region W4 [@Lada:1978aa; @Thronson:1985aa]. One of our goals is to trace the formation of distinct embedded clusters in this region and to attempt to reconstruct the star forming history of the cloud. The W3 Complex is located at a distance of 2.04$\pm$0.107 kpc [^2], and has hosted at least three major episodes of recent cluster formation. According to spectroscopic studies, IC 1795 formed first, about 3-5 Myr [@Oey:2005ly] ago, followed by the W3 “main" cluster located to its West edge, and the W3(OH) cluster group to the East, both with ages of 2-3 Myr [@Bik:2012aa; @Navarete:2011ys]. It has been suggested that IC 1795 triggered the other two episodes in a hierarchical progression [@Oey:2005ly]. The Chandra study by [@Feigelson:2008vn] suggested that the clusters in W3 extend widely and are highly structured, with sources located at relatively large distances from the dynamical centers, including a relatively isolated O star that might have escaped from the main cluster.

In two recent studies, @Rivera-Ingraham:2011yq [@Rivera-Ingraham:2013fj] made use of mid-infrared photometry and far-IR emission mapping from the Spitzer and Herschel[^3] space observatories, that comprise the entire W3 region. They were able to catalog hundreds of young stellar sources (YSOs) across the complex and determine their 