacities and The Emission Coefficientmentioning

confidence: 99%

The light curve of supernova 1987A: The structure of the presupernova and radioactive nickel mixing

Utrobin

2004

Astron. Lett.

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Abstract-We have studied the influence of the presupernova structure and the degree of 56 Ni mixing on the bolometric light curve of SN 1987A in terms of radiation hydrodynamics in the one-group approximation by abandoning LTE and by taking into account nonthermal ionization and the contribution of spectral lines to its opacity. Our study shows that moderate 56 Ni mixing at velocities ≤2500 km scan explain the observed light curve if the density of the outer layers of the presupernova exceeds the value obtained in the evolutionary model of a single nonrotating star severalfold. Abandoning LTE and allowing for nonthermal ionization when solving the equation of state and calculating the mean opacities and the thermal emission coefficient leads to a significant difference between the gas temperature and the radiation temperature in the optically thin layers of the supernova envelope. We demonstrate the fundamental role of the contribution of spectral lines to the opacity in an expanding envelope and of the accurate description of radiative transfer in reproducing the observed shape of the bolometric light curve. We have found that disregarding the contribution of spectral lines to the opacity introduces an error of ∼20% into the explosion energy, and that a similar error is possible when determining the mass of the ejected matter. The resonant scattering of radiation in numerous lines accelerates the outer layers to velocities of ≈36 000 km s −1 ; this additional acceleration affects the outer layers with a mass of ≈10 −6 M . Proper calculations of the supernova luminosity require that not only the delay effects, but also the limb-darkening effects be taken into account.

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Ultraviolet Observations of SN 1987A with the IUE Satellite

Cited by 77 publications

References 0 publications

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

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

LINE IDENTIFICATIONS OF TYPE I SUPERNOVAE: ON THE DETECTION OF Si II FOR THESE HYDROGEN-POOR EVENTS

The light curve of supernova 1987A: The structure of the presupernova and radioactive nickel mixing

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