Detection of CO(1−0) Emission at the Tips of the Tidal Tail in the Antennae Galaxies

Abstract

The tip of the tidal tail, resulting from an encounter between galaxies, features gas concentrations and some star-forming regions, such as tidal dwarf galaxies (TDGs). This region provides a unique laboratory for examining the star formation process in a dynamical environment distinct from that of disk galaxies. Using the Nobeyama 45 m telescope, we conducted ^12 CO(1−0) position-switching observations at the tips of the southern tidal tail in the Antennae galaxies. We detected CO emission not only from the two star-forming TDG candidates but also in regions with no significant star formation. Adopting a Galactic CO-to-H _2 conversion factor without helium correction, the H _2 gas surface density is ∼5–12 M _⊙ pc ^−2 . In most regions, the molecular-to-atomic gas ratio is around unity (0.6–1.9), but we find a region with a high ratio with a 3 σ lower limit of >7.2. The star formation efficiency (SFE) of molecular gas is notably low (<0.15 Gyr ^−1 ), indicating less active star formation than in both nearby disk galaxies (∼0.5–1.0 Gyr ^−1 ) and other TDGs previously observed. Including previous observations, the molecular gas SFEs vary widely among TDGs/tidal tails, from 10 ^−2 to 10 Gyr ^−1 , demonstrating significant variations in star formation activity. Potential factors contributing to the low SFE in the Antennae tail tips include extensive tides and/or the young age of the tail.

Keywords

• Star formation
• Interstellar medium
• Molecular gas
• Galaxy interactions
• Tidal tails
• CO line emission