Confined dense circumstellar material surrounding a regular type II supernova

Abstract

(Fig. 1). The first BB temperature estimate was obtained via careful extrapolation of the UVOT UV M2 and P60 g + i light curves back to the first P48 (detection) point (see inset of Fig. 1 and text for details). The earlytime BB temperature estimates, within the first half day after explosion, are also in agreement with our temperature estimates from the modeling of the early Keck spectra (Fig. 4), showing the highly ionised emission lines at temperatures > ∼ 50 kK. The shaded region and the solid black line (a running mean of the region) denote bolometric luminosity estimates based on the multiband photometry ( Fig. 1) according to three methods used to calculate the total flux from the SED: interpolation, order-4 polynomial fit, and BB fits. The top end of the shaded region can be regarded as our best lower limit on the real bolometric luminosity, based on the photometric observations. The red triangles denote a (more conservative) lower limit on the bolometric luminosity obtained from our spectra (Fig. 2, Fig. 3), beginning with the early set of 4 Keck spectra at < ∼ 10 hr after explosion and ending with our latest spectrum at 57.2days. The blue triangles show the luminosity as obtained by our best BB temperature and radius estimates (Fig. 4), L = 4πR 2 σT 4 ; the luminosity in the first point, at ∼ 3.8 hr after explosion, exceeds 10 44 erg s −1 .

The two promising scenarios to explode core collapse supernovae

“…It seems that the pre-explosion outbursts of CCSNe are common (e.g., Moriya et al 2014;Ofek et al 2014;Svirski & Nakar 2014;Tartaglia et al 2016;Yaron et al 2017), with about one in ten CCSNe suffering a pre-explosion outburst (e.g., Margutti et al 2017). The outburst might result from a single-star process, e.g., strong convection in the pre-collapsing core (Quataert & Shiode 2012;Shiode & Quataert 2014).…”

iPTF Survey for Cool Transients

“…The observation pairs were repeated with a cadence varying between one night and two weeks (depending on weather and the aforementioned scheduling considerations; see Figure 2). The schedule was manually (Yaron et al 2017), SN Ia SN2011fe (Munari et al 2013), SN IIn PTF11fzz (Ofek et al 2013), SN IIb iPTF13ast (Gal-Yam et al 2014), and LRN M101-OT (Blagorodnova et al 2017a). Including I band in a time-domain survey can improve the photometric classification and selection of both SN Ia (by the late-time I band bump) and very cool and/or dusty transients such as luminous red novae (by their extremely red color).…”

The Early Detection and Follow-up of the Highly Obscured Type II Supernova 2016ija/DLT16am∗

“…Alternatively, "flash spectroscopy" at very early phases can probe the physical properties of the CSM as well as the mass-loss history of the progenitor star prior to its explosion (e.g., Gal-Yam et al 2014;Smith et al 2015;Khazov et al 2016;Yaron et al 2017). Even when archival HST data are available, radius estimates through the analysis of very early data can give important results, since the progenitor field might be contaminated by the presence of binary companions (e.g., Tartaglia et al 2017a).…”