SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries

Jennifer E. Andrews; D. J. Sand; S. Valenti; Nathan Smith; Raya Dastidar; D. K. Sahu; Kuntal Misra; Avinash Singh; D. Hiramatsu; P. J. Brown; G. Hosseinzadeh; S. Chen; L. Chomiuk; A. Cikota; E. Congiu; B. Cseh; Scott Davis; N. Elias-Rosa; T. Faran; Morgan Fraser; L. Galbany; C. Gall; A. Gal-Yam; Anjasha Gangopadhyay; M. Gromadzki; C. Inserra; E. Kankare; H. Kuncarayakti; V. Kouprianov; Pankaj Sanwal; K. Sarneczky; M. Shahbandeh; Mridweeka Singh; S. Smartt; J. Strader; M. D. Stritzinger; J. C. Wheeler; Danfeng Xiang; O. Yaron; D. R. Young; Junbo Zhang

doi:10.3847/1538-4357/ab43e3

SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries

Jennifer E. Andrews, D. J. Sand, S. Valenti, Nathan Smith, Raya Dastidar, D. K. Sahu, Kuntal Misra, Avinash Singh, D. Hiramatsu, P. J. Brown, G. Hosseinzadeh, S. Chen, L. Chomiuk, A. Cikota, E. Congiu, B. Cseh, Scott Davis, N. Elias-Rosa, T. Faran, Morgan FraserL. Galbany, C. Gall, A. Gal-Yam, Anjasha Gangopadhyay, M. Gromadzki, C. Inserra, E. Kankare, H. Kuncarayakti, V. Kouprianov, Pankaj Sanwal, K. Sarneczky, M. Shahbandeh, Mridweeka Singh, S. Smartt, J. Strader, M. D. Stritzinger, J. C. Wheeler, Danfeng Xiang, O. Yaron, D. R. Young, Junbo Zhang

DARK

9 Citationer (Scopus)

Abstract

We present high-cadence UV, optical, and near-infrared data on the luminous Type II-P supernova SN 2017gmr from hours after discovery through the first 180 days. SN 2017gmr does not show signs of narrow, high-ionization emission lines in the early optical spectra, yet the optical light-curve evolution suggests that an extra energy source from circumstellar medium (CSM) interaction must be present for at least 2 days after explosion. Modeling of the early light curve indicates a ∼500 R _o progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate that up to 0.130 ± 0.026 M _o of ⁵⁶Ni are present, if the light curve is solely powered by radioactive decay, although the ⁵⁶Ni mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multipeaked emission lines of Hα and [O i] emerge after day 154, as a result of either an asymmetric explosion or asymmetries in the CSM. The lack of narrow lines within the first 2 days of explosion in the likely presence of CSM interaction may be an example of close, dense, asymmetric CSM that is quickly enveloped by the spherical supernova ejecta.

Originalsprog	Engelsk
Artikelnummer	43
Tidsskrift	Astrophysical Journal
Vol/bind	885
Udgave nummer	1
Antal sider	23
ISSN	0004-637X
DOI	https://doi.org/10.3847/1538-4357/ab43e3
Status	Udgivet - 1 nov. 2019

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10.3847/1538-4357/ab43e3

https://iopscience.iop.org/article/10.3847/1538-4357/ab43e3/pdf

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Andrews, J. E., Sand, D. J., Valenti, S., Smith, N., Dastidar, R., Sahu, D. K., Misra, K., Singh, A., Hiramatsu, D., Brown, P. J., Hosseinzadeh, G., Chen, S., Chomiuk, L., Cikota, A., Congiu, E., Cseh, B., Davis, S., Elias-Rosa, N., Faran, T., ... Zhang, J. (2019). SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries. Astrophysical Journal, 885(1), [43]. https://doi.org/10.3847/1538-4357/ab43e3

Andrews, JE, Sand, DJ, Valenti, S, Smith, N, Dastidar, R, Sahu, DK, Misra, K, Singh, A, Hiramatsu, D, Brown, PJ, Hosseinzadeh, G, Chen, S, Chomiuk, L, Cikota, A, Congiu, E, Cseh, B, Davis, S, Elias-Rosa, N, Faran, T, Fraser, M, Galbany, L, Gall, C, Gal-Yam, A, Gangopadhyay, A, Gromadzki, M, Inserra, C, Kankare, E, Kuncarayakti, H, Kouprianov, V, Sanwal, P, Sarneczky, K, Shahbandeh, M, Singh, M, Smartt, S, Strader, J, Stritzinger, MD, Wheeler, JC, Xiang, D, Yaron, O, Young, DR & Zhang, J 2019, 'SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries', Astrophysical Journal, bind 885, nr. 1, 43. https://doi.org/10.3847/1538-4357/ab43e3

