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. Wyatt; J. Vinko; G. C. Anupama; I. Arcavi; Chris Ashall; S. Benetti; Marco Berton; K. A. Bostroem; M. Bulla; J. Burke; 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; J. Haislip; D. A. Howell; E. Y. Hsiao; C. Inserra; E. Kankare; H. Kuncarayakti; V. Kouprianov; Brajesh Kumar; Xue Li; Han Lin; K. Maguire; P. Mazzali; C. McCully; P. Milne; Jun Mo; N. Morrell; M. Nicholl; P. Ochner; F. Olivares; A. Pastorello; F. Patat; M. Phillips; G. Pignata; S. Prentice; A. Reguitti; D. E. Reichart; Rodríguez; Liming Rui; Pankaj Sanwal; K. Sárneczky; M. Shahbandeh; Mridweeka Singh; S. Smartt; J. Strader; M. D. Stritzinger; R. Szakáts; L. Tartaglia; Huijuan Wang; Lingzhi Wang; Xiaofeng Wang; 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. Wyatt, J. Vinko, G. C. Anupama, I. Arcavi, Chris Ashall, S. Benetti, Marco Berton, K. A. Bostroem, M. BullaJ. Burke, 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, J. Haislip, D. A. Howell, E. Y. Hsiao, C. Inserra, E. Kankare, H. Kuncarayakti, V. Kouprianov, Brajesh Kumar, Xue Li, Han Lin, K. Maguire, P. Mazzali, C. McCully, P. Milne, Jun Mo, N. Morrell, M. Nicholl, P. Ochner, F. Olivares, A. Pastorello, F. Patat, M. Phillips, G. Pignata, S. Prentice, A. Reguitti, D. E. Reichart, Rodríguez, Liming Rui, Pankaj Sanwal, K. Sárneczky, M. Shahbandeh, Mridweeka Singh, S. Smartt, J. Strader, M. D. Stritzinger, R. Szakáts, L. Tartaglia, Huijuan Wang, Lingzhi Wang, Xiaofeng Wang, J. C. Wheeler, Danfeng Xiang, O. Yaron, D. R. Young, Junbo Zhang

Research output: Contribution to journal › Article › peer-review

40 Scopus citations

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.

Original language	English (US)
Article number	43
Journal	Astrophysical Journal
Volume	885
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/ab43e3
State	Published - Nov 1 2019

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4357/ab43e3

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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., Wyatt, S., Vinko, J., Anupama, G. C., Arcavi, I., Ashall, C., Benetti, S., Berton, M., Bostroem, K. A., ... Zhang, J. (2019). SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries. Astrophysical Journal, 885(1), Article 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, Wyatt, S, Vinko, J, Anupama, GC, Arcavi, I, Ashall, C, Benetti, S, Berton, M, Bostroem, KA, Bulla, M, Burke, J, 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, Haislip, J, Howell, DA, Hsiao, EY, Inserra, C, Kankare, E, Kuncarayakti, H, Kouprianov, V, Kumar, B, Li, X, Lin, H, Maguire, K, Mazzali, P, McCully, C, Milne, P, Mo, J, Morrell, N, Nicholl, M, Ochner, P, Olivares, F, Pastorello, A, Patat, F, Phillips, M, Pignata, G, Prentice, S, Reguitti, A, Reichart, DE, Rodríguez, Rui, L, Sanwal, P, Sárneczky, K, Shahbandeh, M, Singh, M, Smartt, S, Strader, J, Stritzinger, MD, Szakáts, R, Tartaglia, L, Wang, H, Wang, L, Wang, X, Wheeler, JC, Xiang, D, Yaron, O, Young, DR & Zhang, J 2019, 'SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries', Astrophysical Journal, vol. 885, no. 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.",

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. Wyatt and J. Vinko and Anupama, {G. C.} and I. Arcavi and Chris Ashall and S. Benetti and Marco Berton and Bostroem, {K. A.} and M. Bulla and J. Burke 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 J. Haislip and Howell, {D. A.} and Hsiao, {E. Y.} and C. Inserra and E. Kankare and H. Kuncarayakti and V. Kouprianov and Brajesh Kumar and Xue Li and Han Lin and K. Maguire and P. Mazzali and C. McCully and P. Milne and Jun Mo and N. Morrell and M. Nicholl and P. Ochner and F. Olivares and A. Pastorello and F. Patat and M. Phillips and G. Pignata and S. Prentice and A. Reguitti and Reichart, {D. E.} and Rodr{\'i}guez and Liming Rui and Pankaj Sanwal and K. S{\'a}rneczky and M. Shahbandeh and Mridweeka Singh and S. Smartt and J. Strader and Stritzinger, {M. D.} and R. Szak{\'a}ts and L. Tartaglia and Huijuan Wang and Lingzhi Wang and Xiaofeng Wang and Wheeler, {J. C.} and Danfeng Xiang and O. Yaron and Young, {D. R.} and Junbo Zhang",

year = "2019",

month = nov,

day = "1",

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

language = "English (US)",

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journal = "Astrophysical Journal",

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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 - Wyatt, S.

AU - Vinko, J.

AU - Anupama, G. C.

AU - Arcavi, I.

AU - Ashall, Chris

AU - Benetti, S.

AU - Berton, Marco

AU - Bostroem, K. A.

AU - Bulla, M.

AU - Burke, J.

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 - Haislip, J.

AU - Howell, D. A.

AU - Hsiao, E. Y.

AU - Inserra, C.

AU - Kankare, E.

AU - Kuncarayakti, H.

AU - Kouprianov, V.

AU - Kumar, Brajesh

AU - Li, Xue

AU - Lin, Han

AU - Maguire, K.

AU - Mazzali, P.

AU - McCully, C.

AU - Milne, P.

AU - Mo, Jun

AU - Morrell, N.

AU - Nicholl, M.

AU - Ochner, P.

AU - Olivares, F.

AU - Pastorello, A.

AU - Patat, F.

AU - Phillips, M.

AU - Pignata, G.

AU - Prentice, S.

AU - Reguitti, A.

AU - Reichart, D. E.

AU - Rodríguez,

AU - Rui, Liming

AU - Sanwal, Pankaj

AU - Sárneczky, K.

AU - Shahbandeh, M.

AU - Singh, Mridweeka

AU - Smartt, S.

AU - Strader, J.

AU - Stritzinger, M. D.

AU - Szakáts, R.

AU - Tartaglia, L.

AU - Wang, Huijuan

AU - Wang, Lingzhi

AU - Wang, Xiaofeng

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.

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DO - 10.3847/1538-4357/ab43e3

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VL - 885

JO - Astrophysical Journal

JF - Astrophysical Journal

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ER -

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

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UBVRI & ugriz photometry of supernova SN 2017gmr

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

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ASJC Scopus subject areas

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UBVRI &amp; ugriz photometry of supernova SN 2017gmr

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UBVRI & ugriz photometry of supernova SN 2017gmr