| Abstract : | We present the results from an analysis of three open clusters ECX6-27 IR Cluster– (RA: 20:33:56, Dec: 41:22:54), Majaess 30 (RA: 02:44:36, Dec: 60:59:43), and Teutsch 55 (RA: 02:29:08, Dec: 62:06:19) – situated in the galactic plane using archival data from GAIA DR3 and 2MASS surveys. We used proper motion data from GAIA DR3 to identify likely cluster members separated from the field using a gaussian likelihood model. The cluster radii were estimated as 4´ for ECX6-27 IR Cluster, 3´ for Majaess 30, and 3.5´ for Teutsch 55 by fitting King’s density profile to the radial density profile of the clusters. We followed standard practices of photometric analysis by plotting colour-colour diagram (CCD) and colour-magnitude diagrams (CMDs) of the member stars. The line-of-sight interstellar reddening E(J-H), distances to the clusters, and their ages were obtained from the fit of theoretical isochrones of solar metallicity to the CCD and CMDs. ECX6-27 IR Cluster has E(J-H) = 0.95 ± 0.03 mag, Majaess 30 has E(J-H) = 0.35 ± 0.03, and Teutsch 55 has E(J-H) = 0.2 ± 0.05 mag. The distances and log(age)s of the clusters are respectively: ECX6-27 IR Cluster - 1.995 ± 0.2 kpc and 7.0 ± 0.2; Majaess 30 - 3.162 ± 0.25 kpc and 7.5 ± 0.3; and Teutsch 55 – 3.467 ± 0.4 kpc and 7.3 ± 0.2. Using Kroupa’s form of mass function, we obtain the mass function slopes as -2.68 ± 0.3, -2.42 ± 0.15, and -2.96 ± 0.19 for ECX6-27 IR Cluster, Majaess 30, and Teutsch 55 respectively. The three clusters in the present study are located in the vicinity of larger star forming regions and may be probed to understand the nature of star formation around molecular clouds. |
