Type Ib supernova Master OT J120451.50+265946.6: radio emitting shock with inhomogeneities crossing through a dense shell. (arXiv:1904.06392v1 [astro-ph.HE])

Type Ib supernova Master OT J120451.50+265946.6: radio emitting shock with inhomogeneities crossing through a dense shell. (arXiv:1904.06392v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Chandra_P/0/1/0/all/0/1">Poonam Chandra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nayana_A/0/1/0/all/0/1">A. J. Nayana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bjornsson_C/0/1/0/all/0/1">Claes-Ingvar Bjornsson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taddia_F/0/1/0/all/0/1">Francesco Taddia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lundqvist_P/0/1/0/all/0/1">Peter Lundqvist</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ray_A/0/1/0/all/0/1">Alak K. Ray</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shapee_B/0/1/0/all/0/1">Benjamin Shapee</a>

We present radio observations of a Type Ib supernova (SN) Master OT
J120451.50+265946.6. Our low frequency Giant Metrewave Radio Telescope (GMRT)
data taken when the SN was in the optically thick phase for observed
frequencies reveal inhomogeneities in the structure of the radio emitting
region. The high frequency Karl G. Jansky Very Large Array data indicate that
the shock is crossing through a dense shell between $sim$ 47 to $sim 87$
days. The data $ge 100$ days onwards are reasonably well fit with the
inhomogeneous synchrotron-self absorption model. Our model predicts that the
inhomogeneities should smooth out at late times. Low frequency GMRT
observations at late epochs will test this prediction. Our findings suggest the
importance of obtaining well-sampled wide band radio data in order to
understand the intricate nature of the radio emission from young supernovae.

We present radio observations of a Type Ib supernova (SN) Master OT
J120451.50+265946.6. Our low frequency Giant Metrewave Radio Telescope (GMRT)
data taken when the SN was in the optically thick phase for observed
frequencies reveal inhomogeneities in the structure of the radio emitting
region. The high frequency Karl G. Jansky Very Large Array data indicate that
the shock is crossing through a dense shell between $sim$ 47 to $sim 87$
days. The data $ge 100$ days onwards are reasonably well fit with the
inhomogeneous synchrotron-self absorption model. Our model predicts that the
inhomogeneities should smooth out at late times. Low frequency GMRT
observations at late epochs will test this prediction. Our findings suggest the
importance of obtaining well-sampled wide band radio data in order to
understand the intricate nature of the radio emission from young supernovae.

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