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IGR J16493-4348 is an eclipsing supergiant high-mass X-ray binary (sgHMXB),where accretion onto the compact object occurs via the radially outflowingstellar wind of its early B-type companion. We present an analysis of thesystem's X-ray variability and periodic modulation using pointed observations(2.5-25 keV) and Galactic bulge scans (2-10 keV) from the Rossi X-ray TimingExplorer (RXTE) Proportional Counter Array (PCA), along with Swift Burst AlertTelescope (BAT) 70-month snapshot (14-195 keV) and transient monitor (15-50keV) observations. The orbital eclipse profiles in the PCA bulge scans and BATlight curves are modeled using asymmetric and symmetric step and rampfunctions. We obtain an improved orbital period measurement of 6.7828 $\pm$0.0004 days from an observed minus calculated (O-C) analysis of mid-eclipsetimes derived from the BAT transient monitor and PCA scan data. No evidence isfound for the presence of a strong photoionization or accretion wake. We refinethe superorbital period to 20.067 $\pm$ 0.009 days from the discrete Fouriertransform (DFT) of the BAT transient monitor light curve. A pulse period of1093.1036 $\pm$ 0.0004 s is measured from a pulsar timing analysis usingpointed PCA observations spanning $\sim$1.4 binary orbits. We present pulsetimes of arrival (ToAs), circular and eccentric timing models, and calculationsof the system's Keplerian binary orbital parameters. We derive an X-ray massfunction of $f_{x}(M)$ $=$ 13.2$^{+2.4}_{-2.5}$ $M_{\odot}$ and find a spectraltype of B0.5 Ia for the supergiant companion through constraints on the massand radius of the donor. Measurements of the eclipse half-angle and additionalparameters describing the system geometry are provided.

The Orbital Parameters of the Eclipsing High-Mass X-ray Binary Pulsar IGR J16493-4348 from Pulsar Timing