The positions and unabsorbed 0.2–12 keV X-ray fluxes of the ULX candidates.
| Host galaxy . | Right ascension . | Declination . | Source flux . |
|---|---|---|---|
| . | . | . | (erg cm−2 s−1) . |
| NGC 533 | 01:25:33.63 | +01:46:42.6 | 2.9 ± 0.2 × 10−14 |
| NGC 741 | 01:56:16.14 | +05:38:13.2 | 2.5 ± 0.3 × 10−14 |
| AM 0644−741 | 06:43:02.24 | −74:14:11.1 | 3.5 ± 0.2 × 10−14 |
| ESO 306−003 | 05:29:07.21 | −39:24:58.4 | 2.4 ± 0.4 × 10−14 |
| Host galaxy . | Right ascension . | Declination . | Source flux . |
|---|---|---|---|
| . | . | . | (erg cm−2 s−1) . |
| NGC 533 | 01:25:33.63 | +01:46:42.6 | 2.9 ± 0.2 × 10−14 |
| NGC 741 | 01:56:16.14 | +05:38:13.2 | 2.5 ± 0.3 × 10−14 |
| AM 0644−741 | 06:43:02.24 | −74:14:11.1 | 3.5 ± 0.2 × 10−14 |
| ESO 306−003 | 05:29:07.21 | −39:24:58.4 | 2.4 ± 0.4 × 10−14 |
Notes. The positions of the ULX candidates in NGC 533, NGC 741 and AM 0644−741 are accurate to within 0.6 arcsec (90 per cent confidence level), for the source in ESO 306−003 this value is 1.3 arcsec. We fit the fluxes assuming an absorbed power law with photon index 1.7 and NH = 3 × 1020 cm−2 for consistency with the method used by Walton et al. (2011).
The positions and unabsorbed 0.2–12 keV X-ray fluxes of the ULX candidates.
| Host galaxy . | Right ascension . | Declination . | Source flux . |
|---|---|---|---|
| . | . | . | (erg cm−2 s−1) . |
| NGC 533 | 01:25:33.63 | +01:46:42.6 | 2.9 ± 0.2 × 10−14 |
| NGC 741 | 01:56:16.14 | +05:38:13.2 | 2.5 ± 0.3 × 10−14 |
| AM 0644−741 | 06:43:02.24 | −74:14:11.1 | 3.5 ± 0.2 × 10−14 |
| ESO 306−003 | 05:29:07.21 | −39:24:58.4 | 2.4 ± 0.4 × 10−14 |
| Host galaxy . | Right ascension . | Declination . | Source flux . |
|---|---|---|---|
| . | . | . | (erg cm−2 s−1) . |
| NGC 533 | 01:25:33.63 | +01:46:42.6 | 2.9 ± 0.2 × 10−14 |
| NGC 741 | 01:56:16.14 | +05:38:13.2 | 2.5 ± 0.3 × 10−14 |
| AM 0644−741 | 06:43:02.24 | −74:14:11.1 | 3.5 ± 0.2 × 10−14 |
| ESO 306−003 | 05:29:07.21 | −39:24:58.4 | 2.4 ± 0.4 × 10−14 |
Notes. The positions of the ULX candidates in NGC 533, NGC 741 and AM 0644−741 are accurate to within 0.6 arcsec (90 per cent confidence level), for the source in ESO 306−003 this value is 1.3 arcsec. We fit the fluxes assuming an absorbed power law with photon index 1.7 and NH = 3 × 1020 cm−2 for consistency with the method used by Walton et al. (2011).
This PDF is available to Subscribers Only
View Article Abstract & Purchase OptionsFor full access to this pdf, sign in to an existing account, or purchase an annual subscription.
