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Table A.1.

Proper motion anomalies of Galactic Cepheids.

Name Period ϖ μHG (mas a−1) μHip − μHG (mas a−1) ΔHip μG2 − μHG (mas a−1) ΔG2 PM Bin.



(d) (mas) μα μδ μα μδ μα μδ bin. type
T Ant 5.90 0.32 −6.87 0.03 +6.06 0.04 −0.77 1.02 −0.01 1.05 0.8 −0.07 0.08 −0.07 0.09 1.1
U Aql 7.02 3.63* +1.00 0.03 −8.97 0.03 −1.99 0.92 −0.17 0.74 2.2 +1.01 0.20 −3.97 0.17 23.3 †  ‡ O
SZ Aql 17.14 0.45 +0.32 0.05 −2.67 0.04 −0.10 1.13 +0.31 0.89 0.4 +0.01 0.11 +0.04 0.11 0.4
TT Aql 13.76 0.92 −0.43 0.05 −4.68 0.03 +1.60 1.50 +1.35 1.12 1.6 +0.20 0.12 +0.01 0.11 1.6
FF Aql 6.40 1.84 −0.14 0.01 −9.34 0.01 +0.58 0.27 +0.36 0.32 2.4 −0.87 0.17 −0.47 0.18 5.6 O

Notes. ϖ is the GDR2 parallax (Sect. 2.3), except when marked with * (HIPPARCOS; van Leeuwen 2007 and + Berdnikov et al. 2000, for RY Vel only). The PM vectors at the HIPPARCOS (μHip) and GDR2 (μG2) epochs are compared to the mean PM computed using the HIPPARCOS and GDR2 positions (μHG). The observed differences are listed in terms of signal-to-noise ratio ΔHip and ΔG2. When the Arenou et al. (2018) quality parameters are not all satisfied, the star is marked with † after ΔG2 and when the RUWE 𝜚 >  1.4 they are marked with ‡. The minimum Δ anomaly is set to S/N = 5 for a strong detection (⋆), S/N = 3 for a detection (•) and S/N = 2 for a suspected binary (°). The binary type as listed in the database by Szabados (2003b) is provided in the “Bin. type” column. The complete table is available at the CDS. The binary type is indicated using this code: B – spectroscopic binary (: when confirmation is needed); b – photometric companion, physical relation should be investigated; O – spectroscopic binary with known orbit; V – visual binary.

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