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In preparation for a Hubble Space Telescope (HST) observing project using theCosmic Origins Spectrograph (COS), the positions of all AGN targets havinghigh-S/N far-UV G130M spectra were cross-correlated with a large catalog oflow-redshift galaxy groups homogeneously selected from the spectroscopic sampleof the Sloan Digital Sky Survey (SDSS). Searching for targets behind only thosegroups at z = 0.1-0.2 (which places the OVI doublet in the wavelength region ofpeak COS sensitivity) we identified only one potential S/N = 15-20 target, FBQS1010+3003. An OVI-only absorber was found in its G130M spectrum at z = 0.11326,close to the redshift of a foreground small group of luminous galaxies at z =0.11685. Because there is no associated Lyalpha absorption, anycharacterization of this absorber is necessarily minimal; however, the OVIdetection likely traces "warm" gas in collisional ionization equilibrium at T ~300,000 K. While this discovery is consistent with being interface gas betweencooler, photoionized clouds and a hotter intra-group medium, it could also bewarm, interface gas associated with the circum-galactic medium (CGM) of thesingle closest galaxy. In this case a detailed analysis of the galaxydistribution (complete to 0.2 L*) strongly favors the individual galaxyassociation. This analysis highlights the necessity of both high-S/N > 20 COSdata and a deep galaxy redshift survey of the region in order to test morerigorously the association of OVI-absorbing gas with a galaxy group. A Cycle 23HST/COS program currently is targeting 10 UV-bright AGN behind 12 low-redshiftgalaxy groups to test the warm, group gas hypothesis.

The Warm Circum-Galactic Medium: 10^5-6 K Gas Associated with a Single Galaxy Halo or with an Entire Group of Galaxies?