We present deep , high velocity resolution ( \sim 1.6 km sec ^ { -1 } ) Giant Meterwave Radio Telescope ( GMRT ) HI 21cm synthesis images of the faint ( M _ { B } \sim - 10.6 ) local group dwarf galaxy DDO210 .
We find that the HI distribution in the galaxy is not axi-symmetric , but shows density enhancements in the eastern and southern halves of the galaxy .
The optical emission is lopsided with respect to the HI , most of the bright optical emission arises from the eastern half of the HI disk .
The velocity field of the galaxy is however quite regular and shows a systematic large scale pattern , consistent with the rotational motion .
The rotation curve for the galaxy shows a peak ( inclination corrected ) rotation velocity of only \sim 8 km sec ^ { -1 } , comparable to the random motions in the HI gas .
After correcting for the dynamical support provided by random motions ( the “ asymmetric drift ” correction ) , we find the corrected peak rotation velocity of \sim 16.0 km sec ^ { -1 } .
Mass modeling of the corrected rotation curve shows that the kinematics of DDO210 can be well fit with either a modified isothermal halo ( with a central density \rho _ { 0 } \sim 29 \times 10 ^ { -3 } M _ { \odot } pc ^ { -3 } 
for a stellar mass to light ratio of 3.4 ) or an NFW halo .
In the case of the NFW halo however , a good fit is obtained for a wide range of parameters ; the halo parameters could not be uniquely determined from the fit .
Density profiles with inner slope steeper than \sim 1.2 however provide a poor fit to the data .
Finally , the rotation curve derived using MOND also provides a reasonable fit to the observed rotation curve .