Table 9.
Millimetre and X-ray luminosities of accreting compact objects in XRBs.
| Source | Distance | Millimetre luminosity (a) | X-ray luminosity (b) | Reference |
|---|---|---|---|---|
| (kpc) | (erg s−1) | (erg s−1) | ||
| MAXI J1659−152 | 6 | (7 ± 1) × 1031 | (1.389 ± 0.001) × 1037 | van der Horst et al. (2013) |
| MAXI J1659−152 | 6 | (5 ± 1) × 1031 | (4.60 ± 0.01) × 1037 | van der Horst et al. (2013) |
| MAXI J1659−152 | 6 | < 2.6 × 1031 | (4.81 ± 0.01) × 1037 | van der Horst et al. (2013) |
| MAXI J1659−152 | 6 | < 2.7 × 1031 | (4.67 ± 0.02) × 1037 | van der Horst et al. (2013) |
| V404 Cygni | 2.39 | (3.64 ± 0.06) × 1030 | (8 ± 2) × 1034 | Tetarenko et al. (2019) |
| V404 Cygni | 2.39 | (9.4 ± 0.6) × 1029 | (1.5 ± 0.1) × 1034 | Tetarenko et al. (2019) |
| MAXI J1535−571 | 4.1 | (4.7 ± 0.2) × 1032 | (2.00 ± 0.01) × 1038 | Russell et al. (2020) |
| MAXI J1535−571 | 4.1 | (1.0 ± 0.2) × 1032 | (8.6 ± 0.1) × 1038 | Russell et al. (2020) |
| GX 339−4 | 8 | (1.53 ± 0.08) × 1031 | (1.35 ± 0.08) × 1036 | de Haas et al. (2021) |
| MAXI J1820+070 | 2.96 | (9.651 ± 0.004) × 1031 | (3.50 ± 0.01) × 1037 | Tetarenko et al. (2021) |
| GRS 1915+105 | 8.6 | 2.2 × 1031 | (2.07 ± 0.03) × 1037 | Koljonen & Hovatta (2021) |
| GRS 1915+105 | 8.6 | 2.6 × 1031 | (2.69 ± 0.01) × 1037 | Koljonen & Hovatta (2021) |
| XTE J1118+480 | 1.7 | 6.9 × 1030 | 2.4 × 1035 | Fender et al. (2001) |
| 4U 1820−30 (c) | 6.4 | (1.67 ± 0.09) × 1030 | (3.22 ± 0.03) × 1037 | Díaz Trigo et al. (2017) |
| Aql X-1 | 5.2 | (2.06 ± 0.08) × 1030 | (1.73 ± 0.01) × 1037 | Díaz Trigo et al. (2018) |
| Aql X-1 | 5.2 | (1.31 ± 0.08) × 1030 | (9.2 ± 0.1) × 1037 | Díaz Trigo et al. (2018) |
| Aql X-1 | 5.2 | (2.44 ± 0.09) × 1030 | (6.65 ± 0.07) ×10 36 | Díaz Trigo et al. (2018) |
| PSR J1023+0038 (mean) | 1.37 | (3.2 ± 0.2) × 1028 | (1.7 ± 0.2) × 1033 | This work |
| PSR J1023+0038 (high) | 1.37 | (2.0 ± 0.3) × 1028 | (2.40 ± 0.04) × 1033 | This work |
| PSR J1023+0038 (low) | 1.37 | (3.0 ± 0.5) × 1028 | (3.6 ± 0.4) × 1032 | This work |
Notes. Values are reported for those systems that have been clearly detected in the millimetre/sub-millimetre bands, have a known distance, and have simultaneous or nearly simultaneous millimetre/sub-millimetre and X-ray observations. Systems above the horizontal line are black hole systems, while those below the line are NS systems.
Millimetre luminosities are evaluated at a frequency of 100 GHz. A flat spectrum was assumed to estimate the luminosity for those cases where the flux density is available at other frequencies in the literature, except for MAXI J1820+070 (α = 0.25) and 4U 1820−30 (α = 0.13).
X-ray luminosities are evaluated over the 1–10 keV energy range and are derived from Swift/XRT observations except for the case of J1023, for which values are taken from Table 5. Spectra were extracted using the Swift/XRT data products generator (Evans et al. 2009) and fitted using an absorbed power-law model. For the second pair of simultaneous observations of GRS 1915+105, the X-ray luminosity is evaluated using NICER Obs. ID 2596010301.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.