Other
Scientific paper
Jul 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003hst..prop.9778s&link_type=abstract
HST Proposal ID #9778
Other
Hst Proposal Id #9778 Ism And Circumstellar Matter
Scientific paper
We propose to use two extragalactic sightlines to probe our own Galaxy's "starburst" wind emanating from the Galactic Center. While new infrared imaging and spectroscopy have detected massive stars and very recent {<3x10^6 yrs} star formation in the Galactic Center region, only indirect evidence {e.g., radio loops and arcs, bi-conical cavity edges seen in the mid-IR} exists for a wind. However, these winds are routinely detected from starbursts in other galaxies. Far-UV STIS echelle spectroscopy {E140M} of two targets on either side of the Galactic Center at {l, b}={350,-33} and {349, 55} will allow us to map the kinematics of outflowing gas in high ionization species of N V, Si IV and C IV. Similar spectra of distant {1.5-5 kpc}, bright B stars in the same regions of the sky will allow us to remove foreground contaminating components due to the Sco-Cen OB associations. Lower resolution STIS first-order and FUSE spectra show highly redshifted gas in N V and O VI respectively along these sightlines; these new observations will provide three times better spectral resolution {7-10 km/s in the 1185-1580A region} so that the kinematic signature of the outflow can definitely be detected. The foreground stars will allow us to determine whether the outflow is from the Galactic Center or the Sco-Cen OB associations. Absorption line column densities will be used to estimate the outflowing mass and energy by assuming a metallicity and ionizing source for the gas.
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