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After discovery of the Fermi bubbles, giant structures observed in radio toX-rays have been discussed as possi- ble evidence of past activities in theGalactic Center (GC). We report here on the analysis of Suzaku data pointingaround the Loop I arc. The diffuse X-ray emission was well represented by thethree-component model: (1) an unabsorbed thermal plasma with kT ~ 0.1 keVeither from the Local Hot Bubble (LHB) and/or solar wind charge exchange(SWCX), (2) an absorbed thermal plasma regarded as a contribution from the LoopI and the Galactic halo (GH), and (3) an absorbed power-law componentrepresenting the cosmic X-ray background. The temper- ature of the absorbedthermal plasma was clustered in a range of 0.30 +- 0.02 keV along Loop I ("ON"regions), whereas the temperature was about 20 % lower in the cavity adjacentto the bubbles and Loop I ("OFF" regions) with 0.24 +- 0.03 keV. The emissionmeasure (EM) varied along the Galactic latitude, and was well correlated withthe count rate variation as measured with the ROSAT in 0.75 keV band. Althoughthe amount of neutral gas was not conclusive to constrain on the distance toLoop I, the observed EM values rule out a hypothesis that the structure isclose to the Sun; we argue that the Loop I is a distant, kpc structure of theshock-heated GH gas. We discuss the origin of apparent mismatch in themorphologies of the Fermi bubbles and the Loop I arc, suggesting a two-stepexplosion process in the GC.

Diffuse x-ray emission from the northern arc of loop I observed with suzaku