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The formation mechanism of the hot gaseous halo associated with the Milky WayGalaxy is still under debate. We report new observational constraints on thegaseous halo using 107 lines-of-sight of the Suzaku X-ray observations at$75^{\circ}<l<285^{\circ}$ and $|b|>15^{\circ}$ with a total exposure of 6.4Ms. The gaseous halo spectra are represented by a single-temperature plasmamodel in collisional ionization equilibrium. The median temperature of theobserved fields is 0.26 keV ($3.0\times10^6$ K) with a typical fluctuation of$\sim30$%. The emission measure varies by an order of magnitude and marginallycorrelates with the Galactic latitude. Despite the large scatter of the data,the emission measure distribution is roughly reproduced by a disk-like densitydistribution with a scale length of $\sim7$ kpc, a scale height of $\sim2$ kpc,and a total mass of $\sim5\times10^7$ $M_{\odot}$. In addition, we found that aspherical hot gas with the $\beta$-model profile hardly contributes to theobserved X-rays but that its total mass might reach $\gtrsim10^9$ $M_{\odot}$.Combined with indirect evidence of an extended gaseous halo from otherobservations, the hot gaseous halo likely consists of a dense disk-likecomponent and a rarefied spherical component; the X-ray emissions primarilycome from the former but the mass is dominated by the latter. The disk-likecomponent likely originates from stellar feedback in the Galactic disk due tothe low scale height and the large scatter of the emission measures. The median[O/Fe] of $\sim0.25$ shows the contribution of the core-collapse supernovae andsupports the stellar feedback origin.

Spatial distribution of the Milky Way hot gaseous halo constrained by Suzaku X-ray observations