Filamentary gas spanning the region between the galaxy clusters Abell 3391 and Abell 3395 has been detected using ASCA and ROSAT archived data. The gas has a minimum flux of 1.3x 10~(12)erg cm~(-2)s~(-1) (0.8- 10keV). Within this filament resides a galaxy group for which a flux of (2.0+-0.3) x 10~(13)ergcm~(-2)s~(-1) (0.8 - 10 keV) is determined. An analysis using raytracing determines light scattered into the filamentary region contributes 13% of the count-rate. The structure in which the filamentary gas resides is postulated to be a filament aligned nearly lengthwise with the line of sight. Identification of this structure as a filament is based on the angular and redshift distribution of surrounding galaxies and clusters. The distribution is compatible with the structure being a quasi-linear structure tilted to the line-of-sight such that the ratio of the depth to the tangential distance is between 6:1 and 18:1. The filamentary gas contains on the order of 10~(13)solar madd of gas which is close to 2% of the total mass of the system.
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