Astron. Astrophys. 358, 104-112 (2000)

Footnotes

1. At the particular angle , one obtains .

2. If so the inferred Lorentz factors, relative to our sample, are (3) for HBL (5) for LBL, in the case of p=2 (p=3)

3. These models, in fact, satisfy time variability constraints, assume continuous injection of particles, radiative and adiabatic cooling, - collisions and pair production. The continuous curves shown in Fig. 5 are then not only interpolating curves, but physically possible fits to the data.

4. The three SED correspond to different bins of radio luminosity (at 5 GHz) - which appears correlated with the bolometric luminosity and the position of the peak frequency (Fossati et al. 1998, Ghisellini et al. 1998).

5. Note that again the two trails differ because of the different SEDs: for Mkn 421 the peak of the synchrotron component is between the optical and the X-ray bands and therefore the effect of debeaming is, initially (i.e. for increasing ) to steepen both and ; when the Compton peak enters the X-ray band, flattens. Instead, for PKS 0735+178 the synchrotron peaks between the radio and the optical, and the 1 keV flux is due to Compton and, for the range of angles of sight considered here, the change in the spectral indices turns out to be monotonous.

© European Southern Observatory (ESO) 2000

Online publication: June 26, 2000
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