2017ApJ...843..134S

We analyze the optical counterpart to the ultra-compact high velocity cloud AGC 226067, utilizing imaging taken with the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope. The color-magnitude diagram of the main body of AGC 226067 reveals an exclusively young stellar population, with an age of ∼7-50 Myr, and is consistent with a metallicity of [Fe/H] ∼ -0.3 as previous work has measured via H II region spectroscopy. Additionally, the color-magnitude diagram is consistent with a distance of D ≃ 17 Mpc, suggesting an association with the Virgo cluster. A secondary stellar system located ∼1.'6 (∼8 kpc) away in projection has a similar stellar population. The lack of an old red giant branch (>=5 Gyr) is contrasted with a serendipitously discovered Virgo dwarf in the ACS field of view (Dw J122147+132853), and the total diffuse light from AGC 226067 is consistent with the luminosity function of the resolved ∼7-50 Myr stellar population. The main body of AGC 226067 has a M_V = -11.3 ± 0.3, or M_stars = 5.4 ± 1.3 x 10⁴ M_☉ given the stellar population. We searched 20 deg² of imaging data adjacent to AGC 226067 in the Virgo Cluster, and found two similar stellar systems dominated by a blue stellar population, far from any massive galaxy counterpart-if this population has star-formation properties that are similar to those of AGC 226067, it implies ∼0.1 M_☉ yr^–1 in Virgo intracluster star formation. Given its unusual stellar population, AGC 226067 is likely a stripped remnant and is plausibly the result of compressed gas from the ram pressure stripped M86 subgroup (∼350 kpc away in projection) as it falls into the Virgo Cluster.