A six year image-subtraction light curve of SN 2010jl. (arXiv:1903.02016v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ofek_E/0/1/0/all/0/1">E. O. Ofek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zackay_B/0/1/0/all/0/1">B. Zackay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gal_Yam_A/0/1/0/all/0/1">A. Gal-Yam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sollerman_J/0/1/0/all/0/1">J. Sollerman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fransson_C/0/1/0/all/0/1">C. Fransson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fremling_C/0/1/0/all/0/1">C. Fremling</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kulkarni_S/0/1/0/all/0/1">S. R. Kulkarni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nugent_P/0/1/0/all/0/1">P. E. Nugent</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yaron_O/0/1/0/all/0/1">O. Yaron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kasliwal_M/0/1/0/all/0/1">M. M. Kasliwal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masci_F/0/1/0/all/0/1">F. Masci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laher_R/0/1/0/all/0/1">R. Laher</a>
SN2010jl was a luminous Type IIn supernova (SN), detected in radio, optical,
X-ray and hard X-rays. Here we report on its six year R- and g-band light
curves obtained using the Palomar Transient Factory. The light curve was
generated using a pipeline based on the proper image subtraction method and we
discuss the algorithm performances. As noted before, the R-band light curve, up
to about 300 days after maximum light is well described by a power-law decline
with a power-law index of about -0.5. Between day 300 and day 2300 after
maximum light, it is consistent with a power-law decline, with a power-law
index of about -3.4. The longevity of the light curve suggests that the massive
circum-stellar material around the progenitor was ejected on time scales of at
least tens of years prior to the progenitor explosion.
SN2010jl was a luminous Type IIn supernova (SN), detected in radio, optical,
X-ray and hard X-rays. Here we report on its six year R- and g-band light
curves obtained using the Palomar Transient Factory. The light curve was
generated using a pipeline based on the proper image subtraction method and we
discuss the algorithm performances. As noted before, the R-band light curve, up
to about 300 days after maximum light is well described by a power-law decline
with a power-law index of about -0.5. Between day 300 and day 2300 after
maximum light, it is consistent with a power-law decline, with a power-law
index of about -3.4. The longevity of the light curve suggests that the massive
circum-stellar material around the progenitor was ejected on time scales of at
least tens of years prior to the progenitor explosion.
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