Abstract:
In this paper we study the Cepheids distribution in the Large Magellanic Cloud (LMC) as a function of
their ages using data from the OGLE III photometric catalogue. To determine age of the Pop I Cepheids,
we derived a period – age (PA) relationship using the Cepheids found in the LMC star clusters. We find
two peaks in the period distribution at log P = 0:49 ± 0:01 and log P = 0:28 ± 0:01 days which correspond
to fundamental and first overtone pulsation modes, respectively. Ages of the Cepheids are used to under-
stand star formation scenario in the LMC in last 30–600 Myr. The age distribution of the LMC Cepheids is
found to have a peak at log (Age)=8.2±0.1. This suggests that major star formation event took place at
about 125–200 Myr ago which may have been triggered by a close encounter between the SMC and
the LMC. Cepheids are found to be asymmetrically distributed throughout the LMC and many of them
lie in clumpy structures along the bar. The frequency distribution of Cepheids suggests that most of
the clumps are located to the eastern side of the LMC optical center.
