Multiple High-Velocity Emission-Line Systems in the E+S Pair CPG 29

P. Marziani; W. C. Keel; D. Dultzin--Hacyan; J. W. Sulentic

doi:10.1086/174844

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Multiple High-Velocity Emission-Line Systems in the E+S Pair CPG 29

P. Marziani·W. C. Keel·D. Dultzin--Hacyan·J. W. Sulentic

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Abstract

A detailed study of the mixed-morphology galaxy pair CPG 29 (Arp 119, VV 347) shows spectacular spectroscopic peculiarities in the southern (spiral) component (Mkn 984) including a spatially resolved region, roughly aligned along the minor axis of the galaxy, with multiple emission-line components redshifted by as much as 1300 km s$^{-1}$ with respect to the LINER nucleus. Strong [OI]\l6300 and [SII]ł\l6716,6731 emission suggest shock ionization. The rest of the galaxy's disk is spectroscopically undistinguished, with emission lines characteristic of disk H II regions and, in large part, ordered rotation. We discuss the following four possible explanations for the morphological and spectroscopic peculiarities in the spiral: (1) a super--wind scenario, supported by the high FIR luminosity of the spiral, and by emission line activity similar to that observed in FIR strong galaxies; (2) motion of the spiral through a hot, relatively dense intergalactic medium, possibly associated with the elliptical, that could affect the star formation rate and create a brightened disk rim; (3) a faint companion in direct collision with the disk, at $Δv_r \sim 1000$ \kms, that would straightforwardly explain the existence of the different redshift systems; (4) a pole on collision by the elliptical, that could produce the disturbed morphology and other properties of the spiral. The elliptical/spiral pole--on collision explains the high velocity line emitting regions as tidally stripped gas, and accounts for the presence of gas ionized by moterate velocity shocks. The morphology of Mrk 984 is consistent

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P. Marziani, W. C. Keel, D. Dultzin--Hacyan, J. W. Sulentic. 1994-05-10. Multiple High-Velocity Emission-Line Systems in the E+S Pair CPG 29. https://doi.org/10.1086/174844

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