 
Astron. Astrophys. 334, 427438 (1998)
Appendix A
Table A1. Fluxies of 3C 275.1 at different frequencies  references
Appendix B
We derive the expressions for the velocity components and
deflection angles for two above discussed cases:
i) the magnetic field is parallel to flow velocities in both upstream
and downstream flows
From the boundary conditions, we obtain the following relations for
the velocity components:
Here:
; and
. Putting and
as the ratios of gas and of magnetic field
pressures respectively, we derive:
. The Lorentz factors are described by:
. Since the normal
components of upstream and downstream velocities are related to
Lorentz factors by: . Applying the Lorentz
transformation to above expressions and putting
and , one has after the
calculations:
Here
is the Lorentz factor corresponding to the y 
component of velocity. The above expressions reduce to those ones
given by Bicknell (1994: see also Landau and Lifshitz, 1987) for
. Putting the above expressions for
and , one has:
The above relations can be Lorentz transformed
to the observer's frame. For an example:
,
where and refer to the
shock; subscripts "fl,obs" and "fl,sh" refer to fluid with respect to
observer and fluid with respect to shock respectively. Accordingly,
the velocity components of the gas in the observer's frame for the
ultrarelativistic equation of state, i.e. and
, are given by:
ii) the magnetic field of the upstream flow is
parallel to the velocity flow, while that of downstream flow is
perpendicular
We derive from the above given jump (shock) conditions the expressions
for the normal components of upstream and downstream flow velocities,
as follows: ; ;
; where: and
. Accordingly, one has:
. Here:
and the compression ratio of shock for gas is given by:
. Due to interaction of the magnetic field and
of plasma flow there are the different Lorentz factors for normal
components of velocities , i.e.
, and for those of magnetic field, namely
. The laboratory and rest frame variables are
related via the Lorentz transformation of mass density
, of momentum density
and of energy density . Moreover, the angle
between the jet direction and the observer
(the line of sight), discussed in the beginning of this section, is
related to the angle between normal to the shock surface and the line
of sight and to the angle between observer and
the shock surface by: .
Applying the Lorentz transformation to above solutions, we derive for
the ultrarelativistic equation of state the expressions:
;
. Here: ;
, and
. Thereafter, the relation between the angles
of the pre and postshock velocities to the shock normal is described
by: .
Appendix C
We suppose that the radio structure of 3C 275.1 is already
disturbed at the parsec scale, since there are knots of forbidden line
emission from OII and OIII ions in the nucleus of the host galaxy.
Hence, we made high resolution observation of the core of 3C 275.1.
The VLBI Mk III observation was made in November 16, 1994 at frequency
1.6 GHz with 6 EVN stations: Effelsberg, Jodrell Bank, Medicina,
Noto, Onsala and Westerbork. There were significant interferences from
GLONASS in this session, and in addition due to some technical
problems, almost whole information from baselines with WSRT
station was lost. Using the closure phase method (Jennison 1958,
Rogstad 1968, Rogers et al. 1974) and CLEAN algorithm in AIPS package
(Högbom 1974) to deconvolve the data, we obtained the "clean" map
of 3C 275.1 (Fig. C2). There are not significant features at
distances above 40 mas from the core (the centre of the map).
Probably, the information about it was lost by reason of a very poor
uv coverage of the data. The frequency 1.6 GHz was too low and
the baselines too short to resolve the core of the quasar.
Fig. C2 shows an elongation of the radio structure at a distance
3040 mas from the core with position
angle about . It may be the result of
interaction between outflowing plasma of the QSO and the nonuniform
ionized gas strongly emitting in forbidden [OII] and [OIII] lines. The
contour levels of the elongation are only about 0.51% of the peak. We
suggest, that further studies of the milliarcsecond structure of 3C
275.1 leading to resolving the core of the quasar and to confirming
the elongation of its radio structure are needed.

Fig. C1. The phase vs. time for the uv data used to obtain the "clean" map in Fig. C2. The solid line indicates the model visibilities from the phasereference map (Fig. C2).


Fig. C2. The "clean" EVN map of 3C 275.1 at frequency 1.6 GHz. The peak of the map is 212.9 mJy/beam. The beam is: mas, P.A. .49 . The contour levels are: dashed: 1.5, 0.5; solid: 0.5, 1, 2, 5, 15, 25, 50, 75 % of the peak.

© European Southern Observatory (ESO) 1998
Online publication: May 15, 1998
helpdesk.link@springer.de 