Recent star formation history of the Large and Small Magellanic Clouds
  We traced the age of the last star formation event (LSFE) in the inner Large & Small Magellanic Cloud (L&SMC) using the photometric data from the Optical Gravitational Lensing Experiment (OGLE-III) and the Magellanic Cloud Photometric Survey (MCPS). The LSFE is estimated from the main-sequence turn off point in the color-magnitude diagram (CMD) of a region. Extinction corrected turn off magnitude is converted to age, which represents the LSFE in a region. The spatial map of the LSFE age shows that the star formation has shrunk to the central regions in the last 100Myr in both the galaxies. The location and age of LSFE is found to correlate well with those of the star cluster in both the Clouds. The SMC map shows two separate concentrations of young star formation. We detect peaks of star formation at 0-10, 90-100Myr in the LMC, and 0-10, 50- 60Myr in the SMC. The quenching of star formation in the LMC is found to be asymmetric with respect to the optical center such that most of the young star forming regions are located to the north and east. On deprojecting the data on the LMC plane, the recent star formation appears to be stretched in the north-east direction and the HI gas is found to be distributed preferentially in the North. The centroid is found to shift to north in 200-40Myr, and to north-east in the last 40Myr. In the SMC, we detect a shift in centroid of population of 500-40Myr in the direction of the LMC. We propose that the HI gas in the LMC is pulled to the north of the LMC in the last 200Myr due to the gravitational attraction of our Galaxy at the time of perigalactic passage. The shifted HI gas is preferentially compressed in the north during 200-40Myr and in the north-east in the last 40Myr, due to the motion of the LMC in the Galactic halo. The recent star formation in the SMC is due to the combined gravitational effect of the LMC and the perigalactic passage. 
G Indu and Annapurni Subramaniam
astro-ph.CO