The Supernova Remnant Population of NGC 6946 as Observed in [Fe ii] 1.644 μm with HST*

Abstract

Abstract NGC 6946 is a high-star-formation-rate, face-on, spiral galaxy that has hosted 10 supernovae since 1917. Not surprisingly, a large number of supernova remnants and candidates have been identified either as optical nebulae with high [S ii]:Hα line ratios (147) or as compact non-thermal radio sources (35). However, there are only seven overlaps between these two samples. Here, we apply [Fe ii] 1.644 μm emission as a new diagnostic to search for supernova remnants in an attempt to resolve this discrepancy. [Fe ii] is expected to be relatively strong in the radiative shocks of supernova remnants and almost absent in H ii regions. It is less susceptible to the effects of absorption along the line of sight than the optical lines normally used to identify remnants. Using data from the WFC3 camera on Hubble Space Telescope (HST), we identify 132 [Fe ii] emission nebulae in NGC 6946 as likely supernova remnants. Of these, 54 align with previously known optical supernova remnants. The remaining 78 objects are new; of these 44 are visible in new HST imagery in Hα and [S ii]. This brings the total number of supernova remnant candidates (from optical and/or IR data) in NGC 6946 to 225. A total of 14 coincidences with radio supernova remnant candidates (out of 30 in our search area) are found in this expanded list. The identification of so many new remnant candidates validates the use of [Fe ii] imagery for finding remnants, and suggests that previous remnant searches in other galaxies may be far from complete.