GASEOUS AND STELLAR COMPONENTS IN MIXED PAIRS OF GALAXIES .1. THE DATA

Isolated mixed morphology pairs are composed of an early and a late ty pe galaxy. They are an ideal laboratory for studying the response of g as to a gravitational instability We present data from a kinematic and photometric study of six mixed pairs. High resolution rotation and ve locity dispersion curves, for both gas and stellar components, are pre sented. Slit orientations were along the major axis of the spiral and, in most of the cases, along the line connecting the galaxy nuclei. B and V luminosity and geometrical profiles are also presented. Photomet ric parameters including effective radius and disk scale length are al so presented. Data on the [N II](6583)/H alpha emission line ratio pro vide a further insight into physical conditions of the gas. Half of th e early-type components show lenticular morphology involving a well. d efined disk. Most late-type components show Grand Design spiral struct ure. Rotation curves of both members appear normal along the axes stud ied. The nuclear region of NGC 5297 is the single case where the gaseo us component shows evidence for an apparent counter rotation relative to the stellar component, probably due to the presence of a bar. There is evidence in the early type member NGC 5953, and possibly also in N GC 5296, that the gas component has been acquired from the spiral memb er of the pair. The gas in these objects is concentrated in nuclear st ar forming regions as deduced from (B - V) color. This may be evidence for mass transfer induced activity (cross-fuelling) in these pairs. T he nuclear gas in NGC 5297, 6962 and E 297-G-8 shows a reversal of the [N II] to Wa: emission line intensity ratio. This indicator along wit h the [O III](5007)/H beta ratio suggests that these nuclei show low l evel (LINER) activity.