  We have spectroscopically identified 60 Galactic Wolf-Rayet (WR) stars,
including 38 nitrogen types (WN) and 22 carbon types (WC). Using photometry
from the Spitzer/GLIMPSE and 2MASS databases, the WRs were selected via a
method we have established that exploits their unique infrared colors, which is
mainly the result of excess radiation from free-free scattering within their
dense ionized winds. The selection criteria has been refined since our last
report, and now yields WRs at a rate of ~20% in spectroscopic follow-up of
candidates that comprise a broad color space defined by the color distribution
of all known WRs having B>14 mag. However, there are subregions within the
broad color space which yield WRs at a rate of >50%. Cross-correlation of WR
candidates with archival X-ray point-source catalogs increases the WR detection
rate of the broad color space to ~40%; ten new WR X-ray sources have been
found, in addition to a previously unrecognized X-ray counterpart to a known
WR. The extinction values, distances, and galactocentric radii of all new WRs
are calculated using the method of spectroscopic parallax. Although the
majority of the new WRs have no obvious association with stellar clusters, two
WC8 stars reside in a previously unknown massive-star cluster that lies near
the intersection of the Scutum-Centaurus Arm and the Galaxy's bar, in which
five OB supergiants were also identified. In addition, two WC and four WN stars
were identified in association with the stellar clusters Danks 1 and 2. A WN9
star has also been associated with the cluster [DBS2003] 179. This work brings
the total number of known Galactic WRs to 476, or ~7-8% of the total
empirically estimated population. An examination of their Galactic distribution
reveals a tracing of spiral arms and an enhanced WR surface density toward
several massive-star formation sites (abridged).
