Highly Ionized Envelopes of High Velocity Clouds

Details Highly Ionized Envelopes of High Velocity Clouds Highly Ionized Envelopes of High Velocity Clouds

2009-06-26

arxiv.org/abs/0906.5001v1

AIP Conf.Proc.1135:58-60,2009

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

3 pages, 1 figure, published in Future Directions in Ultraviolet Spectroscopy, Proceedings of the AIP Conference held October

Scientific paper

We present recent results on highly ionized gas in Galactic High-Velocity Clouds (HVCs), originally surveyed in OVI (Sembach et al. 2003). In a new FUSE/HST survey of SiII/III/IV (Shull et al. 2009) toward 37 AGN, we detected SiIII (lambda 1206.500 A) absorption with a sky coverage fraction 81 +/- 5% (61 HVCs along 30 of 37 high-latitude sight lines). The SiIII (lambda 1206.500 A) line is typically 4-5 times stronger than OVI (lambda 1031.926 A). The mean HVC column density of perhaps 10^19 cm^-2 of low-metallicity (0.1 - 0.2 Z_sun) ionized gas in the low halo. Recent determinations of HVC distances allow us to estimate a total reservoir of ~10^8 M_sun. Estimates of infall velocities indicate an infall rate of around 1 M_sun yr^-1, comparable to the replenishment rate for star formation in the disk. HVCs appear to be sheathed by intermediate-temperature gas (10^4.0 - 10^4.5 K) detectable in SiIII and SiIV, as well as hotter gas seen in OVI and other high ions. To prepare for HST observations of 10 HVC-selected sight lines with the Cosmic Origins Spectrograph (COS), we compile FUSE/STIS spectra of these ions, plus FeIII, CIII, CIV, and SIV. Better constraints on the physical properties of HVC envelopes and careful treatment of HVC kinematics and infall rates should come from high-quality (S/N ~ 30-40) COS data.

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