The strongest lines in the optical (observed) spectra of HzRG
are Ly,
CIV
1550, HeII
1640 and CIII]
1909, while
[OII]
3727, [OIII]
5007, 4959, H
dominate
in the NIR. There
are some physical effects
that might make the interpretation of the line profiles and velocity
shifts uncertain.
We mentioned in Sect. 1 that the interaction between the radio jet and the ambient gas could be responsible for the extreme motions in HzRG. Other authors favour a gravitational origin for the kinematics of the gas. One interpretation or another has important consequences: if the velocity fields reflect the gravitational potential, the derived dynamical mass turns out to be correlated with redshift and/or radio power (Baum & McCarthy 2000). As the authors pointed out, this result is not valid if shocks are responsible for the kinematics.
Villar-Martín et al. (1999)
carried out a detailed spectroscopic study of the
intermediate redshift radio galaxy PKS 2250-51 (z=0.31) where a strong
interaction between the radio and optical structures occurs.
The authors resolved two main kinematic components, spatially extended
and detected in all optical (rest frame)
emission lines.
One of the components is
narrow (
km s-1), the line ratios are consistent
with photoionization and it extends beyond the radio
structures. The other component is broad (FWHM as large as 900 km s-1at some spatial positions),
the line ratios are consistent with shock ionization and it is emitted
inside the radio structures. The properties of the
narrow component suggest that it is emitted by
ambient photoionized gas that has not been perturbed, while the properties
of the broad component are consistent with shocked gas.
A similar spectroscopic study could prove or disprove shocks as responsible for the kinematics in HzRG. The studies done so far have been based on the emission line kinematics along the radio axis and they have not provided a definitive answer. We propose that the joint study of the line kinematics (with spectral decomposition of the line profiles) and the line ratios may give the answer. If shocks perturb the kinematics in HzRG, then we should expect similar components and with similar flux ratios as those observed in PKS 2250-41. With 2D spectrographs it will be possible to extend the kinematic studies to regions far from the radio axis, where the interactions are expected to be non existent. The detection of broad lines far from the radio axis would confirm that jet/cloud interactions are not responsible for the extreme motions.
The spectral resolution we use is crucial to be able to
isolate different kinematic components in the extended gas.
A velocity resolution of
km s-1 (
)
would be ideal since it will allow an accurate
decomposition of the emission line profiles. The instrumental profile (IP) is in this
case well matched
with the expected FWHM of the non
perturbed gas (so that we avoid unnecessary instrumental broadening), such
as the diffuse haloes extending beyond the radio
structures. The study of such haloes
can be very useful, since they show the gas properties before any
perturbation.
With the new
NIR arrays it should be possible
to cover the interesting spectral range (HeII
4686 to [OIII]
5007)
for a good number of objects.
The presence of several kinematic components can lead us to derive false rotation curves.
Figure 2 shows two examples of HzRG where the emission lines
show a resemblance with rotation curves (see also Figs. 1 and 2 in Villar-Martín
et al. 1999).
This could be an exciting evidence
for merger events (e.g. Hernquist 1993). However,
the apparent rotation is an artifact, consequence of the
presence of at least two kinematic components. To illustrate this, we
have used the spectrum of the radio galaxy B3 0731+438 (Fig. 1).
We have extracted 1-D
spectra from those spatial pixels where the abrupt jump in the apparent rotation curve
occurs.
Figure 3 shows the Ly
spectral profile at each pixel.
Many HzRG are highly polarized in the optical due to the scattering of nuclear emission (both continuum and emission lines from the broad line region) by (probably) dust in the extended gas (e.g. Cimatti et al. 1997, 1998; Fosbury et al. 1999). The radiation from the extended gas is therefore a mixture of direct and scattered light. Can the scattered broad lines affect our conclusions on the kinematic studies if neglected?
As an example we present
the spectrum of TXS0211-122 (z=2.34), one of
the most highly
polarized (
longward Ly
)
radio galaxies at high redshift.
We have analysed the profile of CIV, which is efficiently
emitted in the broad line region and therefore is subject to scattering.
Figure 5 shows the spectrum in the
region of CIV. There is an underlying broad component with
km s-1. Similar FWHM are often observed in high
redshift quasars suggesting that it is
scattered light.
The fit shows that the CIV line profile is not seriously affected
by the underlying broad component
due to the prominence of the "narrow" emission.
This is usually the case (also for
Ly)
and the studies that have found
km s-1in the extended gas of HzRG are not affected by the effects of scattered light
(McCarthy et al. 1996;
Villar-Martín et al. 1999).
However, we cannot neglect this contribution when studying the line profiles in more detail
(looking for different kinematic components, for instance); we
would interpret
the broad scattered components
as due to extreme motions in the extended gas.
The best way to avoid any possible uncertainty on this issue is
to compare with lines that are not emitted efficiently in the BLR
(and, therefore, they are not scattered), such as HeII1640
(Foltz et al. 1998;
Heckman et al. 1991) or
optical forbidden lines such as [OII] and [OIII]
5007, 4959 (the [OIII]
lines might have a minor contribution from scattered light,
di Serego Alighieri et al. 1997).
Absorption of Ly
photons
can modify dramatically the profile of the line
(van Ojik et al. 1997). Röttgering et al. (1997)
concluded that the effects of associated HI absorption
may be responsible for the shift of the Ly
line with respect
to the high ionization lines in some objects.
By using non resonant lines (HeII
1640, forbidden lines)
we will avoid
this problem. The CIV doublet, although resonant, is less sensitive and more reliable
than Ly
.
The use of high spectral resolution (
Å) can
also help, since we will be able to resolve the absorption troughs
(van Ojik et al. 1997).
The comparison between the FWHM of the emission lines provides information about the processes responsible for the line emission and the kinematics. The detection of different line velocity widths for different lines will lead us to the conclusion that different mechanisms are at work and/or there are regions of different physical conditions. As an example, some radio galaxies with radio/optical interactions show that low ionization lines are broader than high ionization lines (Clark et al. 1998). This has been interpreted as a consequence of shocks: the shocked gas has lower ionization level and more perturbed kinematics than the non perturbed gas.
In this sense, care must be taken
with the doublets (CIV1550, CIII]
1909 and [OII]
3727). At high redshifts
the separation between the two components
is large (7 Å at z=2.5 and 10 Å at z=4) and
the doublet as a whole can show a profile apparently broader
than single lines. This will be the case when the lines are similar in (observed) width or narrower than
the doublet separation. If the lines are much broader the two components will be severely blended,
whatever the resolution we use and the broadening will not be important. This should often be the case
since gas motions can
produce lines of intrinsic
Å at z=2.5.
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