CONSTRAINTS ON THE PROGENITOR SYSTEM AND THE ENVIRONS OF SN 2014J FROM DEEP RADIO OBSERVATIONS

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. Our deep upper limits favor a double-degenerate (DD) scenario-invol...

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Bibliographic Details
Published in:The Astrophysical journal 2014-09, Vol.792 (1), p.1-10
Main Authors: Perez-Torres, M A, Lundqvist, P, Beswick, R J, Bjornsson, C I, Muxlow, T W B, Paragi, Z, Ryder, S, Alberdi, A, Fransson, C, MARCAIDE, J M, Marti-Vidal, I, Ros, E, Argo, M K, Guirado, J C
Format: Article
Language:eng
Subjects:
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
DENSITY
DETECTION
EMISSION
Explosions
Flux
FLUX DENSITY
GALAXIES
Gas density
GIANT STARS
LIMITING VALUES
MASS TRANSFER
Progenitors (astrophysics)
Radio
Red giant stars
SELF-ABSORPTION
SIMULATION
SN2014J
stars: mass-loss
STELLAR WINDS
SUPERNOVAE
Supernovae: individual (SN2011fe
SYNCHROTRONS
VELOCITY
X RADIATION
X-rays
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Summary: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. 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. 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.
ISSN:0004-637X
1538-4357
1538-4357