Table A.6
Best-fit parameters of spectral analysis for 1996 and 2001 with PCA/RXTE observations of NGC 4051 in 3–30 keV energy rangea.
| Observational | α = | log (A) |  |
Eline |  |
 |
|---|---|---|---|---|---|---|
| ID | Γ − 1 | (keV) | (dof) | |||
| 10301-01-04-00 | 0.49 ± 0.08 | –0.02 ± 0.01 | 1.92 ± 0.3 | 6.59 ± 0.08 | 0.9 ± 0.1 | 1.02 (93) |
| 10301-01-07-00 | 0.77 ± 0.09 | 0.12 ± 0.03 | 2.74 ± 0.7 | 6.49 ± 0.03 | 1.9 ± 0.2 | 1.09 (62) |
| 10301-01-08-00 | 0.85 ± 0.09 | 0.17 ± 0.03 | 3.32 ± 0.2 | 6.46 ± 0.07 | 2.1 ± 0.2 | 0.57 (62) |
| 10301-01-09-00 | 1.01 ± 0.07 | 0.37 ± 0.07 | 6.99 ± 0.3 | 6.41 ± 0.03 | 2.6 ± 0.5 | 1.01 (57) |
| 10301-01-22-00 | 0.61 ± 0.09 | –0.01 ± 0.01 | 0.98 ± 0.1 | 6.67 ± 0.09 | 0.68 (57) | |
| 10301-01-58-00 | 0.59 ± 0.09 | –0.02 ± 0.01 | 1.46 ± 0.1 | 6.57 ± 0.06 | 0.7 ± 0.3 | 0.82 (57) |
| 10301-01-59-00 | 0.77 ± 0.05 | 0.09 ± 0.03 | 2.79 ± 0.1 | 6.18 ± 0.07 | 1.7 ± 0.2 | 1.09 (57) |
| 10301-01-60-00 | 1.03 ± 0.06 | 0.47 ± 0.06 | 8.26 ± 0.5 | 6.36 ± 0.09 | 3.8 ± 0.4 | 0.87 (57) |
| 10301-01-61-00 | 0.85 ± 0.05 | 0.19 ± 0.04 | 4.10 ± 0.4 | 6.43 ± 0.08 | 1.9 ± 0.1 | 1.24 (57) |
| 20318-01-01-00 | 0.35 ± 0.09 | 0.04 ± 0.01 | 0.24 ± 0.1 | 6.68 ± 0.04 | 0.6 ± 0.3 | 0.83 (57) |
| 50153-01-01-00 | 0.57 ± 0.09 | –0.14 ± 0.07 | 2.97 ± 0.3 | 6.50 ± 0.09 | 1.6 ± 0.2 | 0.79 (79) |
| 50153-01-01-01 | 1.01 ± 0.10 | 0.03 ± 0.01 | 8.37 ± 0.3 | 6.37 ± 0.08 | 3.6 ± 0.1 | 0.75 (50) |
| 50153-01-01-02 | 0.98 ± 0.09 | 0.97 ± 0.14 | 6.24 ± 0.2 | 6.43 ± 0.09 | 2.4 ± 0.4 | 0.85 (50) |
| 50153-01-01-03 | 1.00 ± 0.08 | 0.97 ± 0.14 | 5.71 ± 0.2 | 6.42 ± 0.03 | 2.1 ± 0.2 | 0.85 (50) |
| 50153-01-01-05 | 0.34 ± 0.08 | 0.33 ± 0.14 | 1.28 ± 0.2 | 6.52 ± 0.04 | 0.9 ± 0.3 | 0.85 (50) |
| 50153-01-01-06 | 0.93 ± 0.04 | 0.06 ± 0.03 | 5.38 ± 0.2 | 6.46 ± 0.08 | 2.2 ± 0.4 | 0.95 (50) |
Notes. (a) The spectral model is gabs x (BMC + Laor). (b)Normalization parameters of the BMC and the Laor components are in units of
erg s−1 kpc−2, where L35 is the source luminosity in units of 1035 erg/s, d10 is the distance to the source in units of 10 kpc, and the Laor component is in units of 10−4 × total photons cm−2 s−1 in line; the parameters of the gabs model were fixed (Eline = 0.75 keV, σ = 0.02 keV, line depth varies from 0.0001 to 0.01) and the parameter kTs of BMC model was fixed at 0.2 keV.
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