Collection of PISN light curves computed with hydrodynamics radiative-transfer code STELLA

The PISN light curve collection All data presented on this page are calculated with the hydrodynamicsradiative-transfer code STELLA (Blinnikov et al. 1998, 2000, 2006) by SashaKozyreva. 1. Helium-core PISN models KEPLER PISN models at zero metallicity by A. Heger (Heger & Woosley 2002)These light curves are calculated with STELLA and unpublished. The results of radiative-transfer simulations computed with SEDONA for some of these models are published in Kasen, Heger, Woosley 2011. 2. H-poor/H-free PISNe (Kozyreva et al.2017 Gilmer et al.2017)Initially hydrogenic GENEVA models at Z=0.001 by R. Hirschi 3. Models with Hydrogen left in the envelope (Kozyreva et al. 2014)Models at Z=0.001. N. Langer's stellar evolution code 4. Modified models P150 and 150M (Kozyreva et al. 2018) In this paper, we used modified models P150 (Gilmer et al. 2017) and 150M(Kozyreva et al. 2014) to match H-rich bright SN OGLE14-073. Both modelshave about 10 M⊙ of hydrogen mixed into the thick oxygen layer and 1.3 M⊙ ofradioactive nickel 56Ni. ---------------The content of the lbol-files: (1) time [days] (2) UBVRI-pseidobolometric [erg/s] (3) bolometric [erg/s] (4) X-ray-EUV <325Å (5) IR >890ÅLuminosities are in log10-scale.---------------The content of the tt-files: (1) time [days] (2) Tbb [K] (3) Rbb [cm] (4) Teff [K] (7) Mbol (8) U (9) B (10) V (11) I (12)R