A Systematic Study of Ia-CSM Supernovae from the ZTF Bright Transient Survey

Creators: Sharma, Yashvi; Sollerman, Jesper; Fremling, Christoffer; Kulkarni, Shrinivas R.; De, Kishalay; Irani, Ido; Schulze, Steve; Strotjohann, Nora Linn; Gal-Yam, Avishay; Maguire, Kate; Perley, Daniel A.; Bellm, Eric C.; Kool, Erik C.; Brink, Thomas G.; Bruch, Rachel; Deckers, Maxime; Dekany, Richard; Dugas, Alison; Filippenko, Alexei V.; Goldwasser, Samantha; Graham, Matthew J.; Graham, Melissa L.; Groom, Steven L.; Hankins, Matt; Jencson, Jacob; Johansson, Joel P.; Karambelkar, Viraj; Kasliwal, Mansi M.; Masci, Frank J.; Medford, Michael S.; Neill, James D.; Nir, Guy; Riddle, Reed L.; Rigault, Mickael; Schweyer, Tassilo; Terwel, Jacco H.; Yan, Lin; Yang, Yi; Yao, Yuhan

Abstract

Among the supernovae (SNe) that show strong interaction with a circumstellar medium (CSM), there is a rare subclass of Type Ia supernovae, SNe Ia-CSM, which show strong narrow hydrogen emission lines much like SNe IIn but on top of a diluted Type Ia spectrum. The only previous systematic study of this class identified 16 SNe Ia-CSM, eight historic and eight from the Palomar Transient Factory (PTF). Now using the successor survey to PTF, the Zwicky Transient Facility (ZTF), we have classified 12 additional SNe Ia-CSM through the systematic Bright Transient Survey (BTS). Consistent with previous studies, we find these SNe to have slowly evolving optical light curves with peak absolute magnitudes between −19.1 and −21, spectra having weak Hβ and large Balmer decrements of ∼7. Out of the 10 SNe from our sample observed by NEOWISE, nine have 3σ detections, with some SNe showing a reduction in the red wing of Hα, indicative of newly formed dust. We do not find our SN Ia-CSM sample to have a significantly different distribution of equivalent widths of He Iλ5876 than SNe IIn as observed in Silverman et al. The hosts tend to be late-type galaxies with recent star formation. We derive a rate estimate of 29⁺²⁷₋₂₁Gpc⁻³ yr⁻¹ for SNe Ia-CSM, which is ∼0.02%–0.2% of the SN Ia rate. We also identify six ambiguous SNe IIn/Ia-CSM in the BTS sample and including them gives an upper limit rate of 0.07%–0.8%. This work nearly doubles the sample of well-studied Ia-CSM objects in Silverman et al., increasing the total number to 28.

Additional Information

© 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Based on observations obtained with the Samuel Oschin Telescope 48 inch and the 60 inch Telescope at the Palomar Observatory as part of the ZTF project. ZTF is supported by the National Science Foundation under Grants No. AST-1440341 and AST-2034437 and a collaboration including current partners Caltech, IPAC, the Weizmann Institute of Science, the Oskar Klein Center at Stockholm University, the University of Maryland, Deutsches Elektronen-Synchrotron and Humboldt University, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, IN2P3, University of Warwick, Ruhr University Bochum, Northwestern University and former partners the University of Washington, Los Alamos National Laboratories, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW. The ZTF forced-photometry service was funded under the Heising-Simons Foundation grant #12540303 (PI: Graham). This work was supported by the GROWTH project (Kasliwal et al. 2019) funded by the National Science Foundation under PIRE grant No. 1545949. The Oskar Klein Centre was funded by the Swedish Research Council. 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. Some of the data presented here were obtained with ALFOSC. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. The SED Machine is based upon work supported by the National Science Foundation under grant No. 1106171. This work has made use of data from the Asteroid Terrestrial-impact Last Alert System (ATLAS) project. The Asteroid Terrestrial-impact Last Alert System (ATLAS) project is primarily funded to search for near earth asteroids through NASA grants NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575; byproducts of the NEO search include images and catalogs from the survey area. The ATLAS science products have been made possible through the contributions of the University of Hawaii Institute for Astronomy, the Queen's University Belfast, the Space Telescope Science Institute, the South African Astronomical Observatory, and The Millennium Institute of Astrophysics (MAS), Chile. This research has made use of the NASA/IPAC Infrared Science Archive, which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. Y.S. thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining grant #1829740, the Brinson Foundation, and the Moore Foundation; her participation in the program has benefited this work. S.S. acknowledges support from the G.R.E.A.T research environment, funded by Vetenskapsrådet, the Swedish Research Council, project number 2016-06012. This work has been supported by the research project grant "Understanding the Dynamic Universe" funded by the Knut and Alice Wallenberg Foundation under Dnr KAW 2018.0067. The research of Y.Y. is supported through a Bengier-Winslow-Robertson Fellowship A.V.F.'s supernova group at UC Berkeley received support from the Christopher R. Redlich Fund and many individual donors. Fritz (van der Walt et al. 2019; Duev et al. 2019) and GROWTH marshal (Kasliwal et al. 2019) (dynamic collaborative platforms for time-domain astronomy) were used in this work. Software: LAMBDAR (Wright et al. 2016), Prospector (Johnson et al. 2021), pySEDM (Rigault et al. 2019), IRAF (Tody 1986, 1993), pyNOT (https://github.com/jkrogager/PyNOT), LPipe (Perley 2019), pypeit (Prochaska et al. 2020), extinction (Barbary 2016), pyraf-dbsp (Bellm & Sesar 2016), FPipe (Fremling et al. 2016), DBSP_DRP (Mandigo-Stoba et al. 2022), ztfquery (Rigault 2018), astropy (Astropy Collaboration et al. 2013, 2018, 2022), matplotlib (Hunter 2007).

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