Broad-emission-line dominated hydrogen-rich luminous supernovae

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...

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Detalles Bibliográficos
Autores: Pessi, Priscila Jael, Anderson, J. P., Folatelli, Gaston, Dessart, L., González Gaitán, S., Möller, A., Gutiérrez, C. P., Mattila, S., Reynolds, T. M., Charalampopoulos, P., Filippenko, A.V., Galbany, Lluís, Gal Yam, A., Gromadzki, M., Hiramatsu, D., Howell, D. A., Inserra, C., Kankare, E., Lunnan, R., Martinez, Laureano, McCully, C., Meza, N., Müller Bravo, T. E., Nicholl, M., Pellegrino, C., Pignata, G., Sollerman, J., Tucker, B. E., Wang, X., Young, D. R.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2023
País:Argentina
Institución:Consejo Nacional de Investigaciones Científicas y Técnicas
Repositorio:CONICET Digital (CONICET)
Idioma:inglés
OAI Identifier:oai:ri.conicet.gov.ar:11336/234197
Acceso en línea:http://hdl.handle.net/11336/234197
Access Level:acceso abierto
Palabra clave:SN 2017GPP
SN 2017HBJ
SN 2017HXZ
SN 2018AQL
SN 2018EPH)
TRANSIENTS: SUPERNOVAE – SUPERNOVAE: INDIVIDUAL (SN 2017CFO
https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
Descripción
Sumario: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.

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