Kinematics of the central regions of NGC 1672

We present the detailed velocity field of the central 2 kpc of the LINER galaxy NGC 1672. The isovelocity map shows a rotational pattern with a velocity gradient of 50 km s(-1) arcsec(-1) in the inner 6 " (1 " approximate to 70 pc), indicating a mass of approximate to 9 x 10(8) M-. inside a radius of 125 pc, equivalent to a density of approximate to 2 x 10(11) M-. kpc(-3). It also shows some asymmetries on a larger scale. An offset of approximate to 60 pc between the nuclear continuum barycenter and the kinematical center is also found. Satoh's model fitting to the observed velocity field reveals several nonaxisymmetric residuals, which do not correlate well with the bar or the circumnuclear ring of H II regions. The inner rotation curve of NGC 1672 reveals that the circumnuclear ring of star formation is located on an inner Lindblad resonance (ILR), and not near the peak of the Lindblad curve, Omega - (kappa/2), as suggested by previous works, which also claimed that the ring rotates faster than its ambient. This motion is not confirmed by the two-dimensional residual-velocity map.