An estimation of the Gaia EDR3 parallax bias from stellar clusters and Magellanic Clouds data

Centro de Astrobiología, CSIC-INTA. Campus ESAC. C. bajo del castillo s/n. 28 692 Villanueva de la Cañada, Madrid, Spain
e-mail: jmaiz@cab.inta-csic.es

Received: 4 October 2021
Accepted: 4 November 2021

Abstract

Context. The early-third Gaia data release (EDR3) parallaxes constitute the most detailed and accurate dataset that currently can be used to determine stellar distances in the solar neighborhood. Nevertheless, there is still room for improvement in their calibration and systematic effects can be further reduced in some circumstances.

Aims. The aim of this paper is to determine an improved Gaia EDR3 parallax bias as a function of magnitude, color, and ecliptic latitude using a single method applied to stars in open clusters, globular clusters, the Large Magellanic Cloud, and the Small Magellanic Cloud.

Methods. I study the behavior of the residuals or differences between the individual (stellar) parallaxes and the group parallaxes, which are assumed to be constant for the corresponding cluster or galaxy. This was done by first applying the Lindegren et al. (2021b, A&A, 649, A4) zero point and then calculating a new zero point from the residuals of the first analysis.

Results. The Lindegren zero point shows very small residuals as a function of magnitude between individual and group parallaxes for G > 13 but significant ones for brighter stars, especially blue ones. The new zero point reduces those residuals, especially in the 9.2 < G < 13 range. The k factor that is used to convert from catalog parallax uncertainties to external uncertainties is small (1.1–1.7) for 9.2 < G < 11 and G > 13, intermediate (1.7–2.0) for 11 < G < 13, and large (>2.0) for G < 9.2. Therefore, significant corrections are needed to calculate distance uncertainties from Gaia EDR3 parallaxes for some stars. There is still room for improvement if future analyses add information from additional stellar clusters, especially for red stars with G < 11 and blue stars with G < 9.2. I also calculated k for stars with RUWE values between 1.4 and 8.0 and for stars with six-parameter solutions, allowing for a correct estiimation of their uncertainties.