Low frequency radio observations of SN 2011dh and the evolution of its post-shock plasma properties
| Autor: | Sayan Chakraborti, Naveen Yadav, Alak Ray |
|---|---|
| Rok vydání: | 2016 |
| Předmět: |
Physics
High Energy Astrophysical Phenomena (astro-ph.HE) Giant Metrewave Radio Telescope 010504 meteorology & atmospheric sciences Astrophysics::High Energy Astrophysical Phenomena Astronomy FOS: Physical sciences Astronomy and Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics Radius Low frequency Light curve 01 natural sciences Luminosity Jansky Supernova Space and Planetary Science 0103 physical sciences Millimeter Astrophysics - High Energy Astrophysical Phenomena 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics 0105 earth and related environmental sciences |
| DOI: | 10.48550/arxiv.1603.00824 |
| Popis: | We present late time, low frequency observations of SN 2011dh made using the Giant Metrewave Radio Telescope (GMRT). Our observations at $325\ \rm MHz$, $610\ \rm MHz$ and $1280\ \rm MHz$ conducted between $93-421\ \rm days$ after the explosion supplement the millimeter and centimeter wave observations conducted between $4-15 \ \rm days$ after explosion using the Combined Array for Research in Millimeter-wave Astronomy (CARMA) and extensive radio observations ($ 1.0-36.5\ \rm GHz$) conducted between $16-93\ \rm days$ after explosion using Jansky Very Large Array (JVLA). We fit a synchrotron self absorption model (SSA) to the $610\ \rm MHz$ and $1280\ \rm MHz$ radio light curves. We use it to determine the radius ($R_{\rm p}$) and magnetic field ($B_{\rm p}$) at $173$ \& $323$ days after the explosion. A comparison of the peak radio luminosity $L_{\rm op}$, with the product of the peak frequency $��_{\rm p}$ and time to peak $t_{\rm p}$ 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, $\dot M/v_{\rm w}$. We derive the mass loss parameter ($A_{\star}$) based on $610\ \rm MHz$ and $1280\ \rm MHz$ radio light curves, which are found to be consistent with each other within error limits. 9 pages, 2 tables and 6 figures. Under review. Comments are welcome |
| Databáze: | OpenAIRE |
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