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; G. Hosseinzadeh; S. Wyatt; J. Vinko; G. C. Anupama; I. Arcavi; Chris Ashall; S. Benetti; Marco Berton; K. A. Bostroem; M. Bulla; J. Burke; L. Chomiuk; A. Cikota; E. Congiu; B. Cseh; Scott Davis; N. Elias-Rosa; 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; P. Mazzali; C. McCully; P. Milne; Jun Mo; N. Morrell; M. Nicholl; P. Ochner; F. Olivares; A. Pastorello; F. Patat; M. Phillips; G. Pignata; A. Reguitti; D. E. Reichart; Ó. 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 Xang; O. Yaron; D. R. Young; Junbo Zhang

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, G. Hosseinzadeh, S. Wyatt, J. Vinko, G. C. Anupama, I. Arcavi, Chris Ashall, S. Benetti, Marco Berton, K. A. Bostroem, M. Bulla, J. BurkeL. Chomiuk, A. Cikota, E. Congiu, B. Cseh, Scott Davis, N. Elias-Rosa, 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, P. Mazzali, C. McCully, P. Milne, Jun Mo, N. Morrell, M. Nicholl, P. Ochner, F. Olivares, A. Pastorello, F. Patat, M. Phillips, G. Pignata, A. Reguitti, D. E. Reichart, Ó. 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 Xang, O. Yaron, D. R. Young, Junbo Zhang

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

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Abstract

We present high-cadence ultraviolet (UV), optical, and near-infrared (NIR) 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 lightcurve 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 lightcurve indicates a ~500R$_{\odot}$ progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate up to 0.130 $\pm$ 0.026 M$_{\odot}$ of $^{56}$Ni are present, if the lightcurve is solely powered by radioactive decay, although the $^{56}$Ni mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multi-peaked emission lines of H$\alpha$ 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 two 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	Undefined/Unknown
Journal	The Astrophysical Journal
Publication status	Published - 01 Jul 2019

Bibliographical note

Submitted to ApJ, 25 pages, plus Appendix

Keywords

astro-ph.HE
astro-ph.SR

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SN 2017gmr : An energetic Type II-P supernova with asymmetries
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Andrews, Jennifer E. ; Sand, D. J. ; Valenti, S. ; Smith, Nathan ; Dastidar, Raya ; Sahu, D. K. ; Misra, Kuntal ; Singh, Avinash ; Hiramatsu, D. ; Hosseinzadeh, G. ; Wyatt, S. ; Vinko, J. ; Anupama, G. C. ; Arcavi, I. ; Ashall, Chris ; Benetti, S. ; Berton, Marco ; Bostroem, K. A. ; Bulla, M. ; Burke, J. ; Chomiuk, L. ; Cikota, A. ; Congiu, E. ; Cseh, B. ; Davis, Scott ; Elias-Rosa, N. ; Fraser, Morgan ; Galbany, L. ; Gall, C. ; Gal-Yam, A. ; Gangopadhyay, Anjasha ; Gromadzki, M. ; Haislip, J. ; Howell, D. A. ; Hsiao, E. Y. ; Inserra, C. ; Kankare, E. ; Kuncarayakti, H. ; Kouprianov, V. ; Kumar, Brajesh ; Li, Xue ; Lin, Han ; Mazzali, P. ; McCully, C. ; Milne, P. ; Mo, Jun ; Morrell, N. ; Nicholl, M. ; Ochner, P. ; Olivares, F. ; Pastorello, A. ; Patat, F. ; Phillips, M. ; Pignata, G. ; Reguitti, A. ; Reichart, D. E. ; Rodríguez, Ó. ; Rui, Liming ; Sanwal, Pankaj ; Sárneczky, K. ; Shahbandeh, M. ; Singh, Mridweeka ; Smartt, S. ; Strader, J. ; Stritzinger, M. D. ; Szakáts, R. ; Tartaglia, L. ; Wang, Huijuan ; Wang, Lingzhi ; Wang, Xiaofeng ; Wheeler, J. C. ; Xang, Danfeng ; Yaron, O. ; Young, D. R. ; Zhang, Junbo. / SN 2017gmr : An energetic Type II-P supernova with asymmetries. In: The Astrophysical Journal. 2019.

