Low frequency radio observations of SN 2011dh and the evolution of its post-shock plasma properties

Naveen Yadav; Alak Ray; Sayan Chakraborti

doi:10.1093/mnras/stw594

paper

Low frequency radio observations of SN 2011dh and the evolution of its post-shock plasma properties

arXiv:1603.00824 · doi:10.1093/mnras/stw594

Abstract

We present late time, low frequency observations of SN 2011dh made using the Giant Metrewave Radio Telescope (GMRT). Our observations at $325 MHz$ , $610 MHz$ and $1280 MHz$ conducted between $93 - 421 days$ after the explosion supplement the millimeter and centimeter wave observations conducted between $4 - 15 days$ after explosion using the Combined Array for Research in Millimeter-wave Astronomy (CARMA) and extensive radio observations ( $1.0 - 36.5 GHz$ ) conducted between $16 - 93 days$ after explosion using Jansky Very Large Array (JVLA). We fit a synchrotron self absorption model (SSA) to the $610 MHz$ and $1280 MHz$ radio light curves. We use it to determine the radius ( $R_{p}$ ) and magnetic field ( $B_{p}$ ) at $173$ \& $323$ days after the explosion. A comparison of the peak radio luminosity $L_{op}$ , with the product of the peak frequency $ν_{p}$ and time to peak $t_{p}$ shows that the supernova evolves between the epochs of CARMA, JVLA and GMRT observations. It shows a general slowing down of the expansion speed of the radio emitting region on a timescale of several hundred days during which the shock is propagating through a circumstellar medium set up by a wind with a constant mass loss parameter, $M ˙ / v_{w}$ . We derive the mass loss parameter ( $A_{⋆}$ ) based on $610 MHz$ and $1280 MHz$ radio light curves, which are found to be consistent with each other within error limits.

arXiv comment9 pages, 2 tables and 6 figures. Under review. Comments are welcome

Low frequency radio observations of SN 2011dh and the evolution of its post-shock plasma properties

Abstract

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