Observations of Type Ia Supernova 2014J for Nearly 900 Days and Constraints on Its Progenitor System. (arXiv:1906.07321v1 [astro-ph.SR])

Observations of Type Ia Supernova 2014J for Nearly 900 Days and Constraints on Its Progenitor System. (arXiv:1906.07321v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Li_W/0/1/0/all/0/1">Wenxiong Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_X/0/1/0/all/0/1">Xiaofeng Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hu_M/0/1/0/all/0/1">Maokai Hu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_Y/0/1/0/all/0/1">Yi Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_J/0/1/0/all/0/1">Jujia Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mo_J/0/1/0/all/0/1">Jun Mo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Z/0/1/0/all/0/1">Zhihao Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_T/0/1/0/all/0/1">Tianmeng Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benetti_S/0/1/0/all/0/1">Stefano Benetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cappellaro_E/0/1/0/all/0/1">Enrico Cappellaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elias_Rosa_N/0/1/0/all/0/1">Nancy Elias-Rosa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Isern_J/0/1/0/all/0/1">Jordi Isern</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morales_Garoffolo_A/0/1/0/all/0/1">Antonia Morales-Garoffolo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_F/0/1/0/all/0/1">Fang Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ochner_P/0/1/0/all/0/1">Paolo Ochner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pastorello_A/0/1/0/all/0/1">Andrea Pastorello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reguitti_A/0/1/0/all/0/1">Andrea Reguitti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tartaglia_L/0/1/0/all/0/1">Leonardo Tartaglia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Terreran_G/0/1/0/all/0/1">Giacomo Terreran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tomasella_L/0/1/0/all/0/1">Lina Tomasella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_L/0/1/0/all/0/1">Lifan Wang</a>

We present extensive ground-based and $Hubble~Space~Telescope$ ($HST$)
photometry of the highly reddened, very nearby type Ia supernova (SN Ia) 2014J
in M82, covering the phases from 9 days before to about 900 days after the
$B$-band maximum. SN 2014J is similar to other normal SNe Ia near the maximum
light, but it shows flux excess in the $B$ band in the early nebular phase.
This excess flux emission can be due to light scattering by some structures of
circumstellar materials located at a few 10$^{17}$ cm, consistent with a single
degenerate progenitor system or a double degenerate progenitor system with mass
outflows in the final evolution or magnetically driven winds around the binary
system. At t$sim$+300 to $sim$+500 days past the $B$-band maximum, the light
curve of SN 2014J shows a faster decline relative to the $^{56}$Ni decay. Such
a feature can be attributed to the significant weakening of the emission
features around [Fe III] $lambda$4700 and [Fe II] $lambda$5200 rather than
the positron escape as previously suggested. Analysis of the $HST$ images taken
at t$>$600 days confirms that the luminosity of SN 2014J maintains a flat
evolution at the very late phase. Fitting the late-time pseudo-bolometric light
curve with radioactive decay of $^{56}$Ni, $^{57}$Ni and $^{55}$Fe isotopes, we
obtain the mass ratio $^{57}$Ni/$^{56}$Ni as $0.035 pm 0.011$, which is
consistent with the corresponding value predicted from the 2D and 3D
delayed-detonation models. Combined with early-time analysis, we propose that
delayed-detonation through single degenerate scenario is most likely favored
for SN 2014J.

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