Spectra of the Remnant of Sn 1885 in M 31

Near UV HST images of the remnant of SN 1885 (S And) in M31 show a 0. 70 ± 0. 05 diameter absorption disk silhouetted against M31’s central bulge, at SN 1885’s historically reported position. The disk’s size corresponds to a linear diameter of 2.5 ± 0.4 pc at a distance of 725 ±70 kpc, implying an average expansion velocity of 11000 ± 2000 kms over 110 years. Low-dispersion FOS spectra over 3200–4800 Å reveal that the absorption arises principally from Ca II H & K (equivalent width ≃ 215 Å), with weaker absorption features of Ca I 4227 Å and Fe I 3720 Å. The flux at Ca II line center indicates a foreground starlight fraction of 0.21, which places SNR 1885 some 64 pc to the near side of the midpoint of the M31 bulge, comparable to its projected 55 pc distance from the nucleus. The absorption line profiles suggest an approximately spherically symmetric, bell-shaped density distribution of supernova ejecta freely expanding at up to 13100 ± 1500 kms. We estimate Ca I, Ca II, and Fe I masses of 2.9 −0.6 × 10 −4 M⊙, 0.005 +0.016 −0.002 M⊙, and 0.013 +0.010 −0.005 M⊙ respectively. If the ionization state of iron is similar to the observed ionization state of calcium, MCaII/MCaI = 16 +42 −5 , then the mass of Fe II is 0.21 −0.08 M⊙, consistent with that expected for either normal or subluminous SN Ia. Subject headings: galaxies: individual (M31) — ISM: supernova remnants — stars: supernovae: individual (SN 1885) — ultraviolet: galaxies — ultraviolet: ISM