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3 results on '"Type II supernovae (1731)"'

1. Supernova 2018cuf: A type iip supernova with a slow fall from plateau

Author

Lluís Galbany, Hanindyo Kuncarayakti, Lindsey Kwok, Y. Dong, Stefano Valenti, Iair Arcavi, K. A. Bostroem, Xiaofeng Wang, D. Andrew Howell, Y. Eweis, Kuntal Misra, Saurabh Jha, Michael J. Lundquist, Keiichi Maeda, S. Wyatt, Griffin Hosseinzadeh, Joseph P. Anderson, Renata Cecília Amaro, Curtis McCully, Sebastián F. Sánchez, David J. Sand, Peter J. Brown, Raya Dastidar, Nathan Smith, Vladimir Kouprianov, J. B. Haislip, Daniel E. Reichart, Jennifer E. Andrews, Jamison Burke, Daichi Hiramatsu, Eric Hsiao, Lingzhi Wang, Jacob E. Jencson, Gastón Folatelli, Jeonghee Rho, J. D. Lyman, and Scott C. Davis

Subjects
spectroscopy, photometry, 010504 meteorology & atmospheric sciences, Supernova, FOS: Physical sciences, Astrophysics, Type (model theory), Plateau (mathematics), 01 natural sciences, Spectral line, purl.org/becyt/ford/1 [https], 0103 physical sciences, Core-collapse supernovae, Core-collapse supernovae (304), Red supergiant, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Type II supernovae, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Photosphere, Degree (graph theory), Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], Light curve, Astronomía, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Type II supernovae (1731), Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present multiband photometry and spectroscopy of SN 2018cuf, a Type IIP (“P” for plateau) supernova (SN) discovered by the Distance Less Than 40 Mpc Survey within 24 hr of explosion. SN 2018cuf appears to be a typical SN IIP, with an absolute V-band magnitude of −16.73 ± 0.32 at maximum and a decline rate of 0.21 ± 0.05 mag/50 days during the plateau phase. The distance of the object was constrained to be 41.8 ± 5.7 Mpc by using the expanding photosphere method. We used spectroscopic and photometric observations from the first year after the explosion to constrain the progenitor of SN 2018cuf using both hydrodynamic light-curve modeling and late-time spectroscopic modeling. The progenitor of SN 2018cuf was most likely a red supergiant of about 14.5 M⊙ that produced 0.04 ± 0.01 M⊙ ⁵⁶Ni during the explosion. We also found ∼0.07 M⊙ of circumstellar material (CSM) around the progenitor is needed to fit the early light curves, where the CSM may originate from presupernova outbursts. During the plateau phase, high-velocity features at ∼11,000 km s⁻¹ were detected in both the optical and near-infrared spectra, supporting the possibility that the ejecta were interacting with some CSM. A very shallow slope during the postplateau phase was also observed, and it is likely due to a low degree of nickel mixing or the relatively high nickel mass in the SN., Facultad de Ciencias Astronómicas y Geofísicas, Instituto de Astrofísica de La Plata

Published
2021
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2. From Supernova to Remnant: Tracking the Evolution of the Oldest Known X-Ray Supernovae.

Author

Ramakrishnan V and Dwarkadas VV

Abstract

Core-collapse supernovae (SNe) expand into a medium created by winds from the pre-SN progenitor. The SN explosion and resulting shock wave(s) heat up the surrounding plasma, giving rise to thermal X-ray emission, which depends on the density of the emitting material. Tracking the variation of the X-ray luminosity over long periods of time thus allows for investigation of the kinematics of the SN shock waves, the structure of the surrounding medium, and the nature of the progenitor star. In this paper, X-ray observations of five of the oldest known X-ray SNe-SN 1970G, SN 1968D, SN 1959D, SN 1957D, and SN 1941C-are analyzed, with the aim of reconstructing their light curves over several decades. For those SNe for which we can extract multiepoch data, the X-ray luminosity appears to decline with time, although with large error bars. No increase in the X-ray emission from SN 1970G is found at later epochs, contrary to previous reports. All five SNe show X-ray luminosities that are of comparable magnitude. We compare the late-time X-ray luminosities of these SNe to those of supernova remnants (SNRs) in the Galaxy, which are a few hundred years old, and find that when the tentative decline is taken into account, the luminosity of the old SNe studied herein could fall below the luminosity of some of the younger SNRs within a few hundred years. However, the X-ray luminosity should begin to increase as the SNe expand in the Sedov phase, thus reaching that of the observed SNRs.

