We study a gas-rich merging dwarf system KUG 0200-096. Deep optical imaging reveals an optically faint tail with a length of 20 kpc, giving a visual impression of tidal antenna similar to NGC 4038/39. The interacting dwarf galaxies have B-band absolute magnitudes of -18.06 and -16.63 mag. We identify a young stellar clump with a stellar mass of 2 × 107 M o at the tip of the antenna, possibly a tidal dwarf galaxy (TDG). The putative TDG candidate is quite blue with a g - r color index of -0.07 mag, whereas the interacting dwarf galaxies have g - r color indices 0.29 and 0.19 mag. The TDG is currently forming stars at the rate of 0.02 M o yr-1. We obtained H i 21 cm line data of KUG 0200-096 using the Giant Metrewave Radio Telescope to get a more detailed view of neutral hydrogen (H i) emission in interacting dwarf galaxies and its TDG. Evidence of a merger between the dwarf galaxy pair is also present in H i kinematics and morphology where we find the H i contents of the interacting pair is disturbed, forming an extended tail toward the TDG. The H i velocity field shows a strong gradient along the H i tidal tail extension. We present a comparative study between the Antennae galaxy, NGC 4038/39, and KUG 0200-096 in both optical and H i gas properties and discuss the possible origin of the KUG 0200-096 TDG.
Bibliographical noteFunding Information:
P.S. and S.-J.Y. acknowledge support by the Samsung Science & Technology Foundation under Project Number SSTF-BA1501-06. S.-J.Y. acknowledges support from the Center for Galaxy Evolution Research (No. 2017R1A5A1070354) through the NRF of Korea and from the Yonsei University Observatory–KASI Joint Research Program (2018).
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science