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Fig. 8


A possible interaction scenario of the pair. A few 100 Myr ago, the two galaxies may have gone through a close encounter, tidally pulling out the gas from their outer disks. The intergalactic Hi hinted by the HIPASS data must be part of the tidally stripped gas. Based on the direction of the gas tail of ESO 435IG 020 and the star formation/interaction timescale between the pair, two galaxies are inferred to be moving away from each other rather than being on the way to the second encounter. However, the main kinematic axis might still be dragged toward the interaction counterpart, generating torque on the disk (more effectively on the gas component), which can be clearly seen only in ESO 435G 016 where the structure is better resolved than ESO 435IG 020, at the resolution probed in this work. The recent bursts of star formation are likely to have been triggered by the shear on the gas disk and/or the re-accretion of the stripped gas.

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