Complex Stellar System ESO65SC03: Open Cluster or Remnant?

Abstract

We present a complete spatial and dynamical study of the poorly populated stellar system ESO65SC03. The radial distribution of the system gives a core and cluster radii of 1.10 ± 0.63 and 5.36 ± 0.24 arcmin, respectively. The SNDP does not show any clear enhancement of the surface stellar number density between the stars of the system and the field regions. We derive the optimum isochrone solution for a particular grid size in the CMD using the statistical cleaning procedure. Using the statistically cleaned CMDs, we find the distance modulus, (m − M) 0 , and reddening, E(B − V ), of the system to be 11.8 ± 0.2 and 0.45 mag, respectively. The mean proper motion of this system is −5.37 ± 0.81 mas yr −1 and 0.31 ± 0.40 in RA and DEC directions, respectively. The mean proper motion of this system is found to be almost similar to the field region. The mass function for the brighter stars is found to be too high for the system to be an open cluster. These combined results place constraints on whether stellar system ESO65SC03 is a POCR or an Asterism. Our understanding is that the ESO65SC03 is in a stage of POCR by losing their main-sequence stars in the dynamic evolution processes.

Effect of Blue Component Stars in Parameters of NGC 6866

“…The cluster center is taken in such way that we have obtained best RDP through it and follow the condition of maximum count within the cluster region. The detail procedure of above said approach is prescribed by the Joshi et al (2015). In the present case, the cluster center (α, δ) is found to be (20 h : 03 m : 54.9 s , + 44 o : 09 ′ : 28.2 ′′ ) in RA − DEC plane.…”

“…We are assumed that the field stars of RCS are uniformly distributed over all the cluster region. To identify the possible giant stars of the cluster, we have been applied the statistical distance algorithm on the RCS [detailed procedure has been prescribed by Joshi et al (2015)]. The core (0 < r≤8.39 arcmin) is considered to be giant stars region and the region, having radial distance range (10 < r≤13.05 arcmin) and equivalent area to giant star region, considered as the filed region.…”

“…The above said decontamination would be carried out through either the photometric statistical criteria (Sharma et al, 2008) or the statistical cleaning in CMDs (Joshi et al, 2014). Recently, Joshi et al (2015) have been introduced the statistical cleaning procedure of field star decontamination through the colour-magnitude distance for field star decontamination, which is dependent on the grid size around the field star. The size of grid would be fixed on the basis of comparison of cluster and field stars in the term of their magnitude and colour (Joshi et al, 2015).…”

“…Recently, Joshi et al (2015) have been introduced the statistical cleaning procedure of field star decontamination through the colour-magnitude distance for field star decontamination, which is dependent on the grid size around the field star. The size of grid would be fixed on the basis of comparison of cluster and field stars in the term of their magnitude and colour (Joshi et al, 2015). After field stars decontamination from the observed CMDs, it becomes very effective tool to derive the precise values of fundamental parameters with the comprehensive results of the Luminosity-function (LF) and the Mass-Function (MF).…”

IC 361:- Near infrared and UBVRI photometric Analysis

“…The cluster radius is found to be 8 arcmin in present analysis leads the value of cluster's diameter is 16±1 arcmin. Since, estimated diameter is greater than the size of observed optical frame as well as other available optical catalogues, therefore, we can not utilized these catalogues for statistical colour-magnitude cleaning (Joshi et al, 2015) due to observations of limited region of cluster. The available 2MASS data of field region of IC 361 is fulfilled criteria of our need.…”