SN 2016B a.k.a ASASSN-16ab: a transitional type II supernova. (arXiv:1904.01844v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dastidar_R/0/1/0/all/0/1">Raya Dastidar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Misra_K/0/1/0/all/0/1">Kuntal Misra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Singh_M/0/1/0/all/0/1">Mridweeka Singh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sahu_D/0/1/0/all/0/1">D. K. Sahu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pastorello_A/0/1/0/all/0/1">A. Pastorello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gangopadhyay_A/0/1/0/all/0/1">Anjasha Gangopadhyay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tomasella_L/0/1/0/all/0/1">L. Tomasella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benetti_S/0/1/0/all/0/1">S. Benetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Terreran_G/0/1/0/all/0/1">G. Terreran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanwal_P/0/1/0/all/0/1">Pankaj Sanwal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kumar_B/0/1/0/all/0/1">Brijesh Kumar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Singh_A/0/1/0/all/0/1">Avinash Singh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kumar_B/0/1/0/all/0/1">Brajesh Kumar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anupama_G/0/1/0/all/0/1">G. C. Anupama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pandey_S/0/1/0/all/0/1">S. B. Pandey</a>
We present photometry, polarimetry and spectroscopy of the Type II supernova
ASASSN-16ab/SN 2016B in PGC 037392. The photometric and spectroscopic follow-up
commenced about two weeks after shock breakout and continued until nearly six
months. The light curve of SN 2016B exhibits intermediate properties between
those of Type IIP and IIL. The early decline is steep (1.68 $pm$ 0.10 mag 100
d$^{-1}$), followed by a shallower plateau phase (0.47 $pm$ 0.24 mag 100
d$^{-1}$). The optically thick phase lasts for 118 d, similar to Type IIP. The
$^{56}$Ni mass estimated from the radioactive tail of the bolometric light
curve is 0.082 $pm$ 0.019 M$_odot$. High velocity component contributing to
the absorption trough of H$alpha$ and H$beta$ in the photospheric spectra are
identified from the spectral modelling from about 57 – 97 d after the outburst,
suggesting a possible SN ejecta and circumstellar material interaction. Such
high velocity features are common in the spectra of Type IIL supernovae. By
modelling the true bolometric light curve of SN 2016B, we estimated a total
ejected mass of $sim$15 M$_odot$, kinetic energy of $sim$1.4 foe and an
initial radius of $sim$400 R$_odot$.
We present photometry, polarimetry and spectroscopy of the Type II supernova
ASASSN-16ab/SN 2016B in PGC 037392. The photometric and spectroscopic follow-up
commenced about two weeks after shock breakout and continued until nearly six
months. The light curve of SN 2016B exhibits intermediate properties between
those of Type IIP and IIL. The early decline is steep (1.68 $pm$ 0.10 mag 100
d$^{-1}$), followed by a shallower plateau phase (0.47 $pm$ 0.24 mag 100
d$^{-1}$). The optically thick phase lasts for 118 d, similar to Type IIP. The
$^{56}$Ni mass estimated from the radioactive tail of the bolometric light
curve is 0.082 $pm$ 0.019 M$_odot$. High velocity component contributing to
the absorption trough of H$alpha$ and H$beta$ in the photospheric spectra are
identified from the spectral modelling from about 57 – 97 d after the outburst,
suggesting a possible SN ejecta and circumstellar material interaction. Such
high velocity features are common in the spectra of Type IIL supernovae. By
modelling the true bolometric light curve of SN 2016B, we estimated a total
ejected mass of $sim$15 M$_odot$, kinetic energy of $sim$1.4 foe and an
initial radius of $sim$400 R$_odot$.
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