Open AccessThe first year of SN 2004dj in NGC 2403 ★
Author(s) -
Vinkó J.,
Takáts K.,
Sárneczky K.,
Szabó Gy. M.,
Mészáros Sz.,
Csorvási R.,
Szalai T.,
Gáspár A.,
Pál A.,
Csizmadia Sz.,
Kóspál A.,
Rácz M.,
Kun M.,
Csák B.,
Fürész G.,
DeBond H.,
Grunhut J.,
Thomson J.,
Mochnacki S.,
Koktay T.
Publication year - 2006
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2006.10416.x
Subject(s) - physics , astrophysics , photometry (optics) , supernova , red supergiant , photosphere , light curve , cepheid variable , population , cosmic distance ladder , spectral energy distribution , type ii supernova , cluster (spacecraft) , astronomy , spectral line , galaxy , supergiant , stars , redshift , demography , sociology , computer science , programming language
New BV RI photometry and optical spectroscopy of the Type IIp supernova 2004dj in NGC 2403, obtained during the first year since discovery, are presented. The progenitor cluster, Sandage 96, is also detected on pre‐explosion frames. The light curve indicates that the explosion occurred about 30 d before discovery, and the plateau phase lasted about +110 ± 20 d after that. The plateau‐phase spectra have been modelled with the synow spectral synthesis code using H, Na i , Ti ii , Sc ii , Fe ii and Ba i lines. The SN distance is inferred from the expanding photosphere method and the standard candle method applicable for SNe IIp. They resulted in distances that are consistent with each other as well as earlier Cepheid and Tully–Fisher distances. The average distance, D = 3.47 ± 0.29 Mpc is proposed for SN 2004dj and NGC 2403. The nickel mass produced by the explosion is estimated as ∼0.02 ± 0.01 M ⊙ . The spectral energy distribution of the progenitor cluster is reanalysed by fitting population synthesis models to our observed BV RI data supplemented by U and JHK magnitudes from the literature. The χ 2 minimization revealed a possible ‘young’ solution with cluster age T cl = 8 Myr , and an ‘old’ solution with T cl = 20–30 Myr . The ‘young’ solution would imply a progenitor mass M > 20 M ⊙ , which is higher than the previously detected progenitor masses for Type II SNe.