Kinematic parameters and membership probabilities of open clusters in the Bordeaux PM2000 catalogue

Abstract

Aims. We derive lists of proper-motions and kinematic membership probabilities for 49 open clusters and possible open clusters in the zone of the Bordeaux PM2000 proper motion catalogue (+11 • ≤ δ ≤ +18 • ). We test different parametrisations of the proper motion and position distribution functions and select the most successful one. In the light of those results, we analyse some objects individually. Methods. We differenciate between cluster and field member stars, and assign membership probabilities, by applying a new and fully automated method based on both parametrisations of the proper motion and position distribution functions, and genetic algorithm optimization heuristics associated with a derivative-based hill climbing algorithm for the likelihood optimization.Results. We present a catalogue comprising kinematic parameters and associated membership probability lists for 49 open clusters and possible open clusters in the Bordeaux PM2000 catalogue region. We note that this is the first determination of proper motions for five open clusters. We confirm the non-existence of two kinematic populations in the region of 15 previously suspected non-existent objects.

CCD astrometric observations of Phoebe in 2005-2008

“…Consequently, as the density of UCAC2 was sufficient for the astrometric reduction, we preferred it to UCAC3. In addition, our determination of zonal errors in the zone of Phoebe confirms the similar results obtained by Krone‐Martins et al (2010).…”

“…We preferred it to UCAC3 although providing a higher density (Zacharias et al 2010), because we have shown that UCAC3 can result in some significant zonal errors in the zone of our observations of Phoebe in [2005][2006][2007][2008]. Such errors in star catalogues have been pointed out and estimated by several authors, for example by Fienga & Andrei (2002) and more recently by Roeser, Demleitner & Schilbach (2010) and Krone-Martins et al (2010). In this latest work, Krone-Martins and co-workers showed that UCAC3 could produce higher systematic zonal errors than UCAC2 in a large zone that overlaps with the zone where Phoebe was located in 2005-2008.…”

ASteCA: Automated Stellar Cluster Analysis

“…Techniques making use of PMs go back to the Vasilevskis-Sanders (V-S) method (Vasilevskis et al 1958;Sanders 1971), which modeled cluster and field stars as a bi-variate Gaussian distributions in the vector point diagram (VPD) solving iteratively the resulting likelihood equation. The original method has been largely improved since and is present in numerous works (Stetson 1980;Zhao & He 1990;Kozhurina-Platais et al 1995;Wu et al 2002;Balaguer-Nunez et al 2004;Javakhishvili et al 2006;Frinchaboy & Majewski 2008;Krone-Martins et al 2010;Sarro et al 2014).…”

Variability in the Massive Open Cluster NGC 1817 from K2: A Rich Population of Asteroseismic Red Clump, Eclipsing Binary, and Main-sequence Pulsating Stars

“…In producing the SEDs, we col-lected photometry from the following sources: ultraviolet photometry from the Galaxy Evolution Explorer (GALEX; Martin et al 2005), Strömgren photometry from , BV I C data from Donati et al (2014), PSF magnitudes from Data Release 14 of the Sloan Digital Sky Survey (SDSS; York et al 2000), mean PSF magnitudes from the Pan-STARRS1 survey (Kaiser et al 2010), the APASS survey (Henden et al 2015), Data Release 2 (DR2) of the Gaia archive (Gaia Collaboration et al 2018a), Two-Micron All-Sky Survey (2MASS; Skrutskie et al 2006) photometry from the All-Sky Point Source Catalog, and from the Wide Field Infrared Explorer (WISE; Wright et al 2010) survey. presented proper motion membership determinations for stars with V < 15, and Krone-Martins et al (2010) also studied the cluster's proper motion membership as part of a larger survey of clusters. However, DR2 from the Gaia spacecraft currently provides the most precise proper motions and parallaxes to gauge cluster membership.…”