Table 7.
Gaia-EDR3 sources that fall within a 3σ positional uncertainty radius of the X-ray sources.
| Gaia-EDR3 | Associated PSR | μα | μδ | D | Teff | V | log (fx/fv) | Macc88 | CV07 | BJ19 | Excluded |
|
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (mas y−1) | (mas y−1) | (kpc) | (K) | (mag) | (Spectral type) | (S) | (GXY) | |||||
| 237123598225544064 | J0340+4130 (4.64″) | −0.5 ± 0.4 | −2.6 ± 0.4 | 2.0 ± 1.1 | 4154 ± 182 | 20.6 ± 0.7 | −0.5 | AGN | − | S, QSR | Y | Y |
| 5339616527672093056 | J1125–5825 (1.27″) | −4.8 ± 0.1 | 1.1 ± 0.1 | 4.0 ± 2.0 | − | 18.7 ± 0.4 | −0.85 | M, AGN, GXY | M1, M5, M2 | S, QSR | N | Y |
| 5339616527704864768 | J1125–5825 (3.85″) | −6.8 ± 0.1 | 1.0 ± 0.1 | 1.7 ± 0.1 | 5488 ± 393 | 16.4 ± 0.3 | −1.7 | M, K, GXY | G8 | S, GXY | N | Y |
| 5878785517750906240 | J1435–5954 (4.35″) | −9.5 ± 0.1 | −2.4 ± 0.1 | 2.2 ± 1.1 | 6635 ± 180 | 19.1 ± 0.4 | −1.3 | M, GXY | M6, M7, M8 | S, GXY | N | Y |
| 5878785517754291968 | J1435–5954 (6.83″) | −6.5 ± 0.2 | −2.6 ± 0.1 | 2.3 ± 1.1 | 5456 ± 212 | 19.9 ± 0.5 | −0.9 | M, AGN, GXY | M5, M6, K7 | S, GXY, QSR | N | Y |
| 4358428942492430336 | J1622–0315 (0.89″) | −13.2 ± 0.3 | 2.3 ± 0.2 | 2.7 ± 1.9 | 6108 ± 254 | 19.6 ± 0.4 | −0.7 | M, GXY, AGN | − − − | S | Y | Y |
| 4310888159960965632 | J1857+0943 (2.71″) | −1.9 ± 0.6 | −4.1 ± 0.6 | 1.5 ± 0.8 | − | 21.5 ± 0.5 | −0.2 | AGN | − − − | S, GXY, QSR | Y | Y |
| 4186460380401976448 | J1926–1314 (0.96″) | − | − | − | − | 18.2 ± 0.5 | −2.1 | M,K | − | S, QSR | N | Y |
| 4186460380401976576 | J1926–1314 (1.96″) | 5.6 ± 0.9 | −4.9 ± 0.5 | 4.2 ± 2.3 | − | 14.7 ± 0.4 | −1.8 | M,K | − | S, QSR | N | Y |
| 4186460380410768640 | J1926–1314 (2.97″) | 2.4 ± 0.1 | −5.4 ± 0.1 | 1.5 ± 0.1 | 5861 ± 123 | 18.4 ± 0.5 | −3.5 | B-F,G,K | M3, M4, F-8 | S, GXY | N | Y |
Notes. The respective pulsars are listed in the second column, followed by the angular distance to the Gaia-EDR3 source in parentheses. The next columns show the proper motions, distances and effective temperatures obtained from TESS Input Catalog – v8.0 (Stassun et al. 2019). The V-band magnitude (Vega) was estimated from the Gaia magnitudes using Johnson-Cousins relationships of Landolt standard stars that were observed with Gaia according to Evans et al. (2018). log (fx/fv) is the X-ray to optical flux ratio. The Macc88, CV07 and BJ19 columns represent classifications according to Maccacaro et al. (1988) Covey et al. (2007) and Bailer-Jones et al. (2019) respectively. S, GXY, QSR and AGN represents star, Galaxy, Quasar and active galactic nucleus, respectively. For all investigated optical/NIR sources, Stassun et al. (2019) reported a star classification in the TESS input catalog.
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