Constraints on the Progenitor System and the Environs of SN 2014J from Deep Radio Observations
Journal article, 2014
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) over dot less than or similar to 7.0 x 10(-10) M yr(-1) (for a wind speed of 100 km s(-1)). If the medium around the supernova is uniform, then n(ISM) less than or similar to 1.3 cm(-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 SN 2014J, the authors obtain limits of (M) over dot less than or similar to 1.2 x 10(-9) M-circle dot yr(-1) (for a wind speed of 100 km s(-1)) and n(ISM) less than or similar to 3.5 cm(-3), for the rho proportional to r(-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.
Supernovae: individual (SN2011fe
SN2014J)
stars: mass-loss
Author
Miguel Angel Perez-Torres
Institute of Astrophysics of Andalusia (IAA)
Centro de Estudios de Física del Cosmos de Aragón
University of Zaragoza
P. Lundqvist
The Oskar Klein Centre
AlbaNova University Center
R. J. Beswick
University of Manchester
Jodrell Bank Observatory
C. I. Bjornsson
AlbaNova University Center
T .W. B. Muxlow
University of Manchester
Jodrell Bank Observatory
Z. Paragi
Joint Institute for VLBI in Europe (JIVE)
S. Ryder
Australian Astronomical Observatory
Antxon Alberdi
Institute of Astrophysics of Andalusia (IAA)
C. Fransson
The Oskar Klein Centre
AlbaNova University Center
J. M. Marcaide
Donostia International Physics Center
Universitat de Valencia
Ivan Marti-Vidal
Chalmers, Earth and Space Sciences, Onsala Space Observatory
Eduardo Ros
Universitat de Valencia
Max Planck Society
M. K. Argo
University of Manchester
Jodrell Bank Observatory
J. C. Guirado
Universitat de Valencia
Astrophysical Journal
0004-637X (ISSN) 1538-4357 (eISSN)
Vol. 792 1 Art. no. 38- 38Advanced Radio Astronomy in Europe (RADIONET3)
European Commission (EC) (EC/FP7/283393), 2012-01-01 -- 2015-12-31.
Subject Categories
Astronomy, Astrophysics and Cosmology
DOI
10.1088/0004-637x/792/1/38