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A DEEP SEARCH for PROMPT RADIO EMISSION from THERMONUCLEAR SUPERNOVAE with the VERY LARGE ARRAY Laura Chomiuk1,11, Alicia M

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A DEEP SEARCH for PROMPT RADIO EMISSION from THERMONUCLEAR SUPERNOVAE with the VERY LARGE ARRAY Laura Chomiuk1,11, Alicia M Draft version July 1, 2018 Preprint typeset using LATEX style emulateapj v. 5/2/11 A DEEP SEARCH FOR PROMPT RADIO EMISSION FROM THERMONUCLEAR SUPERNOVAE WITH THE VERY LARGE ARRAY Laura Chomiuk1;11, Alicia M. Soderberg2, Roger A. Chevalier3, Seth Bruzewski1, Ryan J. Foley4,5, Jerod Parrent2, Jay Strader1, Carles Badenes6 Claes Fransson7 Atish Kamble2, Raffaella Margutti8, Michael P. Rupen9, & Joshua D. Simon10 Draft version July 1, 2018 ABSTRACT Searches for circumstellar material around Type Ia supernovae (SNe Ia) are one of the most powerful tests of the nature of SN Ia progenitors, and radio observations provide a particularly sensitive probe of this material. Here we report radio observations for SNe Ia and their lower-luminosity thermonu- clear cousins. We present the largest, most sensitive, and spectroscopically diverse study of prompt (∆t . 1 yr) radio observations of 85 thermonuclear SNe, including 25 obtained by our team with the unprecedented depth of the Karl G. Jansky Very Large Array. With these observations, SN 2012cg joins SN 2011fe and SN 2014J as a SN Ia with remarkably deep radio limits and excellent temporal −1 _ −9 M yr coverage (six epochs, spanning 5{216 days after explosion, yielding M=vw . 5 × 10 100 km s−1 , assuming B = 0:1 and e = 0:1). All observations yield non-detections, placing strong constraints on the presence of circumstellar material. We present analytical models for the temporal and spectral evolution of prompt radio emission from thermonuclear SNe as expected from interaction with either wind-stratified or uniform density media. These models allow us to constrain the progenitor mass loss rates, with limits ranging _ −9 −4 −1 −1 from M . 10 − 10 M yr , assuming a wind velocity vw = 100 km s . We compare our radio constraints with measurements of Galactic symbiotic binaries to conclude that .10% of thermonuclear SNe have red giant companions. Subject headings: binaries: general | circumstellar matter | radio continuum: stars | supernovae: general | supernovae: individual (SN 2012cg) 1. INTRODUCTION mass, or if significantly sub-Chandrasekhar white dwarfs The nature of the progenitors of Type Ia supernovae can explode as thermonuclear SNe. In addition, the na- (SNe Ia) and other thermonuclear SNe (SNe Iax, Ca- ture of the binary companion remains a puzzle: it could rich SNe; SN 2002es-like explosions; Perets et al. 2010; be a red (super)giant, a subgiant, a main sequence star, Ganeshalingam et al. 2012; Foley et al. 2013) remains or another white dwarf (Iben & Tutukov 1984; Webbink an important gap in our understanding of astrophysics, 1984). A wealth of review articles summarize these out- with important implications for cosmology, stellar phe- standing mysteries; see Branch et al. (1995); Livio (2001); nomenology, and chemical evolution. There is general Howell (2011); Wang & Han (2012); Maoz et al. (2014). agreement that thermonuclear SNe involve a white dwarf in a binary system, but it remains unknown if the white 1.1. Techniques for testing progenitor scenarios dwarf is destabilized by reaching the Chandrasekhar Unlike H-rich core-collapse supernovae, which have lu- minous massive star progenitors (Smartt 2009, 2015), the 1 Department of Physics and Astronomy, Michigan State Uni- direct detection of the themonuclear SN progenitor sys- versity, East Lansing, MI 48824, USA tem in pre-explosion images is not usually a viable tech- 2 Harvard-Smithsonian Center for Astrophysics, 60 Garden nique. The expected white dwarf and any likely com- Street, Cambridge, MA 02138, USA panion are simply too faint for pre-explosion measure- 3 Department of Astronomy, University of Virginia, PO Box arXiv:1510.07662v1 [astro-ph.HE] 26 Oct 2015 400325, Charlottesville, VA 22904, USA ments to be constraining (e.g., Maoz & Mannucci 2008). 4 Astronomy Department, University of Illinois at Urbana- Noteable exceptions are the two nearest SNe Ia of recent Champaign, 1002 W. Green Street, Urbana, IL 61801, USA times, SN 2011fe and SN 2014J (these also yielded non- 5 Department of Physics, University of Illinois at Urbana- detections; Li et al. 2011; Kelly et al. 2014) and SNe Iax Champaign, 1110 W. Green Street, Urbana, IL 61801, USA 6 Department of Physics and Astronomy & Pittsburgh Parti- (see below). cle Physics, Astrophysics, and Cosmology Center (PITT-PACC), Therefore, indirect techniques are needed for constrain- University of Pittsburgh, Pittsburgh, PA 15260, USA ing the progenitors of thermonuclear SNe. Such tests in- 7 Department of Astronomy, Stockholm University, AlbaNova, clude: SE-106 91 Stockholm, Sweden 8 Center for Cosmology and Particle Physics, New York Uni- (a) the impact of the companion on the early SN light versity, 4 Washington Place, New York, NY 10003, USA curve (Kasen 2010; Hayden et al. 