Cloud Structure of Galactic OB Cluster Forming Regions from Combining
  Ground and Space Based Bolometric Observations
  We have developed an iterative procedure to systematically combine the
millimeter and submillimeter images of OB cluster-forming molecular clouds,
which were taken by ground based (CSO, JCMT, APEX, IRAM-30m) and space
telescopes (Herschel, Planck). For the seven luminous ($L$$>$10$^{6}$
$L_{\odot}$) Galactic OB cluster-forming molecular clouds selected for our
analyses, namely W49A, W43-Main, W43-South, W33, G10.6-0.4, G10.2-0.3,
G10.3-0.1, we have performed single-component, modified black-body fits to each
pixel of the combined (sub)millimeter images, and the Herschel PACS and SPIRE
images at shorter wavelengths. The $\sim$10$"$ resolution dust column density
and temperature maps of these sources revealed dramatically different
morphologies, indicating very different modes of OB cluster-formation, or
parent molecular cloud structures in different evolutionary stages. The
molecular clouds W49A, W33, and G10.6-0.4 show centrally concentrated massive
molecular clumps that are connected with approximately radially orientated
molecular gas filaments. The W43-Main and W43-South molecular cloud complexes,
which are located at the intersection of the Galactic near 3-kpc (or Scutum)
arm and the Galactic bar, show a widely scattered distribution of dense
molecular clumps/cores over the observed $\sim$10 pc spatial scale. The
relatively evolved sources G10.2-0.3 and G10.3-0.1 appear to be affected by
stellar feedback, and show a complicated cloud morphology embedded with
abundant dense molecular clumps/cores. We find that with the high angular
resolution we achieved, our visual classification of cloud morphology can be
linked to the systematically derived statistical quantities (i.e., the enclosed
mass profile, the column density probability distribution function, the
two-point correlation function of column density, and the probability
distribution function of clump/core separations).
