Abstract
We report the detection of ongoing star formation in the prominent tidal arms near NGC 3077 (member of the M81 triplet). In total, 36 faint compact H II regions are identified, covering an area of ~4 × 6 kpc2. Most of the H II regions are found at H I column densities above 1 × 1021 cm-2 (on scales of 200 pc), well within the range of threshold columns measured in normal galaxies. The H II luminosity function resembles those derived for other low-mass dwarf galaxies in the same group; we derive a total star formation rate of 2.3 × 10-3 M⊙ yr-1 in the tidal feature. We also present new high-resolution imaging of the molecular gas distribution in the tidal arm using CO observations obtained with the Owens Valley Radio Observatory interferometer. We recover about one-sixth of the CO flux (or M ~ 2 × 106 M⊙, assuming a Galactic conversion factor) originally detected in the IRAM 30 m single-dish observations, indicating the presence of a diffuse molecular gas component in the tidal arm. The brightest CO peak in the interferometer map (comprising half of the detected CO flux) is coincident with one of the brightest H II regions in the feature. Assuming a constant star formation rate since the creation of the tidal feature (presumably ~3 × 108 yr ago), a total mass of ~7 × 105 M⊙ has been transformed from gas into stars. Over this period the star formation in the tidal arm has resulted in an additional enrichment of ΔZ > 0.002. The reservoir of atomic and molecular gas in the tidal arm is ~3 × 108 M⊙, allowing star formation to continue at its present rate for a Hubble time. Such widespread, low-level star formation would be difficult to image around more distant galaxies but may be detectable through intervening absorption in quasar spectra.
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