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title = "SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries",

abstract = "We present high-cadence UV, optical, and near-infrared data on the luminous Type II-P supernova SN 2017gmr from hours after discovery through the first 180 days. SN 2017gmr does not show signs of narrow, high-ionization emission lines in the early optical spectra, yet the optical light-curve evolution suggests that an extra energy source from circumstellar medium (CSM) interaction must be present for at least 2 days after explosion. Modeling of the early light curve indicates a ∼500 R o progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate that up to 0.130 ± 0.026 M o of 56Ni are present, if the light curve is solely powered by radioactive decay, although the 56Ni mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multipeaked emission lines of Hα and [O i] emerge after day 154, as a result of either an asymmetric explosion or asymmetries in the CSM. The lack of narrow lines within the first 2 days of explosion in the likely presence of CSM interaction may be an example of close, dense, asymmetric CSM that is quickly enveloped by the spherical supernova ejecta.",

keywords = "Type II supernovae, Core-collapse supernovae, Massive stars",

author = "Andrews, {Jennifer E.} and Sand, {D. J.} and S. Valenti and Nathan Smith and Raya Dastidar and Sahu, {D. K.} and Kuntal Misra and Avinash Singh and D. Hiramatsu and Brown, {P. J.} and G. Hosseinzadeh and S. Chen and L. Chomiuk and A. Cikota and E. Congiu and B. Cseh and Scott Davis and N. Elias-Rosa and T. Faran and Morgan Fraser and L. Galbany and C. Gall and A. Gal-Yam and Anjasha Gangopadhyay and M. Gromadzki and C. Inserra and E. Kankare and H. Kuncarayakti and V. Kouprianov and Pankaj Sanwal and K. Sarneczky and M. Shahbandeh and Mridweeka Singh and S. Smartt and J. Strader and Stritzinger, {M. D.} and Wheeler, {J. C.} and Danfeng Xiang and O. Yaron and Young, {D. R.} and Junbo Zhang",

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doi = "10.3847/1538-4357/ab43e3",

language = "English",

volume = "885",

journal = "Astrophysical Journal",

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TY - JOUR

T1 - SN 2017gmr

T2 - An Energetic Type II-P Supernova with Asymmetries

AU - Andrews, Jennifer E.

AU - Sand, D. J.

AU - Valenti, S.

AU - Smith, Nathan

AU - Dastidar, Raya

AU - Sahu, D. K.

AU - Misra, Kuntal

AU - Singh, Avinash

AU - Hiramatsu, D.

AU - Brown, P. J.

AU - Hosseinzadeh, G.

AU - Chen, S.

AU - Chomiuk, L.

AU - Cikota, A.

AU - Congiu, E.

AU - Cseh, B.

AU - Davis, Scott

AU - Elias-Rosa, N.

AU - Faran, T.

AU - Fraser, Morgan

AU - Galbany, L.

AU - Gall, C.

AU - Gal-Yam, A.

AU - Gangopadhyay, Anjasha

AU - Gromadzki, M.

AU - Inserra, C.

AU - Kankare, E.

AU - Kuncarayakti, H.

AU - Kouprianov, V.

AU - Sanwal, Pankaj

AU - Sarneczky, K.

AU - Shahbandeh, M.

AU - Singh, Mridweeka

AU - Smartt, S.

AU - Strader, J.

AU - Stritzinger, M. D.

AU - Wheeler, J. C.

AU - Xiang, Danfeng

AU - Yaron, O.

AU - Young, D. R.

AU - Zhang, Junbo

PY - 2019/11/1

Y1 - 2019/11/1

N2 - We present high-cadence UV, optical, and near-infrared data on the luminous Type II-P supernova SN 2017gmr from hours after discovery through the first 180 days. SN 2017gmr does not show signs of narrow, high-ionization emission lines in the early optical spectra, yet the optical light-curve evolution suggests that an extra energy source from circumstellar medium (CSM) interaction must be present for at least 2 days after explosion. Modeling of the early light curve indicates a ∼500 R o progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate that up to 0.130 ± 0.026 M o of 56Ni are present, if the light curve is solely powered by radioactive decay, although the 56Ni mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multipeaked emission lines of Hα and [O i] emerge after day 154, as a result of either an asymmetric explosion or asymmetries in the CSM. The lack of narrow lines within the first 2 days of explosion in the likely presence of CSM interaction may be an example of close, dense, asymmetric CSM that is quickly enveloped by the spherical supernova ejecta.

AB - We present high-cadence UV, optical, and near-infrared data on the luminous Type II-P supernova SN 2017gmr from hours after discovery through the first 180 days. SN 2017gmr does not show signs of narrow, high-ionization emission lines in the early optical spectra, yet the optical light-curve evolution suggests that an extra energy source from circumstellar medium (CSM) interaction must be present for at least 2 days after explosion. Modeling of the early light curve indicates a ∼500 R o progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate that up to 0.130 ± 0.026 M o of 56Ni are present, if the light curve is solely powered by radioactive decay, although the 56Ni mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multipeaked emission lines of Hα and [O i] emerge after day 154, as a result of either an asymmetric explosion or asymmetries in the CSM. The lack of narrow lines within the first 2 days of explosion in the likely presence of CSM interaction may be an example of close, dense, asymmetric CSM that is quickly enveloped by the spherical supernova ejecta.

KW - Type II supernovae

KW - Core-collapse supernovae

KW - Massive stars

U2 - 10.3847/1538-4357/ab43e3

DO - 10.3847/1538-4357/ab43e3

M3 - Journal article

SN - 0004-637X

VL - 885

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 43

ER -

SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries

Abstract

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