Broad-emission-line dominated hydrogen-rich luminous supernovae

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Broad-emission-line dominated hydrogen-rich luminous supernovae. / Pessi, P. J.; Anderson, J. P.; Folatelli, G.; Dessart, L.; González-Gaitán, S.; Möller, A.; Gutiérrez, C. P.; Mattila, S.; Reynolds, T. M.; Charalampopoulos, P.; Filippenko, A. V.; Galbany, L.; Gal-Yam, A.; Gromadzki, M.; Hiramatsu, D.; Howell, D. A.; Inserra, C.; Kankare, E.; Lunnan, R.; Martinez, L.; McCully, C.; Meza, N.; Müller-Bravo, T. E.; Nicholl, M.; Pellegrino, C.; Pignata, G.; Sollerman, J.; Tucker, B. E.; Wang, X.; Young, D. R.

In: Monthly Notices of the Royal Astronomical Society, Vol. 523, No. 4, 04.08.2023, p. 5315-5340.

Research output: Contribution to journal › Journal article › Research › peer-review

Harvard

Pessi, PJ, Anderson, JP, Folatelli, G, Dessart, L, González-Gaitán, S, Möller, A, Gutiérrez, CP, Mattila, S, Reynolds, TM, Charalampopoulos, P, Filippenko, AV, Galbany, L, Gal-Yam, A, Gromadzki, M, Hiramatsu, D, Howell, DA, Inserra, C, Kankare, E, Lunnan, R, Martinez, L, McCully, C, Meza, N, Müller-Bravo, TE, Nicholl, M, Pellegrino, C, Pignata, G, Sollerman, J, Tucker, BE, Wang, X & Young, DR 2023, 'Broad-emission-line dominated hydrogen-rich luminous supernovae', Monthly Notices of the Royal Astronomical Society, vol. 523, no. 4, pp. 5315-5340. https://doi.org/10.1093/mnras/stad1822

APA

Pessi, P. J., Anderson, J. P., Folatelli, G., Dessart, L., González-Gaitán, S., Möller, A., Gutiérrez, C. P., Mattila, S., Reynolds, T. M., Charalampopoulos, P., Filippenko, A. V., Galbany, L., Gal-Yam, A., Gromadzki, M., Hiramatsu, D., Howell, D. A., Inserra, C., Kankare, E., Lunnan, R., ... Young, D. R. (2023). Broad-emission-line dominated hydrogen-rich luminous supernovae. Monthly Notices of the Royal Astronomical Society, 523(4), 5315-5340. https://doi.org/10.1093/mnras/stad1822

Vancouver

Pessi PJ, Anderson JP, Folatelli G, Dessart L, González-Gaitán S, Möller A et al. Broad-emission-line dominated hydrogen-rich luminous supernovae. Monthly Notices of the Royal Astronomical Society. 2023 Aug 4;523(4):5315-5340. https://doi.org/10.1093/mnras/stad1822

Author

Pessi, P. J. ; Anderson, J. P. ; Folatelli, G. ; Dessart, L. ; González-Gaitán, S. ; Möller, A. ; Gutiérrez, C. P. ; Mattila, S. ; Reynolds, T. M. ; Charalampopoulos, P. ; Filippenko, A. V. ; Galbany, L. ; Gal-Yam, A. ; Gromadzki, M. ; Hiramatsu, D. ; Howell, D. A. ; Inserra, C. ; Kankare, E. ; Lunnan, R. ; Martinez, L. ; McCully, C. ; Meza, N. ; Müller-Bravo, T. E. ; Nicholl, M. ; Pellegrino, C. ; Pignata, G. ; Sollerman, J. ; Tucker, B. E. ; Wang, X. ; Young, D. R. / Broad-emission-line dominated hydrogen-rich luminous supernovae. In: Monthly Notices of the Royal Astronomical Society. 2023 ; Vol. 523, No. 4. pp. 5315-5340.

Bibtex

@article{f011f1fd35cd422082ed6e9a2b8a1b28,

title = "Broad-emission-line dominated hydrogen-rich luminous supernovae",

abstract = "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.",

keywords = "SN 2017gpp, SN 2017hbj, SN 2017hxz, SN 2018aql, SN 2018eph), transients: supernovae – supernovae: individual (SN 2017cfo",

author = "Pessi, {P. J.} and Anderson, {J. P.} and G. Folatelli and L. Dessart and S. Gonz{\'a}lez-Gait{\'a}n and A. M{\"o}ller and Guti{\'e}rrez, {C. P.} and S. Mattila and Reynolds, {T. M.} and P. Charalampopoulos and Filippenko, {A. V.} and L. Galbany and A. Gal-Yam and M. Gromadzki and D. Hiramatsu and Howell, {D. A.} and C. Inserra and E. Kankare and R. Lunnan and L. Martinez and C. McCully and N. Meza and M{\"u}ller-Bravo, {T. E.} and M. Nicholl and C. Pellegrino and G. Pignata and J. Sollerman and Tucker, {B. E.} and X. Wang and Young, {D. R.}",

note = "Publisher Copyright: {\textcopyright} 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.",

year = "2023",

month = aug,

day = "4",

doi = "10.1093/mnras/stad1822",

language = "English",

volume = "523",

pages = "5315--5340",

journal = "Royal Astronomical Society. Monthly Notices",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "4",

}

RIS

TY - JOUR

T1 - Broad-emission-line dominated hydrogen-rich luminous supernovae

AU - Pessi, P. J.

AU - Anderson, J. P.

AU - Folatelli, G.

AU - Dessart, L.

AU - González-Gaitán, S.

AU - Möller, A.

AU - Gutiérrez, C. P.

AU - Mattila, S.

AU - Reynolds, T. M.

AU - Charalampopoulos, P.

AU - Filippenko, A. V.

AU - Galbany, L.

AU - Gal-Yam, A.

AU - Gromadzki, M.

AU - Hiramatsu, D.

AU - Howell, D. A.

AU - Inserra, C.

AU - Kankare, E.

AU - Lunnan, R.

AU - Martinez, L.

AU - McCully, C.

AU - Meza, N.

AU - Müller-Bravo, T. E.

AU - Nicholl, M.

AU - Pellegrino, C.

AU - Pignata, G.

AU - Sollerman, J.

AU - Tucker, B. E.

AU - Wang, X.

AU - Young, D. R.

PY - 2023/8/4

Y1 - 2023/8/4

N2 - 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.

AB - 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.

KW - SN 2017gpp

KW - SN 2017hbj

KW - SN 2017hxz

KW - SN 2018aql

KW - SN 2018eph)

KW - transients: supernovae – supernovae: individual (SN 2017cfo

U2 - 10.1093/mnras/stad1822

DO - 10.1093/mnras/stad1822

M3 - Journal article

AN - SCOPUS:85164529415

VL - 523

SP - 5315

EP - 5340

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

SN - 0035-8711

IS - 4

ER -

ID: 362685224

DAWN