SN 2018ijp: the explosion of a stripped-envelope star within a dense H-rich shell?. (arXiv:2009.03331v3 [astro-ph.HE] UPDATED)

SN 2018ijp: the explosion of a stripped-envelope star within a dense H-rich shell?. (arXiv:2009.03331v3 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Tartaglia_L/0/1/0/all/0/1">L. Tartaglia</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:+Barbarino_C/0/1/0/all/0/1">C. Barbarino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taddia_F/0/1/0/all/0/1">F. Taddia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mason_E/0/1/0/all/0/1">E. Mason</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berton_M/0/1/0/all/0/1">M. Berton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taggart_K/0/1/0/all/0/1">K. Taggart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bellm_E/0/1/0/all/0/1">E. C. Bellm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+De_K/0/1/0/all/0/1">K. De</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frederick_S/0/1/0/all/0/1">S. Frederick</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:+Gal_Yam_A/0/1/0/all/0/1">A. Gal-Yam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golkhou_V/0/1/0/all/0/1">V. Z. Golkhou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graham_M/0/1/0/all/0/1">M. Graham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ho_A/0/1/0/all/0/1">A. Y. Q. Ho</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hung_T/0/1/0/all/0/1">T. Hung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaye_S/0/1/0/all/0/1">S. Kaye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_Y/0/1/0/all/0/1">Y. L. Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laher_R/0/1/0/all/0/1">R. R. Laher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masci_F/0/1/0/all/0/1">F. J. Masci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perley_D/0/1/0/all/0/1">D. A. Perley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Porter_M/0/1/0/all/0/1">M. D. Porter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reiley_D/0/1/0/all/0/1">D. J. Reiley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riddle_R/0/1/0/all/0/1">R. Riddle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rusholme_B/0/1/0/all/0/1">B. Rusholme</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soumagnac_M/0/1/0/all/0/1">M. T. Soumagnac</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walters_R/0/1/0/all/0/1">R. Walters</a>

In this paper, we discuss the outcomes of the follow-up campaign of SN
2018ijp, discovered as part of the Zwicky Transient Facility survey for optical
transients. Its first spectrum shows similarities to broad-lined Type Ic
supernovae around maximum light, whereas later spectra display strong
signatures of interaction between rapidly expanding ejecta and a dense H-rich
circumstellar medium, coinciding with a second peak in the photometric
evolution of the transient. This evolution, along with the results of modeling
of the first light curve peak, suggests a scenario where a stripped star
exploded within a dense circumstellar medium. The two main phases in the
evolution of the transient could be interpreted as a first phase dominated by
radioactive decays, and an later interaction-dominated phase where the ejecta
collide with a pre-existing shell. We therefore discuss SN 2018jp within the
context of a massive star depleted of its outer layers exploding within a dense
H-rich circumstellar medium.

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