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Table 2.

Gaia information, inferred distances, and peculiar velocities of the 44 NS-HMXB sources with good astrometric data quality.

Name pmra pmdec Parallax a.e.n. ( † ) σa.e.n.( † †) rest RV Ref. vpec
[mas yr−1] [mas yr−1] [mas] [mas] [kpc] [km s−1] [km s−1]
IGR J00370+6122 −1.80 ± 0.01 −0.53 ± 0.01 0.272 ± 0.012 0.07 7.91 −80.0 ± 3.0 [1]
1A 0114+650 −1.24 ± 0.01 0.76 ± 0.01 0.196 ± 0.011 0.06 6.20 −31.0 ± 5.0 [2]
4U 0115+634 −1.68 ± 0.01 0.50 ± 0.01 0.136 ± 0.016
IGR J01363+6610 −1.63 ± 0.01 −0.03 ± 0.01 0.167 ± 0.011 0.06 4.70
IGR J01583+6713 −1.20 ± 0.01 0.30 ± 0.01 0.133 ± 0.013
LS I+61 303 −0.42 ± 0.01 −0.26 ± 0.01 0.378 ± 0.013 0.07 8.11 −41.4 ± 0.6 [3]
EXO 0331+530 −0.27 ± 0.02 0.44 ± 0.01 0.134 ± 0.020
X Per −1.28 ± 0.05 −1.87 ± 0.02 1.627 ± 0.037 0.29 167.97 1.0 ± 0.9 [4]
XTE J0421+560 −0.47 ± 0.02 −0.51 ± 0.01 0.210 ± 0.015 0.09 15.08
RX J0440.9+4431 0.10 ± 0.02 −1.19 ± 0.01 0.379 ± 0.015 0.07 7.05
EXO 051910+3737.7 1.30 ± 0.04 −4.00 ± 0.02 0.721 ± 0.030 0.18 23.83
1A 0535+262 −0.59 ± 0.03 −2.88 ± 0.02 0.525 ± 0.023 0.12 25.19 −30.0 ± 4.0 [5]
HD 259440 −0.03 ± 0.02 −0.43 ± 0.02 0.540 ± 0.023 0.10 10.64 36.9 ± 0.8 [6]
SAX J0635.2+0533 −0.42 ± 0.01 0.40 ± 0.01 0.142 ± 0.015 0.05 2.84
IGR J08262−3736 −2.37 ± 0.01 3.18 ± 0.01 0.178 ± 0.010 0.04 2.81
IGR J08408−4503 −7.46 ± 0.02 6.10 ± 0.01 0.443 ± 0.017 0.14 16.19 15.3 ± 0.5 [7]
Vela X-1 −4.82 ± 0.01 9.28 ± 0.01 0.496 ± 0.015 0.10 12.15 −3.2 ± 0.9 [8]
GRO J1008−57 −4.70 ± 0.02 3.56 ± 0.01 0.243 ± 0.013 0.03 0.47
2FGL J1019.0−5856 −6.45 ± 0.01 2.26 ± 0.01 0.227 ± 0.010 0.05 3.30 33.0 ± 3.0 [9]
1A 1118−615 −5.42 ± 0.01 1.37 ± 0.01 0.329 ± 0.011 0.07 6.38
1E 1145.1−6141 −6.23 ± 0.01 2.36 ± 0.01 0.127 ± 0.010 0.03 1.04 -13.0 ± 3.0 [10]
2E 1145.5−6155 −6.23 ± 0.02 1.60 ± 0.01 0.475 ± 0.017 0.11 10.14
EXMS B1210−645 −5.95 ± 0.02 0.45 ± 0.02 0.264 ± 0.018 0.11 6.77
GX 301−2 −5.23 ± 0.02 −2.07 ± 0.01 0.251 ± 0.016 0.11 12.94 4.1 ± 2.4 [11]
GX 304−1 −4.34 ± 0.01 −0.24 ± 0.01 0.540 ± 0.014 0.09 10.30
PSR B1259−63 −7.09 ± 0.01 −0.34 ± 0.01 0.443 ± 0.013 0.07 4.90 0.0 ± 1.0 [12] ( * )
IGR J14331−6112 −7.25 ± 0.11 −3.98 ± 0.09 0.415 ± 0.116
