Broad-emission-line dominated hydrogen-rich luminous supernovae
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Hydrogen-rich Type II supernovae (SNe II) are the most frequently observed class of core-collapse SNe (CCSNe). However, most studies that analyse large samples of SNe II lack events with absolute peak magnitudes brighter than −18.5 mag at rest-frame optical wavelengths. Thanks to modern surveys, the detected number of such luminous SNe II (LSNe II) is growing. There exist several mechanisms that could produce luminous SNe II. The most popular propose either the presence of a central engine (a magnetar gradually spinning down or a black hole accreting fallback material) or the interaction of supernova ejecta with circumstellar material (CSM) that turns kinetic energy into radiation energy. In this work, we study the light curves and spectral series of a small sample of six LSNe II that show peculiarities in their H α profile, to attempt to understand the underlying powering mechanism. We favour an interaction scenario with CSM that is not dense enough to be optically thick to electron scattering on large scales – thus, no narrow emission lines are observed. This conclusion is based on the observed light curve (higher luminosity, fast decline, blue colours) and spectral features (lack of persistent narrow lines, broad H α emission, lack of H α absorption, weak, or non-existent metal lines) together with comparison to other luminous events available in the literature. We add to the growing evidence that transients powered by ejecta–CSM interaction do not necessarily display persistent narrow emission lines.
| Originalsprog | Engelsk |
|---|---|
| Tidsskrift | Monthly Notices of the Royal Astronomical Society |
| Vol/bind | 523 |
| Udgave nummer | 4 |
| Sider (fra-til) | 5315-5340 |
| Antal sider | 26 |
| ISSN | 0035-8711 |
| DOI | |
| Status | Udgivet - 4 aug. 2023 |
Bibliografisk note
Funding Information:
LM acknowledges support from a CONICET fellowship and UNRN PI2018 40B885 grant.
Funding Information:
LG acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN), the Agencia Estatal de Investigación (AEI) 10.13039/501100011033, and the European Social Fund (ESF) ‘Investing in your future’ under the 2019 Ramón y Cajal program RYC2019-027683-I and the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016, and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M.
Funding Information:
AVF received generous financial support from the Christopher R. Redlich Fund and many individual donors.
Funding Information:
MG is supported by the EU Horizon 2020 research and innovation programme under grant agreement No 101004719.
Funding Information:
TEMB acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN), the Agencia Estatal de Investigación (AEI) 10.13039/501100011033, and the European Union Next Generation EU/PRTR funds under the 2021 Juan de la Cierva program FJC2021-047124-I and the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016, and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M.
Funding Information:
MN is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 948381) and by a Fellowship from the Alan Turing Institute.
Funding Information:
This work makes use of observations from the Las Cumbres Observatory global telescope network (LCO). LCO data have been obtained via OPTICON. The OPTICON project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant no. 730890. The LCO team is supported by NSF grants AST-1911225 and AST-1911151. This work was funded by ANID, Millennium Science Initiative, ICN12_009.
Funding Information:
TMR acknowledges the financial support of the Vilho, Yrjö and Kalle Väisälä Foundation of the Finnish academy of Science and Letters.
Funding Information:
Support for GP is provided by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics (MAS). PC acknowledges support via an Academy of Finland grant (340613; P.I. R. Kotak).
Funding Information:
XW is supported by the National Natural Science Foundation of China (NSFC grants 12288102, 12033003, and 11633002), the Scholar Program of Beijing Academy of Science and Technology (DZ:BS202002), and the Tencent Xplorer Prize.
Funding Information:
PJP thanks Joe Lyman for guidance with some of the used software. PJP thanks the useful input of Tuomas Kangas. PJP acknowledges funding support by the ESO Ph.D. studentship program.
Publisher Copyright:
© 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
ID: 362685224