Photometric observations of two type Ic-BL Supernovae: 2016coi and 2018ebt. (arXiv:2007.05333v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Tsvetkov_D/0/1/0/all/0/1">D. Yu. Tsvetkov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pavlyuk_N/0/1/0/all/0/1">N. N. Pavlyuk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Echeistov_V/0/1/0/all/0/1">V.A. Echeistov</a>
CCD BVRI photometry is presented for the type Ic-BL Supernovae 2016coi and
2018ebt. The shape of the light curves for both objects is typical for this
class of SNe. A change of brightness decline rate at about 100 days after
maximum light is observed for SN 2016coi. The light curves of SN 2018ebt are
best matched by those of SN Ic-BL 2002ap. For SN 2018ebt, we derived the dates
and magnitudes of maximum light, rates of decline at late stages of evolution
and presented evidence for extinction in the host galaxy being negligible.
CCD BVRI photometry is presented for the type Ic-BL Supernovae 2016coi and
2018ebt. The shape of the light curves for both objects is typical for this
class of SNe. A change of brightness decline rate at about 100 days after
maximum light is observed for SN 2016coi. The light curves of SN 2018ebt are
best matched by those of SN Ic-BL 2002ap. For SN 2018ebt, we derived the dates
and magnitudes of maximum light, rates of decline at late stages of evolution
and presented evidence for extinction in the host galaxy being negligible.
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