Table F.1.
Comparison with previous results on the same observations.
| Source | This work (v/c) | Previous works | Detection (v/c) |
|---|---|---|---|
| (1) | (2) | (3) | (4) |
| 3C 120 | NO | Tombesi et al. (2014) | NO |
| 3C 390.3 | NO | Tombesi et al. (2014) | NO |
| Ark 564 | NO | Tombesi et al. (2010) | NO |
| ESO511-G030 | NO | Tombesi et al. (2010) | NO |
| Mkn 766* | 0.30 ± 0.02 | Tombesi et al. (2010) | 0.091 ± 0.004 |
| MRK 0110 | 0.16 ± 0.01 | Tombesi et al. (2010) | NO |
| Mrk 335 | NO | Tombesi et al. (2010) | NO |
| Mrk 509† | NO | Tombesi et al. (2010) | 0.141 ± 0.002 |
| Mrk 1044‡ | NO | Xu et al. (2023) | NO |
| NGC 1566 | NO | Jana et al. (2021) | NO |
| NGC 2617 | 0.065 ± 0.008 | Giustini et al. (2017) | redshifted |
| NGC 4051 | 0.018 ± 0.006 | Tombesi et al. (2010) | 0.018 ± 0.004 |
| NGC 4593 | NO | Tombesi et al. (2010) | NO |
| NGC 5548 | 0.021 ± 0.008 | Tombesi et al. (2010) | NO |
| 0.428 ± 0.008 | Tombesi et al. (2010) | NO | |
| PKS0558-50 | NO | Tombesi et al. (2014) | NO |
| UGC 3973 | NO | Tombesi et al. (2010) | 0.091 ± 0.004 |
Notes. Column 1: Source name; Column 2: our results; Column 3: previous studies on the source; Column 4: results in previous work. *An absorption feature at the same energy is detected but interpreted as an Fe H-like edge with v ∼ 0.05c, following Pounds et al. (2003), see Sec. 5 for details. †A subthreshold feature at similar energies is reported in Tab. E.1. ‡ A UFO with vout = 0.2c is detected in the same observation in the soft band through RGS spectroscopy (Xu et al. 2023).
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