Table 2.
Distance, density, mass outflow rate, momentum rate and kinetic power for each absorber.
| r/rs | r (pc) | n (cm−3) | Ṁout (M⊙ yr−1) | Ṗout/Ṗrad | ĖK/Lbol | |
|---|---|---|---|---|---|---|
| Warm absorber | ||||||
| rmin,WA | 3.2 × 105 | 18 | 3.6 × 105 | 2.63 Cv | 0.05 Cv | 4.2 × 10−5 Cv |
| rmax,WA | 5.2 × 107 | 3 × 103 | 13 | 430 Cv | 8 Cv | 7 × 10−3 Cv |
| Entrained UFO | ||||||
| rvar,E-UFO | 1.7 × 106 | 110 | 7.5 × 103 | 400 Cv | 495 Cv | 29 Cv |
| Ultra-fast outflow | ||||||
| rmin,UFO | 57 | 3.2 × 10−3 | 2.3 × 109 | 0.41 | 0.62 | 0.04 |
Notes. The distance from the black hole r is given in both units of Schwarzschild radius rs = 2GMBH/c2 and parsec. We listed the estimated density n at such a distance, mass outflow rate in units of solar masses per year, momentum rate in units of the radiation momentum rate Ṗrad = Lbol/c, and kinetic power in units of Lbol. The symbol Cv represents the filling factor of the region, assumed unitary for the region containing the UFO. We use MBH ∼ 5.9 × 108 M⊙ and Lbol ∼ 5.5 × 1045 erg s−1 from Shen et al. (2011). For UFO and E-UFO we only reported the most likely value for the distance of the absorber, while for the WA it is not possible to constrain the region, therefore we report the values computed using rmin, and consider a typical value for the upper limit of rmax,WA ∼ 3 kpc (Di Gesu et al. 2013).
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