On the diversity of superluminous supernovae: ejected mass as the dominant factor
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Nicholl, M.
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Smartt, S. J.
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Jerkstrand, A.
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Inserra, C.
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Sim, S. A.
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Chen, T. W.
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Benetti, S.
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Fraser, M.
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Gal Yam, Avishay
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Kankare, E.
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Maguire, K.
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Smith, K.
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Sullivan, M.
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Valenti, S.
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Young, D. R.
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Baltay, C.
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Bauer, F. E.
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Baumont, S.
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Bersier, D.
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Botticella, M. T.
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Childress, M.
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Dennefeld, M.
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Della Valle, Massimo
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Elias Rosa, N.
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Feindt, U.
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Galbany, Lluis
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Hadjiyska, E.
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Le Guillou, L.
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Leloudas, G.
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Mazzali, P.
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McKinnon, R.
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Polshaw, J.
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Rabinowitz, D.
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Rostami, S.
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Scalzo, R.
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Schmidt, B. P.
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Schulze, S.
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Sollerman, J.
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Taddia, F.
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Yuan, F.
Admission date
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2015-12-11T18:22:06Z
Available date
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2015-12-11T18:22:06Z
Publication date
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2015
Cita de ítem
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Monthly Noticies of the Royal Astronomical Society Volumen: 452 Número: 4 (2015)
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Identifier
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DOI: 10.1093/mnras/stv1522
Identifier
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https://repositorio.uchile.cl/handle/2250/135644
General note
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Artículo de publicación ISI
en_US
Abstract
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We assemble a sample of 24 hydrogen-poor superluminous supernovae (SLSNe). Parameterizing the light-curve shape through rise and decline time-scales shows that the two are highly correlated. Magnetar-powered models can reproduce the correlation, with the diversity in rise and decline rates driven by the diffusion time-scale. Circumstellar interaction models can exhibit a similar rise-decline relation, but only for a narrow range of densities, which may be problematic for these models. We find that SLSNe are approximately 3.5 mag brighter and have light curves three times broader than SNe Ibc, but that the intrinsic shapes are similar. There are a number of SLSNe with particularly broad light curves, possibly indicating two progenitor channels, but statistical tests do not cleanly separate two populations. The general spectral evolution is also presented. Velocities measured from Fe II are similar for SLSNe and SNe Ibc, suggesting that diffusion time differences are dominated by mass or opacity. Flat velocity evolution in most SLSNe suggests a dense shell of ejecta. If opacities in SLSNe are similar to other SNe Ibc, the average ejected mass is higher by a factor 2-3. Assuming. = 0.1 cm(2) g(-1), we estimate a mean (median) SLSN ejecta mass of 10 M-circle dot (6 M-circle dot), with a range of 3-30 M-circle dot. Doubling the assumed opacity brings the masses closer to normal SNe Ibc, but with a high-mass tail. The most probable mechanism for generating SLSNe seems to be the core collapse of a very massive hydrogen-poor star, forming a millisecond magnetar.
Stritzinger, M. D.; Anderson, J. P.; Contreras, C.; Hamuy Wackenhut, Mario(EDP Sciences, 2018)
The first phase of the Carnegie Supernova Project (CSP-I) was a dedicated supernova follow-up program based at the Las Campanas Observatory that collected science data of young, low-redshift supernovae between 2004 and ...
Suntzeff, Nicholas B.; Phillips, M. M.; Covarrubias, R.; Navarrete, M.; Pérez, J. J.; Guerra, A.; Acevedo, M. T.; Doyle, Laurence R.; Harrison, Thomas; Kane, Stephen; Long, Knox S.; Maza Sancho, José; Miller, Scot; Piatti, Andrés E.; Claría, Juan J.; Ahumada, Andrea V.; Pritzl, Barton; Winkler, P. Frank(1999-03)
We present the UBV (RI) light curves of the Type Ia supernova SN 1998bu, which appeared in the nearby galaxy M96 (NGC K3C368). M96 is a spiral galaxy in the Leo I group that has a Cepheid-based
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