SN2018fif: The explosion of a large red supergiant discovered in its infancy by the Zwicky Transient Facility

Maayane T. Soumagnac; Noam Ganot; Avishay Gal-yam; Eran O. Ofek; Ofer Yaron; Eli Waxman; Steve Schulze; Yi Yang; Adam Rubin; S. Bradley Cenko; Jesper Sollerman; Daniel A. Perley; Christoffer Fremling; Peter Nugent; James D. Neill; Emir Karamehmetoglu; Eric C. Bellm; Rachel J. Bruch; Rick Burruss; Virginia Cunningham; Richard Dekany; V. Zach Golkhou; Ido Irani; Mansi M. Kasliwal; Nicholas P Konidaris; Shrinivas R. Kulkarni; Thomas Kupfer; Russ R. Laher; Frank J. Masci; Jonathan Morag; Reed Riddle; Mickael Rigault; Ben Rusholme; Jan van Roestel; Barak Zackay

SN2018fif: The explosion of a large red supergiant discovered in its infancy by the Zwicky Transient Facility

Maayane T. Soumagnac, Noam Ganot, Avishay Gal-yam, Eran O. Ofek, Ofer Yaron, Eli Waxman, Steve Schulze, Yi Yang, Adam Rubin, S. Bradley Cenko, Jesper Sollerman, Daniel A. Perley, Christoffer Fremling, Peter Nugent, James D. Neill, Emir Karamehmetoglu, Eric C. Bellm, Rachel J. Bruch, Rick Burruss, Virginia CunninghamRichard Dekany, V. Zach Golkhou, Ido Irani, Mansi M. Kasliwal, Nicholas P Konidaris, Shrinivas R. Kulkarni, Thomas Kupfer, Russ R. Laher, Frank J. Masci, Jonathan Morag, Reed Riddle, Mickael Rigault, Ben Rusholme, Jan van Roestel, Barak Zackay

Weizmann Institute of Science

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Abstract

High cadence transient surveys are able to capture supernovae closer to their first light than before. Applying analytical models to such early emission, we can constrain the progenitor stars properties. In this paper, we present observations of SN2018fif (ZTF18abokyfk). The supernova was discovered close to first light and monitored by the Zwicky Transient Facility (ZTF) and the Neil Gehrels Swift Observatory. Early spectroscopic observations suggest that the progenitor of SN2018fif was surrounded by relatively small amounts of circumstellar material (CSM) compared to all previous cases. This particularity, coupled with the high cadence multiple-band coverage, makes it a good candidate to investigate using shock-cooling models. We employ the SOPRANOS code, an implementation of the model by Sapir & Waxman (2017). Compared with previous implementations, SOPRANOS has the advantage of including a careful account of the limited temporal validity domain of the shock-cooling model. We find that the progenitor of SN2018fif was a large red supergiant, with a radius of R=1174_{-81}^{+208} solar radii, and an ejected mass of M=5.6_{-1.0}^{+9.1} solar masses. Our model also gives information on the explosion epoch, the progenitor inner structure, the shock velocity and the extinction. The large radius differs from previously modeled objects, and the difference could be either intrinsic or due to the relatively small amount of CSM around SN2018fif, perhaps making it a "cleaner" candidate for applying shock-cooling analytical models.

Original language	English
Number of pages	14
Journal	arXiv
State	Published - 25 Jul 2019

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Soumagnac, M. T., Ganot, N., Gal-yam, A., Ofek, E. O., Yaron, O., Waxman, E., Schulze, S., Yang, Y., Rubin, A., Cenko, S. B., Sollerman, J., Perley, D. A., Fremling, C., Nugent, P., Neill, J. D., Karamehmetoglu, E., Bellm, E. C., Bruch, R. J., Burruss, R., ... Zackay, B. (2019). SN2018fif: The explosion of a large red supergiant discovered in its infancy by the Zwicky Transient Facility. arXiv. https://arxiv.org/abs/1907.11252

@article{ecba810338104374b4ea33ec48b74474,

title = "SN2018fif: The explosion of a large red supergiant discovered in its infancy by the Zwicky Transient Facility",

