The Zwicky Transient Facility phase I sample of hydrogen-rich superluminous supernovae without strong narrow emission linesStockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden..
Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden..
Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden..
Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.;Univ Maryland, Dept Astron, College Pk, MD 20742 USA.;NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Mail Code 661, Greenbelt, MD 20771 USA..
CALTECH, Caltech Opt Observ, 35899 Canfield Rd, Palomar Mt, CA 92060 USA..
Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden..
CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA..
CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA..
Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel..
CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA..
CALTECH, IPAC, 1200 E Calif Blvd, Pasadena, CA 91225 USA..
Univ Claude Bernard Lyon 1, Univ Lyon, CNRS IN2P3, IP2I Lyon, F-69622 Villeurbanne, France..
CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.;CALTECH, Ctr Data Driven Discovery, Pasadena, CA 91125 USA..
CALTECH, IPAC, 1200 E Calif Blvd, Pasadena, CA 91225 USA..
Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RE, Merseyside, England..
CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA..
Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden.;INAF Osservatorio Astron Padova, DellO, Vicolo Osservatorio 5, I-35122 Padua, Italy..
CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA..
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2022 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 516, no 1, p. 1193-1218Article in journal (Refereed) Published
Abstract [en]
We present a sample of 14 hydrogen-rich superluminous supernovae (SLSNe II) from the Zwicky Transient Facility (ZTF) between 2018 and 2020. We include all classified SLSNe with peaks M-g < -20 mag with observed broad but not narrow Balmer emission, corresponding to roughly 20 per cent of all hydrogen-rich SLSNe in ZTF phase I. We examine the light curves and spectra of SLSNe II and attempt to constrain their power source using light-curve models. The brightest events are photometrically and spectroscopically similar to the prototypical SN 2008es, while others are found spectroscopically more reminiscent of non-superluminous SNe II, especially SNe II-L. Ni-56 decay as the primary power source is ruled out. Light-curve models generally cannot distinguish between circumstellar interaction (CSI) and a magnetar central engine, but an excess of ultraviolet (UV) emission signifying CSI is seen in most of the SNe with UV data, at a wide range of photometric properties. Simultaneously, the broad H alpha profiles of the brightest SLSNe II can be explained through electron scattering in a symmetric circumstellar medium (CSM). In other SLSNe II without narrow lines, the CSM may be confined and wholly overrun by the ejecta. CSI, possibly involving mass lost in recent eruptions, is implied to be the dominant power source in most SLSNe II, and the diversity in properties is likely the result of different mass loss histories. Based on their radiated energy, an additional power source may be required for the brightest SLSNe II, however - possibly a central engine combined with CSI.
Place, publisher, year, edition, pages
Oxford University Press (OUP) , 2022. Vol. 516, no 1, p. 1193-1218
Keywords [en]
transients: supernovae, stars: magnetars, stars: mass-loss, galaxies: statistics
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:kth:diva-318180DOI: 10.1093/mnras/stac2218ISI: 000849496600005Scopus ID: 2-s2.0-85138638964OAI: oai:DiVA.org:kth-318180DiVA, id: diva2:1696391
Note
QC 20220916
2022-09-162022-09-162023-06-08Bibliographically approved