ratios by means of a two pass sky subtraction method, and combining reduced frames with an optimized centroid offset calculation. We used dark frames and dome flats obtained within 48 hours of each observation. The final combined product images were then analyzed with a second pipeline, [see @Levine:2006ab], which identifies all possible sources from a given field using the `SExtractor` algorithm [@Bertin:1996aa]. We improved the `SExtractor` detection efficiency in the near-IR images by using a Gaussian convolution filter and maximum deblending [see @Bertin:1996aa]. The pipeline then performs `Daophot` PSF photometry [@Stetson:1987aa], calibrates observed magnitudes to a zero point and finds accurate astrometric solutions.

After astrometric solutions were found, individual field images were combined into mosaics using `Montage` [^4]. In Figure \[fig:JHKmosaic\] we show a RGB panorama constructed from a combination of the $J,\ H\mathrm{\ and\ }K$ mosaics. The image represents a complete spatial coverage of the IC 1795, W3-Main and W3-OH clusters. In the near-infrared the region is transparent to most of the prominent regions of nebulosity and obscuration observable in optical images [e.g. @Ogura:1976aa]. The near-IR images at W3(OH) are particularly interesting because they reveal, with unprecedented detail, several small, embedded stellar groups that lie in a small “chain" 