2004MNRAS.352.1213C

We present and analyse spectra of the Type IIn supernova (SN) 1994W obtained between 18 and 203d after explosion. During the luminous phase (first 100d) the line profiles are composed of three major components: (I) narrow P-Cygni lines with the absorption minima at -700km/s; (II) broad emission lines with blue velocity at zero intensity ∼4000km/s; and (III) broad, smooth wings extending out to at least ∼5000km/s, most apparent in Hα. These components are identified with an expanding circumstellar (CS) envelope, shocked cool gas in the forward post-shock region, and multiple Thomson scattering in the CS envelope, respectively. The absence of broad P-Cygni lines from the SN is the result of the formation of an optically thick, cool, dense shell at the interface of the ejecta and the CS envelope. Models of the SN deceleration and Thomson scattering wings are used to recover the density (n~ 10⁹/cm3), radial extent [∼(4-5)x10¹⁵cm] and Thomson optical depth (τ_T≳ 2.5) of the CS envelope during the first month. The plateau-like SN light curve is reproduced by a hydrodynamical model and is found to be powered by a combination of internal energy leakage after the explosion of an extended pre-SN (∼10¹⁵cm) and subsequent luminosity from CS interaction. The pre-explosion kinematics of the CS envelope is recovered, and is close to homologous expansion with outer velocity ∼1100km/s and a kinematic age of ∼1.5yr. The high mass (∼0.4M_☉) and kinetic energy (∼2x10⁴⁸erg) of the CS envelope, combined with low age, strongly suggest that the CS envelope was explosively ejected ∼1.5yr prior to the SN explosion.