Table 7
Main results for the X-ray binaries (see Fig. 10) identified in the present sample of INTEGRAL sources.
| Object | Hα | Hβ | R | A V | d | Spectral | L X | ||
|
|
|||||||||
| EW | Flux | EW | Flux | mag | (mag) | (kpc) | type | ||
|
|
|||||||||
| IGR J00515−7328 | 4.5 ± 0.6 | 8.4 ± 1.0 | <1.1 | <3.4 | 15.18a | ~1.1b | 60c | O8 V or B0 III | 0.5d (0.1–2; R) |
| 1.3 (0.16–3.5; E) | |||||||||
| 8–11d,e (0.2–10; X) | |||||||||
| <0.027 (0.2–10; N) | |||||||||
| 15–30 (0.3–10; X) | |||||||||
| RX J0101.8−7223 | 28.4 ± 1.4 | 46 ± 2 | 2.4 ± 0.5 | 10 ± 2 | ~14.8f | ~1.5 | 60c | O9–B0 III | 2.3–5.8g (0.2–10; A, R, N) |
| 3.9f (0.2–10; N) | |||||||||
| 36.5h (0.2–10; N) | |||||||||
| IGR J22534+6243 | 31.8 ± 1.6 | 81.0 ± 0.4 | 3.4 ± 0.5 | 3.3 ± 0.5 | 13.7 | ~6.7 | ~4.4 | early B III | 0.003 (0.1–2.4; R) |
| 0.012–0.10 (0.5–10; R, X, C) | |||||||||
| 0.14 (17–60; I) | |||||||||
|
|
|||||||||
| IGR J18256−1035 | 5.5 ± 0.5 | 0.11 ± 0.03 | <10 | <0.03 | — | — | 8i | — | 0.22 (0.3–10; C) |
| 0.15 (2–10; X) | |||||||||
| 0.47 (20–40; I) | |||||||||
| <0.21 (40–100; I) | |||||||||
| 0.56 (17–60; I) | |||||||||
Notes.The upper part of the table deals with the HMXBs identified here, whereas the lower part reports on the single LMXB of our sample. EWs are expressed in Å, line fluxes are in units of 10-15 erg cm-2 s-1, X-ray luminosities are in units of 1035 erg s-1, and the reference band (between round brackets) is expressed in keV. In the last column, the upper case letter indicates the satellite and/or the instrument with which the corresponding X-ray flux measurement was obtained (see text).
from Massey (2002);
from Harries et al. (2003);
from Coe et al. (2010);
from Sturm et al. 2011;
from Haberl et al. (2008);
from Haberl & Pietsch (2004);
from Townsend et al. (2013);
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