4U 1538−522 −6.71 ± 0.01 −4.11 ± 0.01 0.128 ± 0.015 −158.0 ± 11.0 [13]
1H 1555−552 −3.12 ± 0.02 −3.22 ± 0.01 0.732 ± 0.018 0.09 9.58
IGR J16195−4945 −0.18 ± 0.06 −0.54 ± 0.03 0.359 ± 0.051 0.08 0.63
IGR J16465−4507 −1.76 ± 0.02 −3.06 ± 0.01 0.296 ± 0.017
4U 1700−377 2.41 ± 0.03 5.02 ± 0.01 0.633 ± 0.026 0.15 25.81 −60.0 ± 10.0 [14]
RX J1744.7−2713 −0.86 ± 0.02 −2.30 ± 0.02 0.787 ± 0.024 0.09 4.67
IGR J17544−2619 −0.51 ± 0.03 −0.67 ± 0.02 0.396 ± 0.027 0.18 36.39 −46.8 ± 4.0 [15]
LS 5039 7.43 ± 0.01 −8.15 ± 0.01 0.490 ± 0.015 17.3 ± 0.5 [16]
XTE J1855−026 −2.52 ± 0.02 −6.77 ± 0.01 0.078 ± 0.016
IGR J20006+3210 −2.85 ± 0.02 −4.30 ± 0.02 0.067 ± 0.021
RX J2030.5+4751 −2.71 ± 0.02 −4.54 ± 0.02 0.419 ± 0.016 0.15 30.89
GRO J2058+42 −2.21 ± 0.02 −3.35 ± 0.01 0.078 ± 0.015
SAX J2103.5+4545 −3.51 ± 0.01 −3.16 ± 0.01 0.131 ± 0.013
IGR J21347+4737 −2.21 ± 0.01 −2.56 ± 0.01 0.084 ± 0.014 0.02 0.22
Cep X-4 −2.96 ± 0.01 −2.20 ± 0.01 0.105 ± 0.013
4U 2206+543 −4.17 ± 0.02 −3.32 ± 0.01 0.305 ± 0.014 0.11 14.00 −54.5 ± 1.0 [17]
SAX J2239.3+6116 −2.34 ± 0.02 −1.02 ± 0.01 0.104 ± 0.014 0.04 1.04

Notes. pmra and pmdec are respectively the proper motion in RA and Dec available in Gaia EDR3. ( † )astrometric_excess_noise, ( † †)astrometric_excess_noise_sig, see the online documentation (https://gea.esac.esa.int/archive/documentation/GDR3/). rest is the inferred distance, RV the systemic radial velocity, and vpec the inferred peculiar velocity. ( * )Since the systemic radial velocity is not given in this reference (Johnston et al. 1994), we fit the radial velocity curve in Fig. 2 using WebPlotDigitizer (Rohatgi 2021) to retrieve the value in the table.

References. [1] Grunhut et al. (2014); [2] Koenigsberger et al. (2003); [3] Aragona et al. (2009); [4] Grundstrom et al. (2007); [5] Hutchings (1984); [6] Moritani et al. (2018); [7] Gamen et al. (2015); [8] Stickland et al. (1997); [9] Strader et al. (2015); [10] Hutchings et al. (1987); [11] Kaper et al. (2006); [12] Johnston et al. (1994); [13] Abubekerov et al. (2004); [14] Gies & Bolton (1986); [15] Nikolaeva et al. (2013); [16] Casares et al. (2011); [17] Stoyanov et al. (2014).

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