Constraints on the Progenitor System and the Environs of SN 2014J from Deep Radio Observations
Artikel i vetenskaplig tidskrift, 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

stars: mass-loss

SN2014J)

Författare

Miguel Angel Perez-Torres

Universidad de Zaragoza

CSIC - Instituto de Astrofísica de Andalucía (IAA)

Centro de Estudios de Física del Cosmos de Aragón

P. Lundqvist

AlbaNova University Center

The Oskar Klein Centre

R. J. Beswick

Jodrell Bank Observatory

University of Manchester

C. I. Bjornsson

AlbaNova University Center

T .W. B. Muxlow

University of Manchester

Jodrell Bank Observatory

Z. Paragi

Joint Institute for VLBI in Europe

S. Ryder

Australian Astronomical Observatory

Antxon Alberdi

CSIC - Instituto de Astrofísica de Andalucía (IAA)

C. Fransson

The Oskar Klein Centre

AlbaNova University Center

J. M. Marcaide

Universitat de Valencia

Donostia International Physics Center

Ivan Marti-Vidal

Chalmers, Rymd- och geovetenskap, Onsala rymdobservatorium

Eduardo Ros

Max Planck-institutet

Universitat de Valencia

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 Art. no. 38- 38

Ämneskategorier

Astronomi, astrofysik och kosmologi

DOI

10.1088/0004-637x/792/1/38