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SN 2018fif: The Explosion of a Large Red Supergiant Discovered in Its Infancy by the Zwicky Transient Facility

Soumagnac, Maayane T. and Ganot, Noam and Irani, Ido and Gal-Yam, Avishay and Ofek, Eran O. and Waxman, Eli and Morag, Jonathan and Yaron, Ofer and Schulze, Steve and Yang, Yi and Rubin, Adam and Cenko, S. Bradley and Sollerman, Jesper and Perley, Daniel A. and Fremling, Christoffer and Nugent, Peter E. and Neill, James D. and Karamehmetoglu, Emir and Bellm, Eric C. and Bruch, Rachel J. and Burruss, Rick and Cunningham, Virginia and Dekany, Richard and Golkhou, V. Zach and Graham, Matthew J. and Kasliwal, Mansi M. and Konidaris, Nicholas P. and Kulkarni, Shrinivas R. and Kupfer, Thomas and Laher, Russ R. and Masci, Frank J. and Riddle, Reed and Rigault, Mickael and Rusholme, Ben and van Roestel, Jan and Zackay, Barak (2020) SN 2018fif: The Explosion of a Large Red Supergiant Discovered in Its Infancy by the Zwicky Transient Facility. Astrophysical Journal, 902 (1). Art. No. 6. ISSN 1538-4357. doi:10.3847/1538-4357/abb247.

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High-cadence transient surveys are able to capture supernovae closer to their first light than ever before. Applying analytical models to such early emission, we can constrain the progenitor stars' properties. In this paper, we present observations of SN 2018fif (ZTF 18abokyfk). 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 SN 2018fif was surrounded by relatively small amounts of circumstellar material 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 and its extension to early times by Morag et al. Compared with previous implementations, SOPRANOS has the advantage of including a careful account of the limited temporal validity domain of the shock-cooling model as well as allowing usage of the entirety of the early UV data. We find that the progenitor of SN 2018fif was a large red supergiant with a radius of R = 744.0^(+183.0)_(-128.0) R⊙ and an ejected mass of M_(ej) = 9.3^(+0.4)_(-5.8) M⊙. Our model also gives information on the explosion epoch, the progenitor's inner structure, the shock velocity, and the extinction. The distribution of radii is double-peaked, with smaller radii corresponding to lower values of the extinction, earlier recombination times, and a better match to the early UV data. If these correlations persist in future objects, denser spectroscopic monitoring constraining the time of recombination, as well as accurate UV observations (e.g., with ULTRASAT), will help break the extinction/radius degeneracy and independently determine both.

Item Type:Article
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URLURL TypeDescription Paper
Soumagnac, Maayane T.0000-0001-6753-1488
Irani, Ido0000-0002-7996-8780
Gal-Yam, Avishay0000-0002-3653-5598
Ofek, Eran O.0000-0002-6786-8774
Waxman, Eli0000-0002-9038-5877
Yaron, Ofer0000-0002-0301-8017
Schulze, Steve0000-0001-6797-1889
Rubin, Adam0000-0003-4557-0632
Cenko, S. Bradley0000-0003-1673-970X
Sollerman, Jesper0000-0003-1546-6615
Perley, Daniel A.0000-0001-8472-1996
Fremling, Christoffer0000-0002-4223-103X
Nugent, Peter E.0000-0002-3389-0586
Neill, James D.0000-0002-0466-1119
Karamehmetoglu, Emir0000-0001-6209-838X
Bellm, Eric C.0000-0001-8018-5348
Bruch, Rachel J.0000-0001-8208-2473
Cunningham, Virginia0000-0003-2292-0441
Dekany, Richard0000-0002-5884-7867
Golkhou, V. Zach0000-0001-8205-2506
Graham, Matthew J.0000-0002-3168-0139
Kasliwal, Mansi M.0000-0002-5619-4938
Konidaris, Nicholas P.0000-0003-1905-2815
Kulkarni, Shrinivas R.0000-0001-5390-8563
Kupfer, Thomas0000-0002-6540-1484
Laher, Russ R.0000-0003-2451-5482
Masci, Frank J.0000-0002-8532-9395
Riddle, Reed0000-0002-0387-370X
Rigault, Mickael0000-0002-8121-2560
Rusholme, Ben0000-0001-7648-4142
van Roestel, Jan0000-0002-2626-2872
Zackay, Barak0000-0001-5162-9501
Alternate Title:SN2018fif: The explosion of a large red supergiant discovered in its infancy by the Zwicky Transient Facility
Additional Information:© 2020 The American Astronomical Society. Received 2019 July 24; revised 2020 August 17; accepted 2020 August 23; published 2020 October 7. 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.'s research is supported by the EU via ERC grant No. 725161, the ISF GW excellence center, an IMOS space infrastructure grant, and the BSF Transformative program as well as The Benoziyo Endowment Fund for the Advancement of Science, the Deloro Institute for Advanced Research in Space and Optics, The Veronika A. Rabl Physics Discretionary Fund, Paul and Tina Gardner, and the WIS-CIT joint research grant; A.G.Y. is the recipient of the Helen and Martin Kimmel Award for Innovative Investigation. 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. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC. 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. Software: ZTF pipeline (Masci et al. 2019), ZOGY (Zackay et al. 2016), HEAsoft (v6.26, HEASARC 2014), IRAF (Tody 1986, 1993), dynesty (Skilling 2004, 2006; Higson et al. 2019; Speagle 2020), LRIS pipeline (Perley 2019), Astropy (Astropy Collaboration et al. 2013, 2018), Matplotlib (Hunter 2007), Scipy (Virtanen et al. 2020).
Group:Astronomy Department, Infrared Processing and Analysis Center (IPAC), Zwicky Transient Facility
Funding AgencyGrant Number
Ministry of Science (Israel)UNSPECIFIED
Benoziyo Center for AstrophysicsUNSPECIFIED
Israel Science FoundationUNSPECIFIED
Binational Science Foundation (USA-Israel)UNSPECIFIED
Weizmann Institute of ScienceUNSPECIFIED
I-CORE Program of the Planning and Budgeting CommitteeUNSPECIFIED
European Research Council (ERC)725161
Deloro Institute for Advanced Research in Space and OpticsUNSPECIFIED
Veronika A. Rabl Physics Discretionary FundUNSPECIFIED
Paul and Tina GardnerUNSPECIFIED
Helen and Martin Kimmel AwardUNSPECIFIED
ZTF partner institutionsUNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
Subject Keywords:Supernovae ; Type II supernovae ; Astronomy data modeling ; Observational astronomy ; Ultraviolet transient sources ; Transient sources
Issue or Number:1
Classification Code:Unified Astronomy Thesaurus concepts: Supernovae (1668); Type II supernovae (1731); Astronomy data modeling (1859); Observational astronomy (1145); Ultraviolet transient sources (1854); Transient sources (1851)
Record Number:CaltechAUTHORS:20190802-110819439
Persistent URL:
Official Citation:Maayane T. Soumagnac et al 2020 ApJ 902 6
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:97618
Deposited By: Joy Painter
Deposited On:02 Aug 2019 18:25
Last Modified:16 Nov 2021 17:33

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