2022A&A...657A.130M


Query : 2022A&A...657A.130M

2022A&A...657A.130M - Astronomy and Astrophysics, volume 657A, 130-130 (2022/1-1)

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

MAIZ APELLANIZ J.

Abstract (from CDS):


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.

Abstract Copyright: © ESO 2022

Journal keyword(s): astrometry - globular clusters: general - open clusters and associations: general - methods: data analysis - parallaxes - stars: distances

Simbad objects: 21

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Number of rows : 21
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NGC 104 GlC 00 24 05.359 -72 04 53.20   5.78 4.09     ~ 3749 0
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10381 1
3 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6418 1
4 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16265 1
5 HD 36939 V* 05 34 55.2955987536 -05 30 22.104460800   9.00 9.01     B7/8II 79 0
6 HD 36982 Or* 05 35 09.8363878512 -05 27 53.216296776 8.00 8.58 8.46     B1.5Vp 197 0
7 * tet01 Ori D Y*O 05 35 17.2574479992 -05 23 16.570738104 6.08 6.79 6.70 6.40 6.20 B1.5Vp 317 0
8 NGC 2244 83 Em* 06 31 20.5823668840 +04 50 13.424351837   11.20 10.94     ~ 9 0
9 V* V684 Mon EB* 06 40 38.3663658576 +09 47 16.046270268 7.71 8.31 8.44 8.492 8.516 B4 75 0
10 Cl Trumpler 14 5 * 10 43 53.6203837896 -59 33 28.513930068 11.046 11.631 11.302 11.20 10.65 O9V 24 0
11 V* V731 Car EB* 10 45 12.7214663496 -59 44 46.149112428 8.739 9.472 9.229 9.65 8.699 O8V(n)+O9.5V 86 0
12 NGC 5139 GlC 13 26 47.28 -47 28 46.1   6.12 5.33     ~ 3265 0
13 M 5 GlC 15 18 33.22 +02 04 51.7   7.34 5.95     ~ 1888 0
14 M 13 GlC 16 41 41.634 +36 27 40.75     5.8     ~ 2115 0
15 V* V964 Sco bC* 16 54 18.3200772432 -41 51 35.651104416 9.126 9.776 9.603 9.61 9.290 B0.5V 57 0
16 HD 326331 ** 16 54 25.9691286216 -41 49 55.768191852 6.886 7.678 7.497   7.143 O8IVn((f)) 73 0
17 HD 152314 Y*? 16 54 32.0048577720 -41 48 18.848961036 7.256 7.974 7.749 9.01 7.446 O9IV 106 0
18 NGC 6397 GlC 17 40 42.09 -53 40 27.6     5.17     ~ 1893 1
19 2MASS J18184096-1345296 Y*O 18 18 40.9652335752 -13 45 29.644481772 12.01 11.85 11.05     B0.5V 29 0
20 NGC 6752 GlC 19 10 52.11 -59 59 04.4   6.96 6.28     ~ 1911 0
21 NGC 7000 Cl* 20 58 47 +44 19.8           ~ 387 0

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2022.10.01-13:15:09

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