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http://hdl.handle.net/20.500.12386/23900
Titolo: | Selecting superluminous supernovae in faint galaxies from the first year of the Pan-STARRS1 Medium Deep Survey | Autori: | McCrum, M. Smartt, S. J. Rest, A. Smith, K. Kotak, R. Rodney, S. A. Young, D. R. Chornock, R. Berger, E. Foley, R. J. Fraser, M. Wright, D. Scolnic, D. Tonry, J. L. Urata, Y. Huang, K. PASTORELLO, Andrea BOTTICELLA, MARIA TERESA Valenti, S. Mattila, S. Kankare, E. Farrow, D. J. Huber, M. E. Stubbs, C. W. Kirshner, R. P. Bresolin, F. Burgett, W. S. Chambers, K. C. Draper, P. W. Flewelling, H. Jedicke, R. Kaiser, N. Magnier, E. A. Metcalfe, N. Morgan, J. S. Price, P. A. Sweeney, W. Wainscoat, R. J. Waters, C. |
Data pubblicazione: | 2015 | Rivista: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | Numero: | 448 | Fascicolo: | 2 | Da pagina:: | 1206 | Abstract: | The Pan-STARRS1 (PS1) survey has obtained imaging in five bands (griz y<SUB>P1</SUB>) over 10 Medium Deep Survey (MDS) fields covering a total of 70 square degrees. This paper describes the search for apparently hostless supernovae (SNe) within the first year of PS1 MDS data with an aim of discovering superluminous supernovae (SLSNe). A total of 249 hostless transients were discovered down to a limiting magnitude of M<SUB>AB</SUB> ̃ 23.5, of which 76 were classified as Type Ia supernovae (SNe Ia). There were 57 SNe with complete light curves that are likely core-collapse SNe (CCSNe) or type Ic SLSNe and 12 of these have had spectra taken. Of these 12 hostless, non-Type Ia SNe, 7 were SLSNe of type Ic at redshifts between 0.5 and 1.4. This illustrates that the discovery rate of type Ic SLSNe can be maximized by concentrating on hostless transients and removing normal SNe Ia. We present data for two possible SLSNe; PS1-10pm (z = 1.206) and PS1-10ahf (z = 1.1), and estimate the rate of type Ic SLSNe to be between 3^{+3}_{-2}× 10^{-5} and 8^{+2}_{-1}× 10^{-5} that of the CCSN rate within 0.3 ≤ z ≤ 1.4 by applying a Monte Carlo technique. The rate of slowly evolving, type Ic SLSNe (such as SN2007bi) is estimated as a factor of 10 lower than this range. | Acknowledgments: | The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan- STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard–Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant no. AST-1238877, and the University of Maryland. SJS acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement no. [291222] (PI: SJS). This work is based on observations made with the following telescopes: William Herschel Telescope (operated by the Isaac Netwon Group), in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma; the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (USA), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciência, Tecnologia e Inovação (Brazil) and Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina). Some observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Support for SAR was provided by NASA through Hubble Fellowship grant #HST-HF-51312.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. JLT acknowledges support for this work provided by National Science Foundation grant AST-1009749. SM acknowledges financial support from the Academy of Finland (project: 8120503). We thank A. Gal-Yam and P. Nugent for providing the classification of PS1-11acn, which is the PTF object PTF11dws. Facilities: Pan-STARRS1, Gemini, William Herschel Telescope. | URI: | http://hdl.handle.net/20.500.12386/23900 | URL: | https://academic.oup.com/mnras/article/448/2/1206/2907968 | ISSN: | 0035-8711 | DOI: | 10.1093/mnras/stv034 | Bibcode ADS: | 2015MNRAS.448.1206M | Fulltext: | open |
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