abstract = "High cadence transient surveys are able to capture supernovae closer to their first light than before. Applying analytical models to such early emission, we can constrain the progenitor stars properties. In this paper, we present observations of SN2018fif (ZTF18abokyfk). The supernova was discovered close to first light and monitored by the Zwicky Transient Facility (ZTF) and the Neil Gehrels Swift Observatory. Early spectroscopic observations suggest that the progenitor of SN2018fif was surrounded by relatively small amounts of circumstellar material (CSM) compared to all previous cases. This particularity, coupled with the high cadence multiple-band coverage, makes it a good candidate to investigate using shock-cooling models. We employ the SOPRANOS code, an implementation of the model by Sapir \& Waxman (2017). Compared with previous implementations, SOPRANOS has the advantage of including a careful account of the limited temporal validity domain of the shock-cooling model. We find that the progenitor of SN2018fif was a large red supergiant, with a radius of R=1174\_\{-81\}\textasciicircum{}\{+208\} solar radii, and an ejected mass of M=5.6\_\{-1.0\}\textasciicircum{}\{+9.1\} solar masses. Our model also gives information on the explosion epoch, the progenitor inner structure, the shock velocity and the extinction. The large radius differs from previously modeled objects, and the difference could be either intrinsic or due to the relatively small amount of CSM around SN2018fif, perhaps making it a {"}cleaner{"} candidate for applying shock-cooling analytical models.",

author = "Soumagnac, \{Maayane T.\} and Noam Ganot and Avishay Gal-yam and Ofek, \{Eran O.\} and Ofer Yaron and Eli Waxman and Steve Schulze and Yi Yang and Adam Rubin and Cenko, \{S. Bradley\} and Jesper Sollerman and Perley, \{Daniel A.\} and Christoffer Fremling and Peter Nugent and Neill, \{James D.\} and Emir Karamehmetoglu and Bellm, \{Eric C.\} and Bruch, \{Rachel J.\} and Rick Burruss and Virginia Cunningham and Richard Dekany and Golkhou, \{V. Zach\} and Ido Irani and Kasliwal, \{Mansi M.\} and Konidaris, \{Nicholas P\} and Kulkarni, \{Shrinivas R.\} and Thomas Kupfer and Laher, \{Russ R.\} and Masci, \{Frank J.\} and Jonathan Morag and Reed Riddle and Mickael Rigault and Ben Rusholme and Roestel, \{Jan van\} and Barak Zackay",

note = "We dedicate this paper to the memory of Rona Ramon. M.T.S. acknowledges support by a grant from IMOS/ISA, the Ilan Ramon fellowship from the Israel Ministry of Science and Technology and the Benoziyo center for Astrophysics at the Weizmann Institute of Science. E.O.O is grateful for the support by grants from the Israel Science Foundation, Minerva, Israeli Ministry of Science, the US-Israel Binational Science Foundation, the Weizmann Institute and the I-CORE Program of the Planning and Budgeting Committee and the Israel Science Foundation. A.G.-Y. is supported by the EU via ERC grant No. 725161, the Quantum Universe I-Core program, the ISF, the BSF Transformative program, IMOS via ISA and by a Kimmel award. The data presented here are based - in part - on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. We acknowledge the use of public data from the Swift data archive. SED Machine is based upon work supported by the National Science Foundation under Grant No. 1106171 The data presented here were obtained - in part - with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA.The Liverpool Telescope, located on the island of La Palma in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, is operated by Liverpool John Moores University with financial support from the UK Science and Technology Facilities Council.The ACAM spectroscopy was obtained as part of OPT/2018B/011.",

year = "2019",

month = jul,

day = "25",

language = "الإنجليزيّة",

}

Soumagnac, MT, Ganot, N, Gal-yam, A , Ofek, EO, Yaron, O, Waxman, E, Schulze, S, Yang, Y, Rubin, A, Cenko, SB, Sollerman, J, Perley, DA, Fremling, C, Nugent, P, Neill, JD, Karamehmetoglu, E, Bellm, EC, Bruch, RJ, Burruss, R, Cunningham, V, Dekany, R, Golkhou, VZ, Irani, I, Kasliwal, MM, Konidaris, NP, Kulkarni, SR, Kupfer, T, Laher, RR, Masci, FJ, Morag, J, Riddle, R, Rigault, M, Rusholme, B, Roestel, JV & Zackay, B 2019, 'SN2018fif: The explosion of a large red supergiant discovered in its infancy by the Zwicky Transient Facility', arXiv. <https://arxiv.org/abs/1907.11252>

TY - JOUR

T1 - SN2018fif

T2 - The explosion of a large red supergiant discovered in its infancy by the Zwicky Transient Facility

AU - Soumagnac, Maayane T.

AU - Ganot, Noam

AU - Gal-yam, Avishay

AU - Ofek, Eran O.

AU - Yaron, Ofer

AU - Waxman, Eli

AU - Schulze, Steve

AU - Yang, Yi

AU - Rubin, Adam

AU - Cenko, S. Bradley

AU - Sollerman, Jesper

AU - Perley, Daniel A.

AU - Fremling, Christoffer

AU - Nugent, Peter

AU - Neill, James D.

AU - Karamehmetoglu, Emir

AU - Bellm, Eric C.

