Table 1
Input parameters for the emission models shown in Fig. 3 (first row) and Fig. 4 (other rows); “in” and “out” means inside or outside the BLR.
| γmin | γp | γmax | n1 | n2 | B [G] | K [cm-3] | R [cm] | δ | Γ | Pp,45 | Pe,45 | PB,45 | |
|
|
|||||||||||||
| All Blob | 3 | 1200 | 5 × 104 | 2.2 | 3.7 | 0.28 | 3 × 106 | 9.2 × 1014 | 75 | 50 | 247 | 2.2 | 8.2 × 10-4 |
|
|
|||||||||||||
| Jet (in) | 1 | 300 | 6 × 104 | 2 | 3.45 | 0.75 | 1.8 × 104 | 1.5 × 1016 | 19.7 | 10 | 81 | 0.34 | 6.3 × 10-2 |
| Blob | 200 | 700 | 4 × 105 | 2.2 | 3.4 | 0.1 | 6 × 106 | 7.2 × 1014 | 75 | 50 | 10.6 | 0.4 | 6.5 × 10-5 |
|
|
|||||||||||||
| Jet (out) | 3 | 2 × 103 | 6 × 104 | 2 | 4.1 | 0.09 | 3 × 102 | 1.1 × 1017 | 19.7 | 10 | 17.7 | 0.3 | 5 × 10-2 |
| Blob | 100 | 900 | 4 × 105 | 2.2 | 3.6 | 0.18 | 107 | 6.2 × 1014 | 75 | 50 | 3.9 | 0.8 | 1.5 × 10-4 |
Notes. The parameters are: the minimum (γmin), break (γp) and maximum (γmax) Lorentz factor and the low energy (n1) and the high energy (n2) slope of the smoothed power law electron energy distribution, the magnetic field B, the normalization of the electron distribution, K, the radius of the emission region, R, the Doppler factor δ and the corresponding bulk Lorentz factor Γ. Doppler factors are calculated assuming that the observer lies at an angle θv = 0.7° from the jet axis. The last three columns report the power carried by (cold) protons (assuming one proton per emitting electron), relativistic electrons and magnetic field in units of 1045 erg s-1.
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