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Title: Constraints on the progenitor system and the environs of SN 2014J from deep radio observations

We report deep EVN and eMERLIN observations of the Type Ia SN 2014J in the nearby galaxy M82. Our observations represent, together with JVLA observations of SNe 2011fe and 2014J, the most sensitive radio studies of Type Ia SNe ever. By combining data and a proper modeling of the radio emission, we constrain the mass-loss rate from the progenitor system of SN 2014J to M-dot ≲7.0×10{sup −10} M{sub ⊙} yr{sup −1} (for a wind speed of 100 km s{sup –1}). If the medium around the supernova is uniform, then n {sub ISM} ≲ 1.3 cm{sup –3}, which is the most stringent limit for the (uniform) density around a Type Ia SN. Our deep upper limits favor a double-degenerate (DD) scenario—involving two WD stars—for the progenitor system of SN 2014J, as such systems have less circumstellar gas than our upper limits. By contrast, most single-degenerate (SD) scenarios, i.e., the wide family of progenitor systems where a red giant, main-sequence, or sub-giant star donates mass to an exploding WD, are ruled out by our observations. (While completing our work, we noticed that a paper by Margutti et al. was submitted to The Astrophysical Journal. From a non-detection of X-ray emission from SNmore » 2014J, the authors obtain limits of M-dot ≲1.2×10{sup −9} M {sub ☉} yr{sup –1} (for a wind speed of 100 km s{sup –1}) and n {sub ISM} ≲ 3.5 cm{sup –3}, for the ρ∝r {sup –2} wind and constant density cases, respectively. As these limits are less constraining than ours, the findings by Margutti et al. do not alter our conclusions. The X-ray results are, however, important to rule out free-free and synchrotron self-absorption as a reason for the radio non-detections.) Our estimates on the limits on the gas density surrounding SN2011fe, using the flux density limits from Chomiuk et al., agree well with their results. Although we discuss the possibilities of an SD scenario passing observational tests, as well as uncertainties in the modeling of the radio emission, the evidence from SNe 2011fe and 2014J points in the direction of a DD scenario for both.« less
Authors:
;  [1] ; ; ;  [2] ; ; ;  [3] ;  [4] ;  [5] ; ; ;  [6] ;  [7]
  1. Instituto de Astrofísica de Andalucía, Glorieta de las Astronomía, s/n, E-18008 Granada (Spain)
  2. Department of Astronomy, AlbaNova University Center, Stockholm University, SE-10691 Stockholm (Sweden)
  3. Jodrell Bank Centre for Astrophysics, University of Manchester, Oxford Road, Manchester M13 9PL (United Kingdom)
  4. Joint Institute for VLBI in Europe, Postbus 2, 7990 AA Dwingeloo (Netherlands)
  5. Australian Astronomical Observatory, P.O. Box 915, North Ryde, NSW 1670 (Australia)
  6. Departamento de Astronomía i Astrofísica, Universidad de Valencia, E-46100 Burjassot, Valencia (Spain)
  7. Onsala Space Observatory, Chalmers University of Technology, SE-43992 Onsala (Sweden)
Publication Date:
OSTI Identifier:
22365201
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 792; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASTROPHYSICS; DENSITY; DETECTION; EMISSION; FLUX DENSITY; GALAXIES; GIANT STARS; LIMITING VALUES; MASS TRANSFER; SELF-ABSORPTION; SIMULATION; STELLAR WINDS; SUPERNOVAE; SYNCHROTRONS; VELOCITY; X RADIATION