Table 1
Measured absorption line properties and orbital parameters of sources with observed Fe absorption lines.
| Source | Ref. | Type | Porb(h) | i (°) | Fe xxv Kα | Fe xxvi Kα | Fe xxv Kβ | Fe xxvi Kβ |
| E (keV) | E (keV) | E (keV) | E (keV) | |||||
| EW (eV) | EW (eV) | EW (eV) | EW (eV) | |||||
|
|
||||||||
| XB 1916-053 (NS) | (1) | LMXB | 0.8 | 60−80 |
|
|
a
|
|
| D, B |
|
|
|
 eV |
||||
| GX 13+1 (NS) | (2) | LMXB | 577.4 | 60−80b |
|
7.02 ± 0.06 |
|
|
| Atol, B | − 20 ± 5 | − 41 ± 7 | − 33 ± 12 | − 37 ± 15 | ||||
| MXB 1659-298 (NS) | (3) | LMBX | 7.1 | ~80 | 6.64 ± 0.02 |
|
– | – |
| D, E, T |
|
|
– | – | ||||
| X 1254-690 (NS) | (4) | LMXB | 3.9 | 60−80 | – | 6.95 ± 0.03 | – |
|
| D | – |
|
– | − 17 ± 9 | ||||
| X 1624-490 | (5) | LMXB | 20.9 | 60−80 | 6.72 ± 0.03 | 7.0 ± 0.02 | – | – |
| D |
|
|
– | – | ||||
| XB 1323-619 | (6) | LMXB | 2.93 | 60−80 | 6.70 ± 0.03 | 6.98 ± 0.04 | – | – |
| D, qB | − 22 ± 3 | − 27 ± 4 | – | – | ||||
| Cir X-1 (NS) | (7) | B, D, O, J | 398 | high | 6.701 ± 0.009 | 6.965 ± 0.01 | – | – |
| 4U 1630-472 (BH) | (8) | LMXB | 690 | ~70 | 6.72 ± 0.01 |
|
|
|
| D, T, O | − 21 ± 3 |
|
|
|
||||
| GRO J1655-40 (BH) | (9) | microq | 62.9c | 69−85 | 6.63 ± 0.07 | 6.95 ± 0.10 | 7.66 ± 0.13 | – |
| D, O |
|
|
|
– | ||||
| (10) | 6.698 ± 0.001 | 6.999 ± 0.002 | 7.842 ± 0.005 | 8.277 ± 0.01 | ||||
| − 45.59 ± 1.8 | − 30.82 ± 2.37 | − 48.11 ± 4.46 | − 27.63 ± 5.53 | |||||
| GRS 1915+105 (BH) | (11) | microq | 804 | ~70 |
|
|
|
|
|
|
|
|
|||||
| (12) | 6.684 ± 0.022 | 6.984 ± 0.009 | – | – | ||||
| − 6 | − 18 | – | – | |||||
| H1743-322 (BH) | (13) | microq | – | ~70 | 6.709 ± 0.004 | 6.981 ± 0.004 | – | – |
| D, T, O | − 5 ± 1 | − 20 ± 2 | – | – | ||||
| IGR J17091-3624 (BH) | (14) | T, O | – | – | 6.91 ± 0.01 |
|
– | – |
|
|
– | – | |||||
Notes.L – LMXB; microq – micro-quasars; D – deeps; E – eclipses; B – bursts; qB – quasi-periodic bursts; T – transient; O – outburst; J – radio jet.
Identified as S xvi and Ni xxvii transitions by Boirin et al. (2004).
Low i suggested by high radio to X-ray ratio (Schnerr et al. 2003), but high i ≃ 60−80° by detection of Fe abs. lines (Díaz Trigo et al. 2012).
From optical observations (Orosz & Bailyn 1997).
Reference. (1) XMM, Boirin et al. (2004); (2) XMM, Ueda et al. (2001); Díaz Trigo et al. (2012); (3) XMM, Sidoli et al. (2001); (4) XMM, Boirin & Parmar (2003); (5) XMM, Parmar et al. (2002); (6) XMM, Church et al. (2005); (7) Chandra; Brandt & Schulz (2000); (8) Suzaku epoch 4, Kubota et al. (2007); (9) ASCA, Ueda et al. (1998); (10) Chandra, Miller et al. (2008); (11) ASCA, Kotani et al. (2000); (12) Chandra, Lee et al. (2002); (13) Chandra epoch 1, Miller et al. (2006); (14) Chandra, King et al. (2012).
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