Details

Autor(en) / Beteiligte

• Sand, D. J.
• Seth, A. C.
• Crnojevi, D.
• Spekkens, K.
• Strader, J.
• Adams, E. A. K.
• Caldwell, N.
• Guhathakurta, P.
• Kenney, J.
• Randall, S.
• Simon, J. D.
• Toloba, E.
• Willman, B.

Titel

Hubble Space Telescope Imaging of the Ultra-compact High Velocity Cloud AGC 226067: A Stripped Remnant in the Virgo Cluster

Ist Teil von

• The Astrophysical journal, 2017-07, Vol.843 (2), p.134

Ort / Verlag

Philadelphia: The American Astronomical Society

Erscheinungsjahr

2017

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• 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 MV = −11.3 0.3, or Mstars = 5.4 1.3 × 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.