Signatures of Circumstellar Interaction in the Type IIL Supernova ASASSN-15oz. (arXiv:1901.09962v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bostroem_K/0/1/0/all/0/1">K. Azalee Bostroem</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valenti_S/0/1/0/all/0/1">Stefano Valenti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Horesh_A/0/1/0/all/0/1">Assaf Horesh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morozova_V/0/1/0/all/0/1">Viktoriya Morozova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuin_N/0/1/0/all/0/1">N. Paul M. Kuin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wyatt_S/0/1/0/all/0/1">Samuel Wyatt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jerkstrand_A/0/1/0/all/0/1">Anders Jerkstrand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sand_D/0/1/0/all/0/1">David J. Sand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lundquist_M/0/1/0/all/0/1">Michael Lundquist</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_M/0/1/0/all/0/1">Mathew Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sullivan_M/0/1/0/all/0/1">Mark Sullivan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hosseinzadeh_G/0/1/0/all/0/1">Griffin Hosseinzadeh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arcavi_I/0/1/0/all/0/1">Iair Arcavi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Callis_E/0/1/0/all/0/1">Emma Callis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cartier_R/0/1/0/all/0/1">R&#xe9;gis Cartier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gal_Yam_A/0/1/0/all/0/1">Avishay Gal-Yam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galbany_L/0/1/0/all/0/1">Llu&#xed;s Galbany</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gutierrez_C/0/1/0/all/0/1">Claudia Guti&#xe9;rrez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Howell_D/0/1/0/all/0/1">D. Andrew Howell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Inserra_C/0/1/0/all/0/1">Cosimo Inserra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kankare_E/0/1/0/all/0/1">Erkki Kankare</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_K/0/1/0/all/0/1">Kristhell Marisol L&#xf3;pez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McCully_C/0/1/0/all/0/1">Curtis McCully</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pignata_G/0/1/0/all/0/1">Giuliano Pignata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piro_A/0/1/0/all/0/1">Anthony L. Piro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_O/0/1/0/all/0/1">&#xd3;smar Rodr&#xed;guez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smartt_S/0/1/0/all/0/1">Stephen J. Smartt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_K/0/1/0/all/0/1">Kenneth W. Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yaron_O/0/1/0/all/0/1">Ofer Yaron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Young_D/0/1/0/all/0/1">David R. Young</a>

Hydrogen-rich, core-collapse supernovae are typically divided into four
classes: IIP, IIL, IIn, and IIb. In general, interaction with circumstellar
material is only considered for Type IIn supernovae. However, recent
hydrodynamic modeling of IIP and IIL supernovae requires circumstellar material
to reproduce their early light curves. In this scenario, IIL supernovae
experience large amounts of mass loss before exploding. We test this hypothesis
on ASASSN-15oz, a Type IIL supernova. With extensive follow-up in the X- ray,
UV, optical, IR, and radio we present our search for signs of interaction, and
the mass-loss history indicated by their detection. We find evidence of
short-lived intense mass-loss just prior to explosion from light curve
modeling, amounting in 1.5 M$_{odot}$ of material within 1800 R$_{odot}$ of
the progenitor. We also detect the supernova in the radio, indicating mass-loss
rates of $10^{-6}-10^{-7}$ M$_{odot}$ yr$^{-1}$ prior to the extreme mass-loss
period. Our failure to detect the supernova in the X-ray and the lack of narrow
emission lines in the UV, optical, and NIR do not contradict this picture and
place an upper limit on the mass-loss rate outside the extreme period of
$<10^{-4}$ M$_{odot}$ yr$^{-1}$. This paper highlights the importance gathering comprehensive data on more Type II supernovae to enable detailed modeling of the progenitor and supernova which can elucidate their mass-loss histories and envelope structures and thus inform stellar evolution models.

Hydrogen-rich, core-collapse supernovae are typically divided into four
classes: IIP, IIL, IIn, and IIb. In general, interaction with circumstellar
material is only considered for Type IIn supernovae. However, recent
hydrodynamic modeling of IIP and IIL supernovae requires circumstellar material
to reproduce their early light curves. In this scenario, IIL supernovae
experience large amounts of mass loss before exploding. We test this hypothesis
on ASASSN-15oz, a Type IIL supernova. With extensive follow-up in the X- ray,
UV, optical, IR, and radio we present our search for signs of interaction, and
the mass-loss history indicated by their detection. We find evidence of
short-lived intense mass-loss just prior to explosion from light curve
modeling, amounting in 1.5 M$_{odot}$ of material within 1800 R$_{odot}$ of
the progenitor. We also detect the supernova in the radio, indicating mass-loss
rates of $10^{-6}-10^{-7}$ M$_{odot}$ yr$^{-1}$ prior to the extreme mass-loss
period. Our failure to detect the supernova in the X-ray and the lack of narrow
emission lines in the UV, optical, and NIR do not contradict this picture and
place an upper limit on the mass-loss rate outside the extreme period of
$<10^{-4}$ M$_{odot}$ yr$^{-1}$. This paper highlights the importance
gathering comprehensive data on more Type II supernovae to enable detailed
modeling of the progenitor and supernova which can elucidate their mass-loss
histories and envelope structures and thus inform stellar evolution models.

http://arxiv.org/icons/sfx.gif