tokens: × 28.9 arcsec beam), which has the characteristics of a rotating disc with a moderate rotation velocity and a signature of a warp in the SE. The black contours at the centre of this panel are the two highest H i column density contours from the medium resolution total intensity H i map. These H i contours coincide with the kinematic centre as well as the optical centre of the galaxy. The velocity field of UGC 2162 shows no significant sign of recent major interaction. The position velocity (PV) diagram for a slice taken along the H i major axis, position angle (PA) = 307 ° , is shown in the middle panel of Fig. 6 and confirms a rotating disc. A small mass of low density extra-planar H i is seen ∼15–20 arcsec (∼1 kpc) SE of the kinematic centre in the PV diagram. The lower panel of Fig. 6 shows the rotation curve extracted from bbarolo (Di Teodoro Fraternali 2015 ) fit to the medium-resolution cube. The figure shows a slowly rising rotation curve that is a common feature for dwarf galaxies. The bbarolo best fit gives an inclination of 55.5 ° , with V rot at the outermost fitted ring, r = 67.5 arcsec (4.05 kpc) ∼ 25 km s −1 . The M dyn enclosed within each ring fitted with bbarolo is used in Section 4.1 to estimate the galaxy’s virial mass ( M vir ). We also estimated the V rot using the H i W 20 (adjusted for the inclination from the bbarolo model fit) where V rot = 0.5 Δ V [km s −1 ]/sin(i) with Δ V = W 20 (50 km s −1 ) from the GBT spectrum and i = 55.5 ° /180. This second method gives V rot ∼ 30.8 km s −1 at the outer edge of the detected H i disc. These values are also used in the Section 4.1 analysis. Figure 6. UGC 2162 H i kinematics: Top: GMRT velocity field from the medium-resolution cube. The two highest column density contours from the medium-resolution H i integrated map are shown in black. The PV diagram (panel below) slice PA = 307 ° is shown with a grey line. Middle: PV diagram from a PA = 307 ° slice. Positive positional offsets are to the NW. The blue contours are from the data and the red are from the bbarolo best-fitting model. Bottom: Rotation curve derived from the bbarolo five ring model fit. In Fig. 7 , we compare the V rot from for UGC 2162 with the V rot derived from model fits to the VLA H i for the LITTLE THINGS dwarf galaxies by Oh et al. ( 2015 ). The plot shows that the UGC 2162 V rot = 30.8 km s −1 , derived from the GBT W 20 , falls within the range of V rot for LITTLE THINGS with similar M H i and below the LITTLE THINGS median V rot of 39.5 km s −1 . Fig. 8 shows the baryonic and stellar Tully-Fisher relations. Figure 7. V rot versus M gas : UGC 2162 (Black square) and LITTLE THINGS dwarf galaxies (red crosses) from Oh et al. ( 2015 ). The UGC 2162, V rot = 30.8 km s −1 is derived from the GBT W 20 in Section 3.2 . For both UGC 2162 and the LITTLE THINGs galaxies, M gas = 1.4 × M H i with the additional factor to account for molecular gas and He. Figure 8. UGC 2162 Tully–Fisher relations: The position of UGC
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