| Name | Type | R.A. (J2000) | Dec (J2000) | Jet speed | ν (GHz) | F (mJy) | D (kpc) | δ | Γ | θ (deg) |
|---|---|---|---|---|---|---|---|---|---|---|
| CI Cam | HMXRB | 04:19:42.13 | +55:59:57.7 | 0.15c | 22.5 | 450 | 1.0 | 1.01 | 1.01 | 83 |
| XTE J1118+480 | HMXRB | 11:18:10.7 | +48:02:12.3 | 0.4c | 2 x 10+05 | 20 | 1.9 | — | — | — |
| GRO J1655-40 | HMXRB | 16:54:00.13 | -39:50:44.9 | 0.27±0.03c | 1.6 | 3400 | 3.1 | 0.46 | 2.55 | 81 |
| KS 1731-260 | LMXRB | 17:34:13.46 | -26:05:18.6 | — | — | — | — | — | — | — |
| 1E 1740.7-2942 | LMXRB | 17:43:54.83 | -29:44:42.0 | 0.7c | — | — | — | — | — | — |
| XTE J1748-2829 | — | 17:43:54.83 | -29:44:42.0 | ? | 4.9 | 410 | 8.0 | 1.01 | 1.46 | 64 |
| GRS 1758-258 | LMXRB | 18:01:12.40 | -25:44:36.1 | <=0.3c | — | — | — | — | — | — |
| V4641 Sagitarii | HMXRB | 18:19:21.63 | -25:24:25.84 | 0.9c | 4.9 | 400 | 9.6 | 7.31 | 22.37 | 6.9 |
| V691 CrA | LMXRB | 18:25:46.8 | -37:06:18.52 | — | — | — | — | — | — | — |
| LS 5039 | HMXRB | 18:26:15.0 | -14:50:54.2 | >0.15c | 5.0 | 16 | 3.0 | 1.04 | 1.09 | 68 |
| XTE J1859+226 | HMXRB | 18:58:41.58 | +22:39:29.4 | ? | — | — | — | — | — | — |
| SS 433 | HMXRB | 19:11:49.56 | +04:58:57.8 | 0.26c | — | — | — | — | — | — |
| GRS 1915+105 | HMXRB | 19:15:11.5 | +10:56:44.9 | 0.60c | 8.6 | 655 | 12.5 | 0.57 | 2.55 | 70 |
| Cygnus X-1 | HMXRB | 19:58:21.6 | +35:12:05.78 | ? | 1x 10+04 | 15 | 2.0 | — | — | — |
| Cygnus X-3 | HMXRB | 20:32:25.78 | +40:57:27.9 | 0.48-0.81c | 15.0 | 10500 | 10.0 | 3.14 | 2.10 | 14 |
| XTE J1720-318 | LMXRB | 17:19:58.9 | -31:45:01.11 | — | — | — | — | — | — | — |
| Sco X-1 | LMXRB | 16:19:55.06 | -15:38:25.0 | — | 5.0 | 20 | 2.8 | 1.39 | 3.20 | 44 |
List of the 17 known microquasars observable within the Noto–KM3NeT declination limits. The information on distance (D), observing frequency (ν), and corresponding flux density (Fν) was taken from the study by Distefano et al. (2002). From the same work, we also adopted the values of the Doppler factor (δ), the angle between the jet axis and the observer’s line of sight (θ), and the Lorentz factor (Γ), for the resolved microquasars. For unresolved microquasars, no information is available on Γ, δ, or on the jet size.