@article{d5f98553ca13483c92191563e1f4c77a,

title = "SN 2017gmr : An energetic Type II-P supernova with asymmetries",

abstract = " We present high-cadence ultraviolet (UV), optical, and near-infrared (NIR) 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 lightcurve 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 lightcurve indicates a ~500R$_{\odot}$ progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate up to 0.130 $\pm$ 0.026 M$_{\odot}$ of $^{56}$Ni are present, if the lightcurve is solely powered by radioactive decay, although the $^{56}$Ni mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multi-peaked emission lines of H$\alpha$ 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 two 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 = "astro-ph.HE, astro-ph.SR",

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 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 L. Chomiuk and A. Cikota and E. Congiu and B. Cseh and Scott Davis and N. Elias-Rosa 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 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 A. Reguitti and Reichart, {D. E.} and {\'O}. 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 Xang and O. Yaron and Young, {D. R.} and Junbo Zhang",

note = "Submitted to ApJ, 25 pages, plus Appendix",

year = "2019",

month = jul,

day = "1",

language = "Undefined/Unknown",

journal = "The Astrophysical Journal",

issn = "0004-637X",

publisher = "IOP Publishing Ltd.",

}

Andrews, JE, Sand, DJ, Valenti, S, Smith, N, Dastidar, R, Sahu, DK, Misra, K, Singh, A, Hiramatsu, D, Hosseinzadeh, G, Wyatt, S, Vinko, J, Anupama, GC, Arcavi, I, Ashall, C, Benetti, S, Berton, M, Bostroem, KA, Bulla, M, Burke, J, Chomiuk, L, Cikota, A, Congiu, E, Cseh, B, Davis, S, Elias-Rosa, N, 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, Mazzali, P, McCully, C, Milne, P, Mo, J, Morrell, N, Nicholl, M, Ochner, P, Olivares, F, Pastorello, A, Patat, F, Phillips, M, Pignata, G, Reguitti, A, Reichart, DE, Rodríguez, Ó, 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, Xang, D, Yaron, O, Young, DR & Zhang, J 2019, 'SN 2017gmr : An energetic Type II-P supernova with asymmetries', The Astrophysical Journal.

SN 2017gmr : An energetic Type II-P supernova with asymmetries. / Andrews, Jennifer E.; Sand, D. J.; Valenti, S.; Smith, Nathan; Dastidar, Raya; Sahu, D. K.; Misra, Kuntal; Singh, Avinash; Hiramatsu, D.; Hosseinzadeh, G.; Wyatt, S.; Vinko, J.; Anupama, G. C.; Arcavi, I.; Ashall, Chris; Benetti, S.; Berton, Marco; Bostroem, K. A.; Bulla, M.; Burke, J.; Chomiuk, L.; Cikota, A.; Congiu, E.; Cseh, B.; Davis, Scott; Elias-Rosa, N.; Fraser, Morgan; Galbany, L.; Gall, C.; Gal-Yam, A.; Gangopadhyay, Anjasha; Gromadzki, M.; Haislip, J.; Howell, D. A.; Hsiao, E. Y.; Inserra, C.; Kankare, E.; Kuncarayakti, H.; Kouprianov, V.; Kumar, Brajesh; Li, Xue; Lin, Han; Mazzali, P.; McCully, C.; Milne, P.; Mo, Jun; Morrell, N.; Nicholl, M.; Ochner, P.; Olivares, F.; Pastorello, A.; Patat, F.; Phillips, M.; Pignata, G.; Reguitti, A.; Reichart, D. E.; Rodríguez, Ó.; Rui, Liming; Sanwal, Pankaj; Sárneczky, K.; Shahbandeh, M.; Singh, Mridweeka; Smartt, S.; Strader, J.; Stritzinger, M. D.; Szakáts, R.; Tartaglia, L.; Wang, Huijuan; Wang, Lingzhi; Wang, Xiaofeng; Wheeler, J. C.; Xang, Danfeng; Yaron, O.; Young, D. R.; Zhang, Junbo.

In: The Astrophysical Journal, 01.07.2019.

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

TY - JOUR

T1 - SN 2017gmr : 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 - 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 - Chomiuk, L.

AU - Cikota, A.

AU - Congiu, E.

AU - Cseh, B.

AU - Davis, Scott

AU - Elias-Rosa, N.

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 - 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 - Reguitti, A.

AU - Reichart, D. E.

AU - Rodríguez, Ó.

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 - Xang, Danfeng

AU - Yaron, O.

AU - Young, D. R.

AU - Zhang, Junbo

N1 - Submitted to ApJ, 25 pages, plus Appendix

PY - 2019/7/1

Y1 - 2019/7/1

N2 - We present high-cadence ultraviolet (UV), optical, and near-infrared (NIR) 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 lightcurve 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 lightcurve indicates a ~500R$_{\odot}$ progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate up to 0.130 $\pm$ 0.026 M$_{\odot}$ of $^{56}$Ni are present, if the lightcurve is solely powered by radioactive decay, although the $^{56}$Ni mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multi-peaked emission lines of H$\alpha$ 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 two 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 ultraviolet (UV), optical, and near-infrared (NIR) 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 lightcurve 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 lightcurve indicates a ~500R$_{\odot}$ progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate up to 0.130 $\pm$ 0.026 M$_{\odot}$ of $^{56}$Ni are present, if the lightcurve is solely powered by radioactive decay, although the $^{56}$Ni mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multi-peaked emission lines of H$\alpha$ 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 two 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 - astro-ph.HE

KW - astro-ph.SR

M3 - Article

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

ER -