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The peculiar spiral NGC 2782 is the result of a minor merger with a massratio ~4:1 occurring ~200 Myr ago. This merger produced a molecular and HIrich, optically bright Eastern tail and an HI-rich, optically faint Westerntail. Non-detection of CO in the Western Tail by Braine et al. (2001) suggestedthat star formation had not yet begun. However, deep UBVR and H-alphanarrowband images show evidence of recent star formation in the Western tail,though it lacks massive star clusters and cluster complexes. Using HerschelPACS spectroscopy, we discover 158 micron [CII] emission at the location of thethree most luminous H-alpha sources in the Eastern tail, but not at thelocation of the even brighter H-alpha source in the Western tail. The Westerntail is found to have a normal star formation efficiency (SFE), but the Easterntail has a low SFE. The lack of CO and [CII] emission suggests the Western tailHII region may have a low carbon abundance and be undergoing its first starformation. The Western tail is more efficient at forming stars, but lacksmassive clusters. We propose that the low SFE in the Eastern tail may be due toits formation as a splash region where gas heating is important even though ithas sufficient molecular and neutral gas to make massive star clusters. TheWestern tail, which has lower gas surface density and does not form high massstar clusters, is a tidally formed region where gravitational compressionlikely enhances star formation.

Tidal Tails of Minor Mergers II: Comparing Star Formation in the Tidal Tails of NGC 2782