Статья

On the diversity of superluminous supernovae: ejected mass as the dominant factor

M. Nicholl1Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKStephen Smartt1Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKAnders Jerkstrand1Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKC. Inserra1Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKStuart Sim1Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKT. W. Chen1Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKS. Benetti2INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, ItalyMorgan Fraser3Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UKA. Gal‐Yam4Benoziyo Center for Astrophysics, Weizmann Institute of Science, Rehovot 76100, IsraelE. Kankare1Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKK. Maguire5European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching b. München, GermanyK. Smith1Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKM. Sullivan6School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UKStefano Valenti8Las Cumbres Observatory, Global Telescope Network, 6740 Cortona Drive Suite 102, Goleta, CA 93117, USAD. R. Young1Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKC. Baltay9Department of Physics, Yale University, New Haven, CT 06520-8121, USAF. E. Bauer12Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USAS. BaumontSorbonne UniversitéD. Bersier15Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UKM. T. Botticella16INAF – Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, I-80131 Napoli, ItalyM. Childress18Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, AustraliaM. Dennefeld19Institut d'Astrophysique de Paris, CNRS, and Universite Pierre et Marie Curie, 98 bis Boulevard Arago, F-75014 Paris, FranceM. Della Valle16INAF – Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, I-80131 Napoli, ItalyN. Elias–Rosa2INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, ItalyU. Feindt21Physikalisches Institut, Universität Bonn, Nuallee 12, D-53115 Bonn, GermanyL. Galbany11Millennium Institute of Astrophysics, Vicuña Mackenna 4860, 7820436 Macul, Santiago, ChileE. Hadjiyska9Department of Physics, Yale University, New Haven, CT 06520-8121, USAL. Le Guillou14CNRS, UMR 7585, Laboratoire de Physique Nucleaire et des Hautes Energies, 4 place Jussieu, F-75005 Paris, FranceG. Leloudas23Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, DK-2100 Copenhagen, DenmarkP. A. Mazzali15Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UKR. McKinnon9Department of Physics, Yale University, New Haven, CT 06520-8121, USAJ. Polshaw1Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UKD. Rabinowitz9Department of Physics, Yale University, New Haven, CT 06520-8121, USAS. Rostami9Department of Physics, Yale University, New Haven, CT 06520-8121, USAR. Scalzo18Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, AustraliaB. Schmidt18Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, AustraliaS. Schulze10Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, 306, Santiago 22, ChileJ. Sollerman24Department of Astronomy and the Oskar Klein Centre, Stockholm University, AlbaNova, SE-106 91 Stockholm, SwedenF. Taddia24Department of Astronomy and the Oskar Klein Centre, Stockholm University, AlbaNova, SE-106 91 Stockholm, SwedenF. Yuan18Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia

2015en

ABI

Аннотация

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 (6 M ), with a range of 3-30 M . 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.

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Идентификаторы

DOI: 10.1093/mnras/stv1522

Цитирования и источники

Цитирований: 2Использованных источников: 0

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