Published
2020
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3. SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries

Author

Curtis McCully, Brajesh Kumar, Róbert Szakáts, Avishay Gal-Yam, Scott C. Davis, M. J. Singh, Iair Arcavi, Kuntal Misra, Nidia Morrell, Kate Maguire, Marco Berton, S. Valenti, Lluís Galbany, Peter Milne, Anjasha Gangopadhyay, S. Chen, Mattia Bulla, Paolo A. Mazzali, Ósmar Rodríguez, G. C. Anupama, Huijuan Wang, D. K. Sahu, Ferdinando Patat, G. Pignata, Jamison Burke, Mark M. Phillips, Maximilian Stritzinger, Stephen J. Smartt, Chris Ashall, Matt Nicholl, Jay Strader, Jun Mo, Nancy Elias-Rosa, Junbo Zhang, Danfeng Xiang, Christa Gall, Jennifer E. Andrews, Hanindyo Kuncarayakti, F. Olivares, J. B. Haislip, S. J. Prentice, D. E. Reichart, Griffin Hosseinzadeh, Han Lin, Morgan Fraser, Daichi Hiramatsu, John C Wheeler, S. Benetti, D. R. Young, Raya Dastidar, Peter J. Brown, P. Ochner, Melissa Shahbandeh, Enrico Congiu, Liming Rui, O. Yaron, Pankaj Sanwal, Krisztián Sárneczky, Mariusz Gromadzki, David J. Sand, Erkki Kankare, Laura Chomiuk, Aleksandar Cikota, B. Cseh, A. Pastorello, Vladimir Kouprianov, K. A. Bostroem, Tamar Faran, S. Wyatt, Leonardo Tartaglia, Eric Hsiao, D. A. Howell, Nathan Smith, Jozsef Vinko, Xiaofeng Wang, Lingzhi Wang, A. Reguitti, Cosimo Inserra, Xue Li, Avinash Singh, ITA, USA, GBR, DEU, ESP, CHL, DNK, FIN, IND, IRL, ISR, POL, CHN, RUS, SWE, HUN, University of Arizona, University of California Davis, Aryabhatta Research Institute of Observational Sciences, Indian Institute of Astrophysics, University of California Santa Barbara, Texas A&M University, Harvard University, Hungarian Academy of Sciences, Tel Aviv University, Florida State University, INAF - Osservatorio Astronomico di Padova, Metsähovi Radio Observatory, Stockholm University, Michigan State University, Lawrence Berkeley National Laboratory, Osservatorio Astronomico di Brera, CSIC, Hebrew University of Jerusalem, University College Dublin, University of Pittsburgh, Niels Bohr Institute, Weizmann Institute of Science, University of Warsaw, University of North Carolina at Chapel Hill, Cardiff University, University of Turku, Tsinghua University, Trinity College Dublin, Liverpool John Moores University, Carnegie Institution for Science, University of Edinburgh, Universidad de Atacama, European Southern Observatory, Millennium Institute of Astrophysics (MAS), Queen's University Belfast, Aarhus University, KTH Royal Institute of Technology, CAS - National Astronomical Observatories, University of Texas at Austin, Aalto-yliopisto, and Aalto University

Subjects
Type II supernovae (1731), Core-collapse supernovae (304), Massive stars (732), astro-ph.SR, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astronomy & Astrophysics, Atomic, 01 natural sciences, 7. Clean energy, NO, Luminosity, Particle and Plasma Physics, Massive stars, 0103 physical sciences, Core-collapse supernovae, Nuclear, Red supergiant, Astronomy and Astrophysics Programme, Emission spectrum, Ejecta, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), QC, 0105 earth and related environmental sciences, QB, Type II supernovae, astro-ph.HE, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Molecular, Astronomy and Astrophysics, Light curve, Supernova, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Energy source, Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
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., Comment: Submitted to ApJ, 25 pages, plus Appendix

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