We have obtained 21 cm images of 19 spiral galaxies in the Coma cluster , using the VLA in its C and D configurations .
The sample selection was based on morphology , brightness , and optical diameters of galaxies within one Abell radius ( 1.2 ^ { \circ } ) .
The H i detected , yet deficient galaxies show a strong correlation in their H i properties with projected distance from the cluster center .
The most strongly H i deficient ( Def _ { \mathrm { HI } } > 0.4 ) galaxies are located inside a radius of 30 ^ { \prime } ( { \sim } 0.6 Mpc ) from the center of Coma , roughly the extent of the central X-ray emission .
These central galaxies show clear asymmetries in their H i distribution and/or shifts between the optical and 21 cm positions .
Another 12 spirals were not detected in H i with typical H i mass upper limits of 10 ^ { 8 } M _ { \odot } .
Seven out of the twelve non detections are located in the central region of Coma , roughly within 30 ^ { \prime } from the center .
The other non detections are to the east and southwest of the center .

Seven so called blue disk galaxies in Coma were observed in H i and six were detected .
These galaxies are relatively close to the central region of Coma .
The non detected one is the closest to the center .
The six detected blue galaxies are mildly H i deficient .
We did a more sensitive search for H i from 11 of the 15 known post starburst galaxies in Coma .
None were detected with typical H i mass limits between 3 and 7 \times 10 ^ { 7 } M _ { \odot } .

Our results present and enhance a picture already familiar for well studied clusters .
H i poor galaxies ( deficient ones and non-detections ) are concentrated toward the center of the cluster .
The H i morphology of the central galaxies , with optical disks extending beyond the H i disks is unique to cluster environments and strongly suggests an interaction with the IGM .
A new result in Coma is the clumpy distribution of gas deficiency .
In the cluster center the deficient galaxies are to the east while the non-detections are to the west .
In the outer parts the gas rich galaxies are north of Coma , non-detected spirals are found in the NGC 4944 group to the east and NGC 4839 group to the south west .
This supports recent findings that merging of groups is ongoing in the center of Coma , further out the NGC 4944 and NGC 4839 must have passed at least once through the core , while the galaxies to the north have yet to fall in .