Maqola

Cosmic evolution and metal aversion in superluminous supernova host galaxies

S. SchulzeDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, IsraelT. KrühlerMax-Planck-Institut für extraterrestrische Physik, Gießenbachstraße, D-85748 Garching, GermanyG. LeloudasDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, DenmarkJ. GorosabelDepartamento de Física Aplicada I, Unidad Asociada Grupo Ciencia Planetarias UPV/EHU-IAA/CSIC, E.T.S. Ingeniería, Universidad del País-Vasco UPV/EHU, Alameda de Urquijo s/n, E-48013 Bilbao, SpainA. MehnerJohannes BüchnerInstituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Vicuña Mackenna 4860, 7820436 Macul, Santiago, ChileS. KimInstituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Vicuña Mackenna 4860, 7820436 Macul, Santiago, ChileE. IbarInstituto de Física y Astronomía, Universidad de Valparaíso, Avda. Gran Bretaña 1111, Valparaíso, ChileR. AmorínCavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge CB3 0HE, UKR. Herrero‐IllanaESO, Alonso de Cordova 3107, Vitacura, Santiago de Chile, ChileJ. P. AndersonF. E. BauerInstituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Vicuña Mackenna 4860, 7820436 Macul, Santiago, ChileL. ChristensenDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, DenmarkM. de PasqualeMullard Space Science Laboratory - University College London, Holmbury Rd, Dorking RH5 6NT, UKA. de Ugarte PostigoInstituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, E-18008, Granada, SpainAnna GallazziINAF − Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, I-50125 Firenze, ItalyJ. HjorthDark 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, ChileD. MalesaniDark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, DenmarkMartin SparreHeidelberger Institut fur Theoretische Studien, Schloss-Wolfsbrunnenweg 35, D-69118 Heidelberg, GermanyB. StalderInstitute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USAA. A. StarkSmithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138, USAC. C. ThöneInstituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, E-18008, Granada, SpainJ. Craig WheelerDepartment of Astronomy, University of Texas at Austin, Austin, TX 78712, USA

2017en

ABI

Annotatsiya

The SUperluminous Supernova Host galaxIES survey aims to provide strong new constraints on the progenitors of superluminous supernovae (SLSNe) by understanding the relationship to their host galaxies. We present the photometric properties of 53 H-poor and 16 H-rich SLSN host galaxies out to z ∼ 4. We model their spectral energy distributions to derive physical properties, which we compare with other galaxy populations. At low redshift, H-poor SLSNe are preferentially found in very blue, low-mass galaxies with high average specific star formation rates. As redshift increases, the host population follows the general evolution of star-forming galaxies towards more luminous galaxies. After accounting for secular evolution, we find evidence for differential evolution in galaxy mass, but not in the B band and the far-ultraviolet luminosity (3σ confidence). Most remarkable is the scarcity of hosts with stellar masses above 1010 M⊙ for both classes of SLSNe. In case of H-poor SLSNe, we attribute this to a stifled production efficiency above ∼0.4 solar metallicity. However, we argue that, in addition to low metallicity, a short-lived stellar population is also required to regulate the SLSN production. H-rich SLSNe are found in a very diverse population of star-forming galaxies. Still, the scarcity of massive hosts suggests a stifled production efficiency above ∼0.8 solar metallicity. The large dispersion of the H-rich SLSNe host properties is in stark contrast to those of gamma-ray burst, regular core-collapse SN, and H-poor SLSNe host galaxies. We propose that multiple progenitor channels give rise to this subclass.

Hali tarjima qilinmagan

Identifikatorlar

DOI: 10.1093/mnras/stx2352

Iqtiboslar va manbalar

3 ta iqtibos0 ta foydalanilgan manba

Koʻrsatkichlar — AkademScholar