Cloud G074.11+00.11: a stellar cluster in formation
  We present molecular line and dust continuum observations of a
Planck-detected cold cloud, G074.11+00.11. The cloud consists of a system of
curved filaments and a central star-forming clump. The clump is associated with
several infrared sources and H2O maser emission. We aim to determine the mass
distribution and gas dynamics within the clump, to investigate if the
filamentary structure seen around the clump repeats itself on a smaller scale,
and to estimate the fractions of mass contained in dense cores and filaments.
The velocity distribution of pristine dense gas can be used to investigate the
global dynamical state of the clump, the role of filamentary inflows, filament
fragmentation and core accretion. We use molecular line and continuum
observations from single dish observatories and interferometric facilities to
study the kinematics of the region. The molecular line observations show that
the central clump may have formed as a result of a large-scale filament
collision. The central clump contains three compact cores. Assuming a distance
of 2.3 kpc, based on Gaia observations and a three-dimensional extinction
method of background stars, the mass of the central clump exceeds 700 solar
masses, which is roughly 25% of the total mass of the cloud. Our virial
analysis suggests that the central clump and all identified substructures are
collapsing. We find no evidence for small-scale filaments associated with the
cores. Our observations indicate that the clump is fragmented into three cores
with masses in the range [10,50] solar masses and that all three are
collapsing. The presence of an H2O maser emission suggests active star
formation. However, the CO lines show only weak signs of outflows. We suggest
that the region is young and any processes leading to star formation have just
recently begun.
