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A satisfactory explanation for the observed structure of the diffuse Galactic X-ray background has been elusive. It has been suggested that the soft ($\sim$0.25 keV) component is emission from the Local Hot Bubble (LHB) while several components may contribute to the hard ($\sim$0.5$-$2.0 keV) emission which is observed to be uncorrelated with Galactic latitude. We have begun a program which will utilize the archival ROSAT PSPC data to analyze both the soft and the hard components of the diffuse Galactic X-ray emission. We will mosaic some 60 pointed observations along the Galactic plane covering more than a 100 degree$^{2}$ region between $l_{II}$ = 0$^{\circ}$ and $l_{II}$ = 30$^{\circ}$ and $\left|b_{II} \right|$ $\leq$ 3$^{\circ}$. The average exposure over this field is $\sim$15,000 sec. We will present some of the early work we have carried out for a small region of the total field and describe the procedures we will employ in the subsequent program. Early results from some selected small regions will be discussed.
