J/MNRAS/461/2003 SN 2013ej light curves 1 to 450d after explosion (Yuan+, 2016) ================================================================================ 450 d of Type II SN 2013ej in optical and near-infrared. Yuan F., Jerkstrand A., Valenti S., Sollerman J., Seitenzahl I.R., Pastorello A., Schulze S., Chen T.-W., Childress M.J., Fraser M., Fremling C., Kotak R., Ruiter A.J., Schmidt B.P., Smartt S.J., Taddia F., Terreran G., Tucker B.E., Barbarino C., Benetti S., Elias-Rosa N., Gal-Yam A., Howell D.A., Inserra C., Kankare E., Lee M.Y., Li K.L., Maguire K., Margheim S., Mehner A., Ochner P., Sullivan M., Tomasella L., Young D.R. =2016MNRAS.461.2003Y (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Supernovae ; Photometry, UBVRI ; Photometry, infrared ; Photometry, SDSS Keywords: supernovae: general - supernovae: individual: SN 2013ej Abstract: We present optical and near-infrared photometric and spectroscopic observations of SN 2013ej, in galaxy M74, from 1 to 450 d after the explosion. SN 2013ej is a hydrogen-rich supernova, classified as a Type IIL due to its relatively fast decline following the initial peak. It has a relatively high peak luminosity (absolute magnitude M_V_=-17.6) but a small ^56^Ni production of ~0.023M_{sun}_. Its photospheric evolution is similar to other Type II SNe, with shallow absorption in the H_{alpha}_ profile typical for a Type IIL. During transition to the radioactive decay tail at ~100d, we find the SN to grow bluer in B-V colour, in contrast to some other Type II supernovae. At late times, the bolometric light curve declined faster than expected from ^56^Co decay and we observed unusually broad and asymmetric nebular emission lines. Based on comparison of nebular emission lines most sensitive to the progenitor core mass, we find our observations are best matched to synthesized spectral models with a M_ZAMS_=12-15 M_{sun}_ progenitor. The derived mass range is similar to but not higher than the mass estimated for Type IIP progenitors. This is against the idea that Type IIL are from more massive stars. Observations are consistent with the SN having a progenitor with a relatively low-mass envelope. Description: The LCOGT network started an extensive monitoring campaign of SN 2013ej a few days after its discovery (Valenti et al., 2014, Cat. (J/MNRAS/438/L101). Multiband (UBVRIgriz) photometric observations were carried out with nine 1-m telescopes. Objects: ------------------------------------------------------------- RA (2000) DE Designation(s) ------------------------------------------------------------- 01 36 48.16 +15 45 31.0 SN 2013ej = PSN J01364816+1545310 ------------------------------------------------------------- File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table2.dat 43 722 Optical and NIR photometric observations of SN 2013ej -------------------------------------------------------------------------------- See also: J/MNRAS/438/L101 : First month on SN 2013ej (Valenti+, 2014) Byte-by-byte Description of file: table2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 10 A10 "date" Obs.Date UT observation date 12- 20 F9.3 d JD Julian date (JD-2400000) 22- 26 F5.2 mag mag Magnitude in Filter 28- 31 F4.2 mag e_mag rms uncertainty on mag 33- 34 A2 --- Filt Filter (1) 36- 43 A8 --- Tel Telescope/Instrument (2) -------------------------------------------------------------------------------- Note (1): Filtesr are UBVRIJHKs and ugriz. Note (2): Optical telescopes and instruments as follows: 1m008 = LCOGT 1m at Mc-Donald observatory, USA 1m010 = LCOGT 1m at Sutherland, South Africa 1m012 = LCOGT 1m at Sutherland, South Africa 1m013 = LCOGT 1m at Sutherland, South Africa 1m004 = LCOGT 1m at Cerro Tololo, Cile 1m005 = LCOGT 1m at Cerro Tololo, Cile 1m009 = LCOGT 1m at Cerro Tololo, Cile 1m003 = LCOGT 1m at Siding Spring, Australia 1m011 = LCOGT 1m at Siding Spring, Australia LOT = 1m at the Lulin Observatory in Taiwan AFOSC = INAF 1.82 m + AFOSC SBIG = INAF Schmidt 67/92 cm + SBIG NTT = NTT + EFOSC2 VLT = X-shooter Acquisition and Guiding camera See Section 2 for further details. -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Patricia Vannier [CDS] 27-Nov-2017