  In this paper we present the identification of two periodic X-ray signals
coming from the direction of the Small Magellanic Cloud (SMC). On detection
with the Rossi X-ray Timing Explorer (RXTE), the 175.4s and 85.4s pulsations
were considered to originate from new Be/X-ray binary (BeXRB) pulsars with
unknown locations. Using rapid follow-up INTEGRAL and XMM-Newton observations,
we show the first pulsar (designated SXP175) to be coincident with a candidate
high-mass X-ray binary (HMXB) in the northern bar region of the SMC undergoing
a small Type II outburst. The orbital period (87d) and spectral class
(B0-B0.5IIIe) of this system are determined and presented here for the first
time. The second pulsar is shown not to be new at all, but is consistent with
being SXP91.1 - a pulsar discovered at the very beginning of the 13 year long
RXTE key monitoring programme of the SMC. Whilst it is theoretically possible
for accreting neutron stars to change spin period so dramatically over such a
short time, the X-ray and optical data available for this source suggest this
spin-up is continuous during long phases of X-ray quiescence, where accretion
driven spin-up of the neutron star should be minimal.
