Rapidly evolving transients in the Dark Energy Survey
Author
Pursiainen, M.; Childress, M.; Smith, M.; Prajs, S.; Sullivan, M.; Davis, T. M.; Foley, R. J.; Asorey, J.; Calcino, J.; Carollo, D.; Curtin, C.; D'Andrea, C. B.; Glazebrook, K.; Gutierrez, C.; Hinton, S. R.; Hoormann, J. K.; Inserra, C.; Kessler, R.; King, A.; Kuehn, K.; Lewis, G. F.; Lidman, C.; Macaulay, E.; Möller, A.; Nichol, Robert C.; Sako, M.; Sommer, N. E.; Swann, E.; Tucker, B. E.; Uddin, S. A.; Wiseman, P.; Zhang, B.; Abbott, T. M.C.; Abdalla, F. B.; Allam, S.; Annis, J.; Avila, S.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Rosell, A. Carnero; Kind, M. Carrasco; Carretero, J.; Castander, F. J.; Cunha, C. E.; Davis, C.; De Vicente, J.; Diehl, H. T.; Doel, P.; Eifler, T. F.; Flaugher, B.; Fosalba, P.; Frieman, J.; García-Bellido Capdevila, Juan; Gruen, D.; Gruendl, R. A.; Gutierrez, G.; Hartley, W. G.; Hollowood, D. L.; Honscheid, K.; James, D. J.; Jeltema, T.; Kuropatkin, N.; Li, T. S.; Lima, M.; Maia, M. A.G.; Martini, P.; Menanteau, F.; Ogando, R. L.C.; Plazas, A. A.; Roodman, A.; Sánchez, E.Publisher
Oxford University Press on behalf of the Royal Astronomical SocietyDate
2018-08-29Citation
10.1093/mnras/sty2309
Monthly Notices of the Royal Astronomical Society 481.1 (2018): 894-917
ISSN
0035-8711 (print); 1365-2966 (online)DOI
10.1093/mnras/sty2309Funded by
We acknowledge support from EU/FP7-ERC grant no [615929]. Based in part on data obtained from the ESO Science Archive Facility under program 097.D-0709. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020 Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacâo Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovaçâo, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy SurveyProject
info:eu-repo/grantAgreement/EC/FP7/615929Editor's Version
https://doi.org/10.1093/mnras/sty2309Subjects
Supernovae: general; FísicaNote
This article has been accepted for publication in Monthly Notices of Royal Astronomical Society © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.Rights
© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.Abstract
We present the results of a search for rapidly evolving transients in the Dark Energy Survey Supernova Programme. These events are characterized by fast light-curve evolution (rise to peak in≲10 d and exponential decline in≲30 d after peak).We discovered 72 events, including 37 transients with a spectroscopic redshift from host galaxy spectral features. The 37 events increase the total number of rapid optical transients by more than a factor of two. They are found at a wide range of redshifts (0.05 < z < 1.56) and peak brightnesses (-15.75 > Mg > -22.25). The multiband photometry is well fit by a blackbody up to few weeks after peak. The events appear to be hot (T ≈ 10 000-30 000 K) and large (R ≈ 1014 - 2 × 1015 cm) at peak, and generally expand and cool in time, though some events show evidence for a receding photosphere with roughly constant temperature. Spectra taken around peak are dominated by a blue featureless continuum consistent with hot, optically thick ejecta. We compare our events with a previously suggested physical scenario involving shock breakout in an optically thick wind surrounding a core-collapse supernova, we conclude that current models for such a scenario might need an additional power source to describe the exponential decline. We find that these transients tend to favour star-forming host galaxies, which could be consistent with a core-collapse origin. However, more detailed modelling of the light curves is necessary to determine their physical origin.
Files in this item
Google Scholar:Pursiainen, M.
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Childress, M.
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Smith, M.
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Prajs, S.
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Sullivan, M.
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Davis, T. M.
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Foley, R. J.
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Asorey, J.
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Calcino, J.
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Carollo, D.
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Curtin, C.
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D'Andrea, C. B.
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Glazebrook, K.
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Gutierrez, C.
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Hinton, S. R.
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Hoormann, J. K.
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Inserra, C.
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Kessler, R.
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King, A.
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Kuehn, K.
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Lewis, G. F.
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Lidman, C.
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Macaulay, E.
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Möller, A.
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Nichol, Robert C.
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Sako, M.
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Sommer, N. E.
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Swann, E.
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Tucker, B. E.
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Uddin, S. A.
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Wiseman, P.
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Zhang, B.
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Abbott, T. M.C.
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Abdalla, F. B.
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Allam, S.
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Annis, J.
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Avila, S.
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Brooks, D.
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Buckley-Geer, E.
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Burke, D. L.
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Rosell, A. Carnero
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Kind, M. Carrasco
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Carretero, J.
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Castander, F. J.
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Cunha, C. E.
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Davis, C.
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De Vicente, J.
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Diehl, H. T.
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Doel, P.
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Eifler, T. F.
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Flaugher, B.
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Fosalba, P.
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Frieman, J.
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García-Bellido Capdevila, Juan
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Gruen, D.
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Gruendl, R. A.
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Gutierrez, G.
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Hartley, W. G.
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Hollowood, D. L.
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Honscheid, K.
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James, D. J.
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Jeltema, T.
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Kuropatkin, N.
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Li, T. S.
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Lima, M.
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Maia, M. A.G.
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Martini, P.
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Menanteau, F.
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Ogando, R. L.C.
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Plazas, A. A.
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Roodman, A.
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Sánchez, E.
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