Star Formation Rate Distribution in the Galaxy NGC 1232
  NGC 1232 is a face-on spiral galaxy and a great laboratory for the study of
star-formation due to its proximity. We obtained high spatial resolution
H{\alpha} images of this galaxy, with adaptive optics, using the SAM instrument
at the SOAR telescope, and used these images to study its H ii regions. These
observations allowed us to produce the most complete H ii region catalog for it
to date, with a total of 976 sources. This doubles the number of H ii regions
previously found for this object. We used these data to construct the H ii
luminosity function, and obtained a power-law index lower than the typical
values found for Sc galaxies. This shallower slope is related to the presence
of a significant number of high-luminosity H ii regions (logL>39 dex). We also
constructed the size distribution function, verifying that, as for most
galaxies, NGC 1232 follows an exponential law. We also used the H{\alpha}
luminosity to calculate the star formation rate. An extremely interesting fact
about this galaxy is that X-ray diffuse observations suggest that NGC 1232
recently suffered a collision with a dwarf galaxy. We found an absence of star
formation around the region where the X-ray emission is more intense, which we
interpret as a star formation quenching due to the collision. Along with that,
we found an excess of star-forming regions in the northeast part of the galaxy,
where the X-ray emission is less intense.
