Table 6
Identification flags.
| Flag | Description |
|---|---|
| ps | X-ray variability indicating spin period |
| xrb | Other secure HMXB identification (e.g. BH binary) |
| po | Optical variability indicating orbital period |
| os | Orbital solution exists |
| ox | Assuming X-ray period as orbital period |
| oo | Assuming optical period as orbital period |
| oxo | Periods from X-ray and optical are consistent |
| em | Balmer (Hα) emission detected |
| sx | IR excess found from SED fit |
| ix | IR excess found in IR colours |
| xvs | X-ray variability from eROSITA larger than 100(a) |
| xvl | Long term variability larger than 30(a) |
| xs | Typical X-ray spectrum (well described by power-law (PL) with index <1.3) |
| xs: | X-ray spectrum well fit with PL index frozen to 1(b) |
| wd | X-ray spectrum typical for Be/WD XRB |
| oi | Good optical match |
| qc | Match with a catalogue contradicting HMXB nature |
| nv | No counterpart in VMC selection found |
| nm | No counterpart in MCPS selection found |
| ns | SED fit contradicting OB classification |
Notes. Flags indicating either typical behaviour of a HMXB (top part) or of contamination to the catalogue caused by chance-coincidence (bottom part). If not otherwise mentioned, flags with a colon indicate an uncertain property or a weaker version of the original flag. (a)Using var as described in Sect. 4.2.2 as a measure. The analysis of short- and long-term variability in comparison to AGNs is described in Sect. 5.4. (b)For faint sources, a high local absorption can lead to similar spectra as harder PL indices. A large amount of absorbing circumstellar matter is often observed in HMXBs.
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