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<jats:title>Abstract</jats:title> <jats:p>We present initial results from the <jats:italic>K</jats:italic>-band Focal Plane Array Examinations of Young STellar Object Natal Environments survey, a large project on the 100 m Green Bank Telescope mapping ammonia emission across 11 giant molecular clouds at distances of 0.9–3.0 kpc (Cygnus X North, Cygnus X South, M16, M17, Mon R1, Mon R2, NGC 2264, NGC 7538, <jats:italic>Rosette</jats:italic>, W3, and W48). This data release includes the NH<jats:sub>3</jats:sub> (1,1) and (2,2) maps for each cloud, which are modeled to produce maps of kinetic temperature, centroid velocity, velocity dispersion, and ammonia column density. Median cloud kinetic temperatures range from 11.4 ± 2.2 K in the coldest cloud (Mon R1) to 23.0 ± 6.5 K in the warmest cloud (M17). Using dendrograms on the NH<jats:sub>3</jats:sub> (1,1) integrated intensity maps, we identify 856 dense gas clumps across the 11 clouds. Depending on the cloud observed, 40%–100% of the clumps are aligned spatially with filaments identified in H<jats:sub>2</jats:sub> column density maps derived from spectral energy distribution fitting of dust continuum emission. A virial analysis reveals that 523 of the 835 clumps (∼63%) with mass estimates are bound by gravity alone. We find no significant difference between the virial parameter distributions for clumps aligned with the dust-continuum filaments and those unaligned with filaments. In some clouds, however, hubs or ridges of dense gas with unusually high mass and low virial parameters are located within a single filament or at the intersection of multiple filaments. These hubs and ridges tend to host water maser emission, multiple 70 <jats:italic>μ</jats:italic>m detected protostars, and have masses and radii above an empirical threshold for forming massive stars.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Nearby blue compact dwarf (BCD) galaxies are arguably our best local analogs of galaxies in the earlier universe that may host relics of black hole (BH) seeds. Here we present high-resolution <jats:italic>Chandra X-ray Observatory</jats:italic> and Karl G. Jansky Very Large Array observations of five nearby BCDs with stellar masses of less than the Small Magellanic Cloud (<jats:italic>M</jats:italic> <jats:sub>⋆</jats:sub> ∼ 10<jats:sup>7</jats:sup>–10<jats:sup>8.4</jats:sup> <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>). We search for signatures of accreting massive BHs at X-ray and radio wavelengths, which are more sensitive to lower BH accretion rates than optical searches. We detect a total of 10 hard X-ray sources and 10 compact radio sources at luminosities consistent with star-formation-related emission. We find one case of a spatially coincident X-ray and radio source within the astrometric uncertainties. If the X-ray and radio emission are indeed coming from the same source, the origin of the radiation is plausibly from an active massive BH with log (<jats:italic>M</jats:italic> <jats:sub>BH</jats:sub>/<jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub>) ∼ 4.8 ± 1.1. However, given that the X-ray and radio emission are also coincident with a young star cluster complex, we consider the combination of an X-ray binary and a supernova remnant (or H <jats:sc>ii</jats:sc> region) a viable alternative explanation. Overall, we do not find compelling evidence for active massive BHs in our target BCDs, which on average have stellar masses more than an order of magnitude lower than previous samples of dwarf galaxies found to host massive BHs. Our results suggest that moderately accreting massive BHs in BCDs are not so common as to permit unambiguous detection in a small sample.</jats:p>