Table 3
Input parameters used to model the SED.
| Date | R diss | Rdiss/RS |
|
B | Γ | γ b | γ max | s 1 | s 2 | ||
| [1] | [2] | [3] | [4] | [5] | [6] | [7] | [8] | [9] | [10] | ||
|
|
|||||||||||
| 2009 May 05 | 67.5 | 1500 | 0.030 | 4.4 | 13 | 10 | 3000 | 0 | 2.65 | ||
| 2009 May 15 | 49.5 | 1100 | 0.0055 | 6.0 | 11 | 50 | 1500 | 0 | 2.7 | ||
| 2010 Jul. 08 | 103.5 | 2300 | 0.044 | 2.1 | 16 | 50 | 3000 | 0 | 2.8 | ||
| 2011 Jun. 21 | 108.0 | 2400 | 0.025 | 2.2 | 16 | 240 | 4000 | 0.5 | 3.9 | ||
| 2011 Oct. 09 | 90.0 | 2000 | 0.032 | 3.3 | 12 | 80 | 5000 | 1 | 3.05 | ||
Notes. Column [1]: date; Col. [2]: distance of the blob from the black hole in units of 1015 cm; Col. [3]: Rdiss in units of the Schwarzschild radius RS; Col. [4]: power injected in the blob calculated in the comoving frame, in units of 1045 erg s-1; Col. [5]: magnetic field in Gauss; Col. [6]: bulk Lorentz factor; Col. [7]: random Lorentz factor of the injected electrons at the break of the distribution; Col. [8]: maximum random Lorentz factor of the injected electrons; Cols. [9] and [10]: slopes of the injected electron distribution [Q(γ)] below and above γb. All models assume a black hole mass M = 1.5 × 108 M⊙ and an accretion disc luminosity Ld = 9 × 1045 erg s-1, corresponding to Ld/LEdd = 0.4. The X-ray corona has a luminosity LX = 0.3Ld. The radius of the BLR is fixed to RBLR = 3 × 1017 cm. The spectral shape of the corona is assumed to be ∝ ν-1exp(− hν/150 keV). The viewing angle is 3° for all models.
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