AU - Bruch, Rachel J.

AU - Burruss, Rick

AU - Cunningham, Virginia

AU - Dekany, Richard

AU - Golkhou, V. Zach

AU - Irani, Ido

AU - Kasliwal, Mansi M.

AU - Konidaris, Nicholas P

AU - Kulkarni, Shrinivas R.

AU - Kupfer, Thomas

AU - Laher, Russ R.

AU - Masci, Frank J.

AU - Morag, Jonathan

AU - Riddle, Reed

AU - Rigault, Mickael

AU - Rusholme, Ben

AU - Roestel, Jan van

AU - Zackay, Barak

N1 - We dedicate this paper to the memory of Rona Ramon. M.T.S. acknowledges support by a grant from IMOS/ISA, the Ilan Ramon fellowship from the Israel Ministry of Science and Technology and the Benoziyo center for Astrophysics at the Weizmann Institute of Science. E.O.O is grateful for the support by grants from the Israel Science Foundation, Minerva, Israeli Ministry of Science, the US-Israel Binational Science Foundation, the Weizmann Institute and the I-CORE Program of the Planning and Budgeting Committee and the Israel Science Foundation. A.G.-Y. is supported by the EU via ERC grant No. 725161, the Quantum Universe I-Core program, the ISF, the BSF Transformative program, IMOS via ISA and by a Kimmel award. The data presented here are based - in part - on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. We acknowledge the use of public data from the Swift data archive. SED Machine is based upon work supported by the National Science Foundation under Grant No. 1106171 The data presented here were obtained - in part - with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA.The Liverpool Telescope, located on the island of La Palma in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, is operated by Liverpool John Moores University with financial support from the UK Science and Technology Facilities Council.The ACAM spectroscopy was obtained as part of OPT/2018B/011.

PY - 2019/7/25

Y1 - 2019/7/25

N2 - High cadence transient surveys are able to capture supernovae closer to their first light than before. Applying analytical models to such early emission, we can constrain the progenitor stars properties. In this paper, we present observations of SN2018fif (ZTF18abokyfk). The supernova was discovered close to first light and monitored by the Zwicky Transient Facility (ZTF) and the Neil Gehrels Swift Observatory. Early spectroscopic observations suggest that the progenitor of SN2018fif was surrounded by relatively small amounts of circumstellar material (CSM) compared to all previous cases. This particularity, coupled with the high cadence multiple-band coverage, makes it a good candidate to investigate using shock-cooling models. We employ the SOPRANOS code, an implementation of the model by Sapir & Waxman (2017). Compared with previous implementations, SOPRANOS has the advantage of including a careful account of the limited temporal validity domain of the shock-cooling model. We find that the progenitor of SN2018fif was a large red supergiant, with a radius of R=1174_{-81}^{+208} solar radii, and an ejected mass of M=5.6_{-1.0}^{+9.1} solar masses. Our model also gives information on the explosion epoch, the progenitor inner structure, the shock velocity and the extinction. The large radius differs from previously modeled objects, and the difference could be either intrinsic or due to the relatively small amount of CSM around SN2018fif, perhaps making it a "cleaner" candidate for applying shock-cooling analytical models.

AB - High cadence transient surveys are able to capture supernovae closer to their first light than before. Applying analytical models to such early emission, we can constrain the progenitor stars properties. In this paper, we present observations of SN2018fif (ZTF18abokyfk). The supernova was discovered close to first light and monitored by the Zwicky Transient Facility (ZTF) and the Neil Gehrels Swift Observatory. Early spectroscopic observations suggest that the progenitor of SN2018fif was surrounded by relatively small amounts of circumstellar material (CSM) compared to all previous cases. This particularity, coupled with the high cadence multiple-band coverage, makes it a good candidate to investigate using shock-cooling models. We employ the SOPRANOS code, an implementation of the model by Sapir & Waxman (2017). Compared with previous implementations, SOPRANOS has the advantage of including a careful account of the limited temporal validity domain of the shock-cooling model. We find that the progenitor of SN2018fif was a large red supergiant, with a radius of R=1174_{-81}^{+208} solar radii, and an ejected mass of M=5.6_{-1.0}^{+9.1} solar masses. Our model also gives information on the explosion epoch, the progenitor inner structure, the shock velocity and the extinction. The large radius differs from previously modeled objects, and the difference could be either intrinsic or due to the relatively small amount of CSM around SN2018fif, perhaps making it a "cleaner" candidate for applying shock-cooling analytical models.

M3 - مقالة

SN - 2331-8422

JO - arXiv

JF - arXiv

ER -

SN2018fif: The explosion of a large red supergiant discovered in its infancy by the Zwicky Transient Facility

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