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In the star formation process, the vital impact of environmental factors suchas feedback from massive stars and stellar density on the form of the initialmass function (IMF) at low-mass end is yet to be understood. Hence asystematic, highly sensitive observational analysis of a sample of regionsunder diverse environmental conditions is essential. We analyse the IMF ofeight young clusters ($<$5 Myr), namely IC1848-West, IC1848-East, NGC 1893, NGC2244, NGC 2362, NGC 6611, Stock 8 and Cygnus OB2, which are located at theGalactocentric distance ($R_g$) range $\sim$6-12 kpc along with nearby clusterIC348 using deep near-IR photometry and Gaia DR2. These clusters are embeddedin massive stellar environments of radiation strength $log(L_{FUV}/L_{\odot})$$\sim$2.6 to 6.8, $log(L_{EUV})$ $\sim$42.2 to 50.85 photons/s, with stellardensity in the range of $\sim$170 - 1220 stars/pc$^2$. After structuralanalysis and field decontamination we obtain an unbiased, uniformly sensitivesample of pre-main-sequence members of the clusters down to brown-dwarf regime.The lognormal fit to the IMF of nine clusters gives the mean characteristicmass ($m_c$) and $\sigma$ of 0.32$\pm$0.02 $M_\odot$ and 0.47$\pm$0.02,respectively. We compare the IMF with that of low- and high-mass clustersacross the Milky Way. We also check for any systematic variation with respectto the radiation field strength, stellar density as well with $R_g$. Weconclude that there is no strong evidence for environmental effect in theunderlying form of the IMF of these clusters.

Testing the role of environmental effects on the initial mass function of low-mass stars