The Complexity of the Cetus Stream Unveiled from the Fusion of
  STREAMFINDER and StarGO
  We combine the power of two stream-searching tools, STREAMFINDER and StarGO
applied to the Gaia EDR3 data, to detect stellar debris belonging to the Cetus
stream system that forms a complex, nearly polar structure around the Milky
Way. In this work, we find the southern extensions of the northern Cetus stream
as the Palca stream and a new southern stream, which overlap on the sky but
have different distances. These two stream wraps extend over more than
$\sim100\deg$ on the sky ($-60\deg<\delta<+40\deg$). The current N-body model
of the system reproduces both wraps in the trailing arm. We also show that the
Cetus system is confidently associated with the Triangulum/Pisces, Willka Yaku,
and the recently discovered C-20 streams. The association with the ATLAS-Aliqa
Uma stream is much weaker. All of these stellar debris are very metal-poor,
comparable to the average metallicity of the southern Cetus stream with [Fe/H]
= $-2.17\pm0.2$. The estimated stellar mass of the Cetus progenitor is at least
$10^{5.6}\rm\,M_\odot$, compatible with Ursa Minor or Draco dwarf galaxies. The
associated globular cluster with similar stellar mass, NGC 5824 very possibly
was accreted in the same group infall. The multi-wrap Cetus stream is a perfect
example of a dwarf galaxy that has undergone several periods of stripping,
leaving behind debris at multiple locations in the halo. The full
characterization of such systems is crucial to unravel the assembly history of
the Milky Way and, as importantly, to provide nearby fossils to study ancient
low-mass dwarf galaxies.
