Maqola

Spectroscopy of superluminous supernova host galaxies. A preference of hydrogen-poor events for extreme emission line galaxies

G. LeloudasDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, DenmarkS. SchulzeMillennium Institute of Astrophysics, Vicua Mackenna 4860, 7820436 Macul, Santiago, ChileT. KrühlerJ. GorosabelInstituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, E-18008 Granada, SpainL. ChristensenDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, DenmarkA. MehnerA. de Ugarte PostigoInstituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, E-18008 Granada, SpainR. AmorínINAF – Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monteporzio Catone, Roma, ItalyC. C. ThöneInstituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, E-18008 Granada, SpainJ. P. AndersonF. E. BauerInstituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, 306, Santiago 22, ChileAnna GallazziINAF -INAF -Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze, ItalyK. G. HełminiakSubaru Telescope, National Astronomical Observatory of Japan, 650 North Aohoku Place, Hilo, HI 96720, USAJ. HjorthDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, DenmarkE. IbarInstituto de Fsica y Astronoma, Universidad de Valparaso, Avda. Gran Bretaa 1111, Valparaso, ChileD. MalesaniDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, DenmarkN. MorrellLas Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, ChileJozsef VinkoDepartment of Optics and Quantum Electronics, University of Szeged, Szeged, Dem ter 9, 6720, HungaryJ. Craig WheelerDepartment of Astronomy, University of Texas at Austin, Austin, TX 78712, USA

2015en

Ochiq kirishBronza

ABI

Annotatsiya

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.

Hali tarjima qilinmagan

Identifikatorlar

DOI: 10.1093/mnras/stv320

Iqtiboslar va manbalar

3 ta iqtibos0 ta foydalanilgan manba