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We present a detailed spectroscopic study of the hot gas toward the Galacticbulge along the 4U 1820-303 sight line by a combination analysis of emissionand absorption spectra. In addition to the absorption lines of OVII Kalpha,OVII Kbeta, OVIII Kalpha and NeIX Kalpha by Chandra LTGS as shown by previousworks, Suzaku detected clearly the emission lines of OVII, OVIII, NeIX and NeXfrom the vicinity. We used simplified plasma models with constant temperatureand density. Evaluation of the background and foreground emission was performedcarefully, including stellar X-ray contribution based on the recent X-rayobservational results and stellar distribution simulator. If we assume that oneplasma component exists in front of 4U1820-303 and the other one at the back,the obtained temperatures are T= 1.7 +/- 0.2 MK for the front-side plasma andT=3.9(+0.4-0.3) MK for the backside. This scheme is consistent with a hot andthick ISM disk as suggested by the extragalactic source observations and anX-ray bulge around the Galactic center.

An X-ray Spectroscopic Study of the Hot Interstellar Medium Toward the Galactic Bulge