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|Title:||Spectroscopy of superluminous supernova host galaxies. A preference of hydrogen-poor events for extreme emission line galaxies||Authors:||Leloudas, G.
de Ugarte Postigo, A.
Thöne, C. C.
Anderson, J. P.
Bauer, F. E.
GALLAZZI, Anna Rita
Hełminiak, K. G.
Wheeler, J. C.
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||449||Issue:||1||First Page:||917||Abstract:||Superluminous supernovae (SLSNe) are very bright explosions that were only discovered recently and that show a preference for occurring in faint dwarf galaxies. Understanding why stellar evolution yields different types of stellar explosions in these environments is fundamental in order to both uncover the elusive progenitors of SLSNe and to study star formation in dwarf galaxies. In this paper, we present the first results of our project to study SUperluminous Supernova Host galaxIES, focusing on the sample for which we have obtained spectroscopy. We show that SLSNe-I and SLSNe-R (hydrogen-poor) often (̃50 per cent in our sample) occur in a class of galaxies that is known as Extreme Emission Line Galaxies (EELGs). The probability of this happening by chance is negligible and we therefore conclude that the extreme environmental conditions and the SLSN phenomenon are related. In contrast, SLSNe-II (hydrogen-rich) occur in more massive, more metal-rich galaxies with softer radiation fields. Therefore, if SLSNe-II constitute a uniform class, their progenitor systems are likely different from those of H-poor SLSNe. Gamma-ray bursts (GRBs) are, on average, not found in as extreme environments as H-poor SLSNe. We propose that H-poor SLSNe result from the very first stars exploding in a starburst, even earlier than GRBs. This might indicate a bottom-light initial mass function in these systems. SLSNe present a novel method of selecting candidate EELGs independent of their luminosity.||Acknowledgments:||We are grateful to Enrique Pérez-Montero for sharing with us his photoionization models. We also thank: Manos Chatzopoulos for the spectrum of SN 2008am, Andrew Levan for discussions concerning observation planning, Robert Quimby for providing us blind offsets for PTF09cwl and for confirming to us the coordinates and nature of PTF10qaf, and Paul Vreeswijk for comments. We acknowledge useful discussions with Jesus Zavala. SS acknowledges support from CONICYT-Chile FONDECYT 3140534, Basal-CATA PFB-06/2007, and Project IC120009 ‘Millennium Institute of Astrophysics (MAS)’ of Iniciativa Científica Milenio del Ministerio de Economía, Fomento y Turismo. The research activity of AdUP, CT and JG is supported by Spanish research project AYA2012-5 39362-C02-02. AdUP acknowledges support by the European Commission under the Marie Curie Career Integration Grant programme (FP7-PEOPLE-2012-CIG 322307). FEB acknowledges support from Basal-CATA PFB-06/2007, CONICYT-Chile (FONDECYT 1141218, ‘EMBIGGEN’ Anillo ACT1101) and Project IC120009 ‘Millennium Institute of Astrophysics (MAS)’ of the Iniciativa Científica Milenio del Ministerio de Economía, Fomento y Turismo. AG acknowledges financial support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 267251 (AstroFIt). KGH acknowledges support provided by the National Astronomical Observatory of Japan as Subaru Astronomical Research Fellow, and the Polish National Science centre grant 2011/03/N/ST9/01819. EI acknowledges funding from CONICYT/FONDECYT postdoctoral project no: 3130504. JV is supported by Hungarian OTKA Grant NN 107637. This work was supported in part by NSF grant AST 11-09801 to JCW and by NSF grant PHYS-1066293 and the hospitality of the Aspen Center for Physics extended to JCW. The Dark Cosmology Centre is funded by the Danish National Research Foundation. This research has made use of the GHostS data base, which is partly funded by Spitzer /NASA grant RSA Agreement No. 1287913. Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. Based on observations made with Magellan as part of CN2013A-195, CN2013B-70, CN2013B-34, CN2014A-114. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 089.D-0902(ABC), 091.D-0734(ABC), 290.D-5139(A), 093.D-0867(A).||URI:||http://hdl.handle.net/20.500.12386/23606||URL:||https://arxiv.org/abs/1409.8331
|Appears in Collections:||1.01 Articoli in rivista|
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