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

Tutkimustuotos: Lehtiartikkeli

Tutkijat

  • 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
  • Ja 60 muuta
  • 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

Organisaatiot

  • University of Arizona
  • University of California at Davis
  • Aryabhatta Research Institute of Observational Sciences
  • University of Delhi
  • Indian Institute of Astrophysics
  • Indian Institute of Science Bangalore
  • University of California at Santa Barbara
  • Texas A and M University
  • Harvard University
  • Hungarian Academy of Sciences
  • University of Texas at Austin
  • Tel Aviv University
  • Florida State University
  • INAF - Osservatorio Astronomico di Padova
  • University of Turku
  • Stockholm University
  • Guangzhou University
  • Michigan State University
  • Lawrence Berkeley National Laboratory
  • Osservatorio Astronomico di Brera
  • CSIC
  • Institute of Space Studies of Catalonia
  • Hebrew University of Jerusalem
  • University College Dublin
  • University of Pittsburgh
  • Niels Bohr Institute
  • Weizmann Institute of Science
  • Pt. Ravishankar Shukla University
  • University of Warsaw
  • University of North Carolina
  • Cardiff University
  • RAS - Pulkovo Astronomical Observatory
  • Tsinghua University
  • Trinity College Dublin
  • Liverpool John Moores University
  • Max Planck Institute for Astrophysics
  • University of Edinburgh
  • Universidad de Atacama
  • European Southern Observatory
  • Queen's University Belfast
  • Aarhus University
  • Royal Institute of Technology
  • CAS - National Astronomical Observatories
  • Las Cumbres Observatory
  • Observatories of the Carnegie Institution for Science
  • Millennium Institute of Astrophysics (MAS)
  • Universidad Andrés Bello
  • CASSACA: Chinese Academy of Sciences South America Center for Astronomy

Kuvaus

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.

Yksityiskohdat

AlkuperäiskieliEnglanti
Artikkeli43
JulkaisuAstrophysical Journal
Vuosikerta885
Numero1
TilaJulkaistu - 1 marraskuuta 2019
OKM-julkaisutyyppiA1 Julkaistu artikkeli, soviteltu

ID: 39179903