The StEllar Counterparts of COmpact high velocity clouds (SECCO) survey. I. Photos of ghosts

TL;DR

This survey searched for stellar counterparts of ultra-compact high-velocity HI clouds using the Large Binocular Telescope but found no evidence of associated dwarf galaxies within 1.5 Mpc, suggesting these clouds are unlikely to be typical Local Group dwarfs.

Contribution

The first wide-field imaging survey targeting the stellar counterparts of UCHVCs, providing constraints on their nature and ruling out typical dwarf galaxy associations.

Findings

No stellar counterparts detected for most UCHVCs.

Survey sensitivity rules out dwarf galaxies brighter than M_V=-8 within 1.5 Mpc.

Most UCHVCs are unlikely to be associated with known dwarf galaxies.

Abstract

We present an imaging survey aimed at searching for the stellar counterparts of recently discovered ultra-compact high-velocity HI clouds (UCHVC). Adams et al. (2013) proposed these clouds to be candidate mini-haloes in the Local Group and/or its surroundings, within a distance range of 0.25-2.0 Mpc. Using the Large Binocular Telescope we obtain wide-field (~ 23' X 23') g- and r-band images of the twenty-five most promising and most compact clouds among the fifty-nine identified by Adams et al. Careful visual inspection of all the images does not reveal any stellar counterpart even slightly resembling LeoP, the only local dwarf galaxy that was found as a counterpart to a previously detected high velocity cloud. Only a possible distant (D>3.0 Mpc) counterpart to HVC274.68+74.70-123 has been identified on our images. The point source photometry in the central 17.3' X 7.7' chips reaches r<= 26.5, and is expected to contain most of the stellar counterparts to the UCHVCs. However, no obvious stellar over-density is detected in any of our fields, in marked contrast to our comparison LeoP field in which the dwarf galaxy is detected at a >30 sigma significance level. Only HVC352.45+59.06+263 may be associated with a weak over-density, whose nature cannot be ascertained with our data. Sensitivity tests shows that our survey would have detected any dwarf galaxy dominated by an old stellar population, with an integrated absolute magnitude M_V<= -8.0, a half-light radius r_h<= 300 pc, and lying within 1.5 Mpc from us, thereby confirming that it is unlikely that the observed UCHVCs are associated with stellar counterparts typical of known Local Group dwarf galaxies.