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Table 3.

eROSITA X-ray properties from aperture photometry.

Source eRASS [1] eRASS:4? [2] Net cts. [3] F0.5 − 7 kev, s[4] F0.5 − 7 kev, c[5] L2 − 10 keV[6] αOX[7]
[erg cm−2 s−1] [erg cm−2 s−1] [erg s−1]
J202040−621509 1 No 9.5 ± 3.9 7 . 82 − 4.47 + 11.06 × 10 − 14 $ 7.82^{+11.06}_{-4.47} \times 10^{-14} $ Unconst. 1 . 83 − 0.83 + 1.35 × 10 46 $ 1.83^{+1.35}_{-0.83}\times 10^{46} $( * ) − 1 . 27 − 0.10 + 0.09 $ -1.27^{+0.09}_{-0.10} $
J020916−562650 2, 3, 4 Yes 21.5 ± 5.3 4 . 99 − 2.02 + 3.71 × 10 − 14 $ 4.99^{+3.71}_{-2.02}\times 10^{-14} $ 2 . 57 − 0.80 + 1.35 × 10 − 14 $ 2.57^{+1.35}_{-0.80}\times 10^{-14} $ 8 . 70 − 2.18 + 2.71 × 10 45 $ 8.70^{+2.71}_{-2.18}\times 10^{45} $ − 1 . 15 − 0.05 + 0.05 $ -1.15^{+0.05}_{-0.05} $

Notes. [1] eRASS in which the quasar is detected. The bold font indicates the eRASS in which Pb is minimal. [2] Was the source detected in eRASS:4? [3] Net counts in the 0.2−2.3 keV eRASS:4 images. [4] Maximal single eRASS flux in the 0.5-keV band. [5] eRASS:4 flux. [6] Hard restframe X-ray luminosity. ( * )We note that the luminosity of J202040−621509 is only based on its eRASS1 detection, while for J020916−562650 we used the cumulative data from eRASS:4. [7] Spectral index connecting X-ray to optical SED.

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