  We combined Chandra ACIS observations of the globular cluster 47 Tucanae
(hereafter, 47 Tuc) from 2000, 2002, and 2014-15 to create a deeper X-ray
source list, and study some of the faint radio millisecond pulsars (MSPs)
present in this cluster. We have detected 370 X-ray sources within the
half-mass radius (2$'$.79) of the cluster, 81 of which are newly identified, by
including new data and using improved source detection techniques. The majority
of the newly identified sources are in the crowded core region, indicating
cluster membership. We associate five of the new X-ray sources with
chromospherically active BY Dra or W UMa variables identified by Albrow et al.
(2001). We present alternative positions derived from two methods, centroiding
and image reconstruction, for faint, crowded sources. We are able to extract
X-ray spectra of the recently discovered MSPs 47 Tuc aa, 47 Tuc ab, the newly
timed MSP 47 Tuc Z, and the newly resolved MSPs 47 Tuc S and 47 Tuc F.
Generally, they are well fit by black body or neutron star atmosphere models,
with temperatures, luminosities and emitting radii similar to those of other
known MSPs in 47 Tuc, though 47 Tuc aa and 47 Tuc ab reach lower X-ray
luminosities. We limit X-ray emission from the full surface of the rapidly
spinning (542 Hz) MSP 47 Tuc aa, and use this limit to put an upper bound for
amplitude of r-mode oscillations in this pulsar as $\alpha<2.5\times 10^{-9}$
and constrain the shape of the r-mode instability window.
