2026-10-15T02:17:27Z https://www.scidb.cn/oai

10.57760/sciencedb.0104k 2026-09-04T17:33:52Z

2026-09-04 Radial Velocities of the Solar Neighborhood Open Cluster based on Gaia DR3 doi:10.57760/sciencedb.0104k en This dataset is derived from the paper "Revisiting the Radial velocities of Nearby Open Clusters Using Gaia DR3" and includes a Table1.fits file that records a total of 171 open clusters in the vicinity of the Sun. The study examined samples through color magnitude maps and PARSEC age lines, retaining only the intrinsic color \ (0.2 \ leq (G_ {\ rm BP} - GY {\ rm RP}) 0 \ leq1.2 \) mag and at least 20 member stars with radial velocities. The average radial velocity and velocity dispersion of the star cluster are obtained through iterative outlier removal and Gaussian fitting of the member stars; The tangential velocity dispersion is calculated from Gaia data corrected for system motion and perspective effects. The radial velocity of the member stars is determined by the RVS spectrometer of Gaia satellite, with a wavelength range of 846-870 nm and a spectral resolution of approximately 11500. Gaia DR3 covers a total of 34 months of observations from July 25, 2014 to May 28, 2017, with a reference epoch of 2016.0. The sample mainly covers the silver latitude (| b |<30 ^ \ circle \) and the area about 500 pc away from the sun; Each row in the table represents an open star cluster, with Name being the OCSN number; RAdeg and DEdeg are right ascension and declination (degrees); Plx and e_plx are the disparity and its error (mas); Logt is the logarithm of age; E (B-V) and (m-M) 0 are respectively the chromatic aberration and distance modulus (mag); Sigma-R.A. and sigma-Decl. represent the tangential velocity dispersion in two directions; Mu_SV_c and sigma-RV_c are the average radial velocity and radial velocity dispersion (km s ⁻¹); N_RV is the number of member stars involved in the fitting. All 171 records have no null, NaN, or infinite values. The apparent velocity dispersion may still be affected by Gaia measurement errors and unidentified binary orbital movements, and should be considered as the upper limit reference for the true intrinsic velocity dispersion of star clusters. FITS files can be read using TOPCAT or Python Astropy.  Gaia; open cluster; radial velocity Tang Tong PUBLIC https://creativecommons.org/licenses/by-nc-sa/4.0/ dataset http://www.doi.org/10.1088/1538-3873/ae8479 Science Data Bank