  We present BIMA and SCUBA observations of the young cluster associated with
BD +40 4124 in the dense molecular gas tracer CS J=2-1 and the continuum dust
continuum at 3.1 mm and 850 micron. The dense gas and dust in the system is
aligned into a long ridge morphology extending ~0.4 pc with 16 gas clumps of
estimated masses ranging from 0.14 - 1.8 Solar masses. A north-south variation
in the CS center line velocity can be explained with a two cloud model. We
posit that the BD +40 4124 stellar cluster formed from a cloud-cloud collision.
The largest linewidths occur near V1318 Cyg-S, a massive star affecting its
natal environment. In contrast, the dense gas near the other, more evolved,
massive stars displays no evidence for disruption; the material must either be
processed into the star, dissipate, or relax, fairly quickly. The more evolved
low-mass protostars are more likely to be found near the massive stars. If the
majority of low-mass stars are coeval, the seemingly evolved low-mass
protostars are not older: the massive stars have eroded their structures.
Finally, at the highest resolution, the 3.1 mm dust emission is resolved into a
flattened structure 3100 by 1500 AU with an estimated mass of 3.4 Solar masses.
The continuum and CS emission are offset by 1.1 arcsec from the southern binary
source. A simple estimate of the extinction due to the continuum emission
structure is AV = 700 mag. From the offset and as the southern source is
detected in the optical, the continuum emission is from a previously unknown
very young, intermediate-mass, embedded stellar object. (see high resolution
figures at http://eeyore.astro.uiuc.edu/~lwl/recent/bd40.pdf).
