The Interstellar Line of Sight to the Interacting Galaxy NGC 5195

Abstract

We present moderately high-resolution echelle observations of the nucleus of NGC 5195, the line of sight to which samples intervening interstellar material associated with the outer spiral arm of M51. Our spectra reveal absorption from interstellar Na i, K i, Ca ii, and CH+, and from a number of diffuse interstellar bands (DIBs), at a velocity close to that exhibited by H i 21 cm emission from M51 at the position of NGC 5195. The H i column density implied by the equivalent width of the λ5780.5 DIB, based on the relationship between Wλ(5780.5) and N(H i) derived for sight lines in the local Galactic interstellar medium, is consistent with the column density obtained from the integrated H i emission. The H2 column density predicted from the observed column density of K i, using the Galactic relationship between N (K i) and N(H2), is comparable to N (H i), suggesting a high molecular fraction (∼0.65) for the M51 gas toward NGC 5195. The DIBs toward NGC 5195 are, on average, ∼40% weaker than would be expected based on the K i column density, a further indication that the gas in this direction has a high molecular content. The M51 material is characterized also by a high N(Na i)/N(Ca ii) ratio (≳11), indicative of a high degree of Ca depletion, and a high Wλ(5797.1)/Wλ(5780.5) ratio (∼1.6), suggestive of either a very weak ambient radiation field or a significantly shielded environment. A high N(CH+)/N(CH) ratio (≳2.3) for the M51 material toward NGC 5195 may be the result of enhanced turbulence due to interactions between M51 and its companion.