Using the Optical–NIR Spectral Energy Distributions To Search for the Evidence of Dust Formation of 66 Supernovae. (arXiv:2110.15197v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Li_J/0/1/0/all/0/1">Jing-Yao Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_S/0/1/0/all/0/1">Shan-Qin Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gan_W/0/1/0/all/0/1">Wen-Pei Gan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_T/0/1/0/all/0/1">Tao Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lian_J/0/1/0/all/0/1">Ji-Shun Lian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bai_S/0/1/0/all/0/1">Song-Yao Bai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liang_E/0/1/0/all/0/1">En-Wei Liang</a>
In this paper, we searched for the dust formation evidence of 66 supernovae
(SNe) by using the blackbody model and the blackbody plus dust {emission} model
to fit their early$-$time optical$-$near infrared (NIR) spectral energy
distributions (SEDs). We find that, while the blackbody model can fit most SEDs
of the SNe in our sample, the model cannot fit the SEDs of some SNe, in which
the SEDs of 2 SNe (SNe~2010bq and 2012ca) show NIR excesses which can be
attributed to the emission from the heated dust. We use blackbody plus dust
emission model to fit the SEDs showing NIR excesses, finding that both graphite
and silicate dust models can fit the SEDs, and the graphite model get
reasonable temperatures or better fits. Assuming that the dust is graphite, the
best-fitting temperatures (masses) of the dust of the SNe~2010bq and 2012ca are
$sim 1300-1800$ K ($sim 0.1-3.4 times 10^{-4}$ M$_odot$) and $sim
600-1000$ K ($sim 0.6-7.5 times 10^{-3}$ M$_odot$), respectively. We compare
the vaporization radii and the blackbody radii of the dust shells of the 2 SNe
with the upper limits of the ejecta radii of the SNe at the first epochs, and
demonstrate that the NIR excesses of the SEDs of the 2 SNe might be caused by
the pre-existing dust.
In this paper, we searched for the dust formation evidence of 66 supernovae
(SNe) by using the blackbody model and the blackbody plus dust {emission} model
to fit their early$-$time optical$-$near infrared (NIR) spectral energy
distributions (SEDs). We find that, while the blackbody model can fit most SEDs
of the SNe in our sample, the model cannot fit the SEDs of some SNe, in which
the SEDs of 2 SNe (SNe~2010bq and 2012ca) show NIR excesses which can be
attributed to the emission from the heated dust. We use blackbody plus dust
emission model to fit the SEDs showing NIR excesses, finding that both graphite
and silicate dust models can fit the SEDs, and the graphite model get
reasonable temperatures or better fits. Assuming that the dust is graphite, the
best-fitting temperatures (masses) of the dust of the SNe~2010bq and 2012ca are
$sim 1300-1800$ K ($sim 0.1-3.4 times 10^{-4}$ M$_odot$) and $sim
600-1000$ K ($sim 0.6-7.5 times 10^{-3}$ M$_odot$), respectively. We compare
the vaporization radii and the blackbody radii of the dust shells of the 2 SNe
with the upper limits of the ejecta radii of the SNe at the first epochs, and
demonstrate that the NIR excesses of the SEDs of the 2 SNe might be caused by
the pre-existing dust.
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