ATCA H i and radio continuum observations of the peculiar southern galaxy IC 2554 and its surroundings reveal typical signatures of an interacting galaxy group .
We detected a large H i cloud between IC 2554 and the elliptical galaxy NGC 3136B .
The gas dynamics in IC 2554 itself , which is sometimes described as a colliding pair , are surprisingly regular , whereas NGC 3136B was not detected .
The H i cloud , which emerges from IC 2554 as a large arc-shaped plume , has a size of \sim 30 kpc , larger than that of IC 2554 .
The total H i mass of the IC 2554 system is \sim 2 \times 10 ^ { 9 } M _ { \odot } , a third of which resides in the H i cloud .
It is possible that tidal interaction between IC 2554 and NGC 3136B caused this spectacular H i cloud , but the possibility of IC 2554 being a merger remnant is also discussed .
We also detected H i gas in the nearby galaxies ESO 092-G009 and RKK 1959 as well as an associated H i cloud , ATCA J1006–6710 .
Together they have an H i mass of \sim 4.6 \times 10 ^ { 8 } M _ { \odot } .
Another new H i source , ATCA J1007–6659 , with an H i mass of only \sim 2.2 \times 10 ^ { 7 } M _ { \odot } was detected roughly between IC 2554 and ESO 092-G009 and corresponds to a face-on low surface brightness dwarf galaxy .
Star formation is evident only in the galaxy IC 2554 with a rate of \sim 4 M _ { \odot } yr ^ { -1 } .