  We present new HI observations of the nearby dwarf galaxy NGC 3741. This
galaxy has an extremely extended HI disk, which allows us to trace the rotation
curve out to unprecedented distances in terms of the optical disk: we reach 42
B-band exponential scale lengths or about 7 kpc. The HI disk is strongly
warped, but the warp is very symmetric. The distribution and kinematics are
accurately derived by building model data cubes, which closely reproduce the
observations. In order to account for the observed features in the data cube,
radial motions of the order of 5-13 km/s are needed. They are consistent with
an inner bar of several hundreds of pc and accretion of material in the outer
regions.
  The observed rotation curve was decomposed into its stellar, gaseous and dark
components. The Burkert dark halo (with a central constant density core)
provides very good fits. The dark halo density distribution predicted by the
LambdaCDM theory fails to fit the data, unless NGC 3741 is a 2.5-sigma
exception to the predicted relation between concentration parameter and virial
mass and has at the same time a high value of the virial mass (though poorly
constrained) of 10$^{11}$ solar masses. Noticeably, MOND seems to be consistent
with the observed rotation curve. Scaling up the contribution of the gaseous
disk also gives a good fit.
