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Aperture synthesis observations of two HI cloud complexes located in theperiphery of the Virgo galaxy cluster are presented. These low HI-mass clouds($M_{HI}<$ 10$^{9}$) are seen projected on the M region of the western Virgocluster, where the galaxy population is thought to lie behind the main Acluster surrounding M87. The kinematic measurements of both unresolved Areciboand resolved VLA-C observations are in good agreement. The HI detections cannotbe identified with any optical, IR, or UV emission from available archivalimaging. They are inert at these wavelengths. The HI masses of the individualVLA detections range from 7.28 $\leq$ log($M_{HI}) \leq $ 7.85. The totaldynamical mass estimates are several times their HI content, ranging from 7.00$\leq$ log($M_{dyn}) \leq $ 9.07, with the assumption that the clouds areself-gravitating and in dynamical equilibrium. We report the observedparameters derived from the VLA observations. One of these HI clouds appears tobe the most isolated optically inert detection observed in the outer reaches ofVirgo.

Clouds Toward the Virgo Cluster Periphery: Gas-rich Optically Inert Galaxies