2010; Bianco et al. 2011; 9 National Research Council of Canada, Herzberg Astronomy Ganeshalingam et al. 2011; Brown et al. 2012; Foley et al. and Astrophysics Programs, Dominion Radio Astrophysical Ob- servatory, P.O. Box 248, Penticton, BC V2A 6J9, Canada 2012c; Zheng et al. 2013; Olling et al. 2015; Marion et al. 10 Carnegie Observatories, 813 Santa Barbara St., Pasadena, 2015); CA 91101, USA (b) searches for the companion star in nearby SN Ia rem- 11 [email protected] nants (Ruiz-Lapuente et al. 2004; Kerzendorf et al. 2009, 2 2012, 2013, 2014; Schaefer & Pagnotta 2012); ing the amount of H-rich material entrained in the SN (c) late-time nebular spectroscopy to search for compan- ejecta, presumably from the blast wave sweeping over ion material entrained in the SN ejecta (Leonard 2007; a companion star; Leonard 2007; Shappee et al. 2013; Shappee et al. 2013; Lundqvist et al. 2013, 2015); Lundqvist et al. 2013, 2015). (d) estimates of white dwarf mass and ejecta mass from light curves and nucleosynthesis (Howell et al. 2006; 1.2.3. Radio observations Stritzinger et al. 2006; Seitenzahl et al. 2013; Scalzo et al. Observations of non-thermal radio emission trace elec- 2014; Yamaguchi et al. 2015); and trons accelerated to relativistic speeds via diffusive shock (e) characterization of the circumstellar environment at acceleration, emitting synchrotron radiation. Radio ob- the SN site Panagia et al. (2006); Russell & Immler servations with the Very Large Array over a period of (2012); Margutti et al. (2012); Chomiuk et al. (2012b); two decades set upper limits on the emission from 27 Margutti et al. (2014). The latter strategy, carried out SNe Ia (Panagia et al. 2006, and references therein). The using radio continuum emission, is the subject of this 25 −1 most constraining luminosity limits are . 10 erg s paper. Hz−1 over timescales of 10{1000 days after explosion. In order to predict the expected radio luminosity, Panagia 1.2. Studies of circumstellar material et al. (2006) assume a model in which the radio-emitting 1.2.1. Theoretical expectations SN blast wave is expanding at 10,000 km s−1, the syn- The various progenitor channels associated with ther- chrotron emission is absorbed by free-free processes in monuclear SNe are each associated with a signature cir- an external wind of temperature of 2 × 104 K, and the cumbinary environment (see Chomiuk et al. 2012b and synchrotron luminosity is scaled to observations of the Margutti et al. 2014 for more discussion). The compo- Type Ib/c supernova SN 1983N. Typical limits on the −1 sition, density, and radial profile are shaped by the late _ −5 M yr mass loss rate are then M=vw . 10 100 km s−1 , but time evolution of the progenitor system. For example, −1 _ −7 M yr the densest circumstellar medium (CSM) should be ex- extend down to M=vw . 3×10 100 km s−1 in the most pelled by a red giant companion; the SN would then sensitive cases. explode in a wind-stratified medium, with the density The radio observations from Panagia et al. (2006) were declining with radius from the giant. White dwarfs with stacked by Hancock et al. (2011) to achieve maximal main-sequence or sub-giant companions would be sur- sensitivity. The stacked radio observation still yielded rounded by a much less dense wind, but may host dense a non-detection, but the \typical" limit on the progen- narrow shells of material at some radii: the remnants of itor mass loss rate is an order of magnitude more con- −1 nova explosions (Chomiuk et al. 2012b). Theory predicts _ −6 M yr straining, M=vw . 10 100 km s−1 (using the formalism a diversity of circumbinary environments for double de- of Panagia et al. 2006, which assume a fixed blast wave generate systems (where the companion is a He or CO velocity and free-free absorption). white dwarf), including wind-stratified material (Guillo- More recently, very deep radio limits have been placed chon et al. 2010; Dan et al. 2011; Ji et al. 2013), nova on the nearby SNe Ia 2011fe and 2014J using the syn- shells (Shen et al. 2013), tidal tails of shredded white chrotron self-absorption formalism described in detail in dwarf material (Raskin & Kasen 2013), or low densi- this paper (Horesh et al. 2012; Chomiuk et al. 2012b; ties indistinguishable from the local interstellar medium. P´erez-Torres et al. 2014). This reconsideration of syn- Therefore, the overarching goal of the radio survey pre- chrotron opacity was driven by the work of Chevalier sented here is the search for material in the local explo- (1998), which showed that for the fast blast wave veloc- sion environment, with important implications for binary ities and relatively low-density environments of Type I evolution and mass transfer in thermonuclear SN progen- SNe, synchrotron self-absorption dominates over free- itor systems. free absorption. Due to the proximity of SN 2011fe and A wide range of multi-wavelength observations have, to SN 2014J and intensive observing campaigns, mass loss date, placed important constraints on the environments rates in these two explosions are strongly constrained, of SNe Ia.
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