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X-ray observations of highly ionized metal absorption lines at z=0 providecritical information of the hot gas distribution in and around the Milky Way.We present a study of more than ten-year Chandra and XMM-Newton observations of3C 273, one of the brightest extragalactic X-ray sources. Compared withprevious work, We obtain much tighter constraints of the physical properties ofthe X-ray absorber. We also find a large, non-thermal velocity at ~ 100 - 150km/s is the main reason for the higher line equivalent width when compared withother sightlines. Using joint analysis with X-ray emission and ultravioletobservations, we derive a size of 5 - 15 kpc and a temperature of (1.5-1.8)10^6 K for the X-ray absorber. The 3C 273 sightline passes through a number ofGalactic structures, including the radio Loop I, IV, the North Polar Spur, andthe neighborhood of the newly discovered "Fermi bubbles". We argue that theX-ray absorber is unlikely associated with the nearby radio Loop I and IV;however, the non-thermal velocity can be naturally explained as the result ofthe expansion of the "Fermi bubbles". Our data implies an shock-expansionvelocity of 200 - 300 km/s. Our study indicates a likely complex environmentfor the production of the Galactic X-ray absorbers along different sightlines,and highlights the significance of probing galactic feedback with highresolution X-ray spectroscopy.

High Resolution X-ray Spectroscopy of the Local Hot Gas along the 3C 273 Sightline