The Broad-lined Ic Supernova ZTF18aaqjovh (SN 2018bvw): An Optically-discovered Engine-driven Supernova Candidate with Luminous Radio Emission

Creators: Ho, Anna Y. Q.; Corsi, Alessandra; Cenko, S. Bradley; Taddia, Francesco; Kulkarni, S. R.; Adams, Scott; De, Kishalay; Dekany, Richard; Frederiks, Dmitry D.; Fremling, Christoffer; Golkhou, V. Zach; Graham, Matthew J.; Hung, Tiara; Kupfer, Thomas; Laher, Russ R.; Mahabal, Ashish; Masci, Frank J.; Miller, Adam A.; Neill, James D.; Reiley, Daniel; Riddle, Reed; Ridnaia, Anna; Rusholme, Ben; Sharma, Yashvi; Sollerman, Jesper; Soumagnac, Maayane T.; Svinkin, Dmitry S.; Shupe, David L.

Abstract

We present ZTF18aaqjovh (SN 2018bvw), a high-velocity ("broad-lined") stripped-envelope (Type Ic) supernova (Ic-BL SN) discovered in the Zwicky Transient Facility one-day cadence survey. ZTF18aaqjovh shares a number of features in common with engine-driven explosions: the photospheric velocity and the shape of the optical light curve are very similar to those of the Type Ic-BL SN 1998bw, which was associated with a low-luminosity gamma-ray burst (LLGRB) and had relativistic ejecta. However, the radio luminosity of ZTF18aaqjovh is almost two orders of magnitude fainter than that of SN 1998bw at the same velocity phase, and the shock velocity is at most mildly relativistic (v = 0.06–0.4c). A search of high-energy catalogs reveals no compelling gamma-ray burst (GRB) counterpart to ZTF18aaqjovh, and the limit on the prompt GRB luminosity of L_(γ,iso)≈1.6×10⁴⁸ erg/s⁻¹ excludes a classical GRB but not an LLGRB. Altogether, ZTF18aaqjovh represents another transition event between engine-driven SNe associated with GRBs and "ordinary" Ic-BL SNe.

Additional Information

© 2020 The American Astronomical Society. Received 2019 December 20; revised 2020 February 25; accepted 2020 March 2; published 2020 April 23. Based 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. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This work made use of the data products generated by the NYU SN group, and released under Bianco et al. (2016), available at https://github.com/nyusngroup/SESNspectraLib. SED Machine is based upon work supported by the National Science Foundation under grant No. 1106171. The ZTF forced-photometry service was funded under the Heising–Simons Foundation grant #12540303 (PI: Graham). Partially based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. 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 National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. A.Y.Q.H. is supported by a National Science Foundation Graduate Research Fellowship under grant No. DGE1144469. A.C. acknowledges support from the National Science Foundation CAREER award #1455090. A.C. and A.Y.Q.H. acknowledge support from the Chandra GI award #19500451. This work was partially supported by the GROWTH project funded by the National Science Foundation under PIRE grant No. 1545949. A.A.M. is funded by the Large Synoptic Survey Telescope Corporation, the Brinson Foundation, and the Moore Foundation in support of the LSSTC Data Science Fellowship Program; he also receives support as a CIERA Fellow by the CIERA Postdoctoral Fellowship Program (Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University). C.F. gratefully acknowledges support of his research by the Heising–Simons Foundation (#2018-0907).

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