On The Nature of ultra-faint Dwarf Galaxy Candidates II: The case of
  Cetus II
  We obtained deep Gemini GMOS-S $g,r$ photometry of the ultra-faint dwarf
galaxy candidate Cetus II with the aim of providing stronger constraints on its
size, luminosity and stellar population. Cetus II is an important object in the
size-luminosity plane as it occupies the transition zone between dwarf galaxies
and star clusters. All known objects smaller than Cetus II ($r_h \sim 20$ pc)
are reported to be star clusters, while most larger objects are likely dwarf
galaxies. We found a prominent excess of main-sequence stars in the
colour-magnitude diagram of Cetus II, best described by a single stellar
population with an age of 11.2 Gyr, metallicity of [Fe/H] = $-1.28$ dex, an
[$\alpha$/Fe] = 0.0 dex at a heliocentric distance of 26.3$\pm$1.2 kpc. As well
as being spatially located within the Sagittarius dwarf tidal stream, these
properties are well matched to the Sagittarius galaxy's Population B stars.
Interestingly, like our recent findings on the ultra-faint dwarf galaxy
candidate Tucana V, the stellar field in the direction of Cetus II shows no
evidence of a concentrated overdensity despite tracing the main sequence for
over six magnitudes. These results strongly support the picture that Cetus II
is not an ultra-faint stellar system in the Milky Way halo, but made up of
stars from the Sagittarius tidal stream.
