Here we present H i line and 20-cm radio continuum data of the nearby galaxy pair NGC 1512/1510 as obtained with the Australia Telescope Compact Array ( ATCA ) .
These are complemented by GALEX UV - , SINGG H \alpha - and Spitzer mid-infrared images , allowing us to compare the distribution and kinematics of the neutral atomic gas with the locations and ages of the stellar clusters within the system .

For the barred , double-ring galaxy NGC 1512 we find a very large H i disk , \sim 4 \times its optical diameter , with two pronounced spiral/tidal arms .
Both its gas distribution and the distribution of the star-forming regions are affected by gravitational interaction with the neighbouring blue compact dwarf galaxy NGC 1510 .
While the inner disk of NGC 1512 shows quite regular rotation , deviations are visible along the outer arms and at the position of NGC 1510 .
From the H i rotation curve of NGC 1512 we estimate a dynamical mass of M _ { dyn } \ga 3 \times 10 ^ { 11 } M _ { \odot } , compared to an H i mass of M _ { HI } = 5.7 \times 10 ^ { 9 } M _ { \odot } ( \sim 2 % M _ { dyn } ) .

The two most distant H i clumps , at radii of \sim 80 kpc , show signs of star formation and are likely tidal dwarf galaxies ( TDGs ) .
Both lie along an extrapolation of the eastern-most H i arm , with the most compact H i cloud located at the tip of the arm .

The 20-cm radio continuum map indicates extended star formation activity not only in the central regions of both galaxies but also in between them .
Star formation ( SF ) in the outer disk of NGC 1512 is revealed by deep optical- and two-color ultraviolet images .
Using the latter we determine the properties of \ga 200 stellar clusters and explore their correlation with dense H i clumps in the even larger 2XH i disk .
Outside the inner star-forming ring of NGC 1512 , which must contain a large reservoir of molecular gas , H i turns out to be an excellent tracer of SF activity .

The multi-wavelength analysis of the NGC 1512/1510 system , which is probably in the first stages of a minor merger having started \sim 400 Myr ago , links stellar and gaseous galaxy properties on scales from one to 100 kpc .