EXTENSIVE SPECTROSCOPY and PHOTOMETRY of the TYPE IIP SUPERNOVA 2013ej

G. Dhungana, R. Kehoe, J. Vinko, J. M. Silverman, J. C. Wheeler, W. Zheng, G. H. Marion, O. D. Fox, C. Akerlof, B. I. Biro, T. Borkovits, S. B. Cenko, K. I. Clubb, A. V. Filippenko, F. V. Ferrante, C. A. Gibson, M. L. Graham, T. Hegedus, P. Kelly, J. KelemenW. H. Lee, G. Marschalko, L. Molnár, A. P. Nagy, A. Ordasi, A. Pal, K. Sarneczky, I. Shivvers, R. Szakats, T. Szalai, E. Szegedi-Elek, P. Székely, A. Szing, K. Takáts, K. Vida

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Abstract

We present extensive optical (UBV RI, griz, and open CCD) and near-infrared (ZY JH) photometry for the very nearby Type IIP SN 2013ej extending from +1 to +461 days after shock breakout, estimated to be MJD 56496.9 ± 0.3. Substantial time series ultraviolet and optical spectroscopy obtained from +8 to +135 days are also presented. Considering well-observed SNe IIP from the literature, we derive UBV RIJHK bolometric calibrations from UBV RI and unfiltered measurements that potentially reach 2% precision with a B-V colordependent correction. We observe moderately strong Si γ l6355 as early as +8 days. The photospheric velocity (vph) is determined by modeling the spectra in the vicinity of Fe γ l5169 whenever observed, and interpolating at photometric epochs based on a semianalytic method. This gives vph = 4500 ± 500 km s?1 at +50 days. We also observe spectral homogeneity of ultraviolet spectra at +1012 days for SNe IIP, while variations are evident a week after explosion. Using the expanding photosphere method, from combined analysis of SN 2013ej and SN 2002ap, we estimate the distance to the host galaxy to be 9.0+0.4 -0.6 Mpc, consistent with distance estimates from other methods. Photometric and spectroscopic analysis during the plateau phase, which we estimated to be 94 ± 7 days long, yields an explosion energy of 0.9 ± 0.3 × 1051 erg, a final pre-explosion progenitor mass of 15.2 ± 4.2 Mo and a radius of 250 ± 70 Ro. We observe a broken exponential profile beyond +120 days, with a break point at +183 ± 16 days. Measurements beyond this break time yield a 56Ni mass of 0.013 ± 0.001 Mo.

Original languageEnglish (US)
Article number6
JournalAstrophysical Journal
Volume822
Issue number1
DOIs
StatePublished - May 1 2016

Bibliographical note

Funding Information:
This research was supported by NASA grant NNX10A196H (P.I. Kehoe), NSF grant AST-1109801 (P.I. Wheeler), and Hungarian OTKA grant NN 107637 (P.I. Vinko). J.M.S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. T.S. is funded by OTKA Postdoctoral Fellowship award PD 112325. K.S. has been supported by the Lendulet-2009 program of the Hungarian Academy of Sciences and ESA PECS Contract No. 4000110889/14/NL/NDe.

Keywords

  • galaxies: distances and redshifts
  • supernovae: general
  • supernovae: individual (SN 2013ej)
  • techniques: photometric

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