The spatial distribution of the H+[
] emission is displayed in Fig. 1
together with the slit positions of the long-slit spectra. Most of the
emission originates from knots in the spiral arm regions. These knots are
the typical signatures of the presence of
regions. The emission is also
found to originate close to the dust lanes. The complex dust lane structures in
the area of the bulge and bar are evident in the continuum image of NGC 6221
(Fig. 2). We estimate a bar projected radius of about 20''-25'' in agreement
with Elmegreen & Elmegreen (1985).
![]() |
Figure 2: Stellar continuum image of NGC 6221. The image orientation and scale are the same as in Fig. 1 |
From the isophotal analysis of the continuum image and the two DENIS images
in the bands I and J, the position of the bar was determined.
The maximum in ellipticity and the plateau of the position angle profile
around (Fig. 3) were used as indicators of the bar component.
This position angle value is also consistent with the orientation of the
dust lanes in Fig. 2. P&B derive for NGC 6221 a position angle for the
line-of-nodes of
. They also stated that the major axis
of the bar is exactly perpendicular to the line-of-nodes. We believe they
confused the position angles of the major axis of galaxy with that of the bar
as can be seen by Fig. 2 in this paper and by Plates 2 and 3 in their
paper and from our velocity field.
The uncalibrated surface brightness profile of the bar shows an exponential
decrease, although heavily influenced by the presence of dust lanes.
![]() |
Figure 4:
[N II](![]() ![]() ![]() ![]() ![]() ![]() ![]() |
The measured ionized gas and stellar kinematics of the galaxy NGC 6221 are presented for the observed position angles in Figs. 5-9.
In all the spectra we found an offset of 4''-5'' between the stellar
kinematical centre (obtained from the position of the maximum intensity of
continuum) and the gaseous kinematical centre (estimated from the maximum
emission of the H and [
] lines).
The position of the gaseous kinematical centre coincides with that estimated
by P&B. For the systemic velocity we measured
while P&B obtained a slightly larger value of
. If we use the
emission lines data as reference for the centre, we find for all intermediate
position angles that the folded velocity and velocity dispersion curves of
ionized gas and stars present strong asymmetries. On the other hand, using
the absorption lines data as reference for the centre the asymmetries of
the folded kinematical profiles are minimized. In the following the absorption
line data are therefore used to give the true centre for both ionized gas
and stars.
In order to bring out the asymmetries in the gas velocity curves we compare
them with the empirically derived curve of circular velocity projected onto
the different position angles. We adopted the equation of the rotation curve
of a galaxy represented as a sequence of flattened spheroids of
Brandt (1960)
as applied by Bettoni & Galletta (1997) for their sample of barred galaxies.
The parameters of the curve were found by the best fit to the major axis NE
side of ionized gas rotation curve (which has the more regular pattern)
assuming a galaxy inclination of (RC3). The resulting curve has
been folded for the major axis SW side. Then it has been projected onto the
remaining the position angles assuming that the mean motions were symmetric
with respect to the galaxy rotation axis. These projected curves
(see Figs. 5-9) allow us to estimate when ionized gas and stars deviate from
circular motions.
The kinematics of the ionized gas and stars measured along the NGC 6221 optical major axis is shown in Fig. 5.
The ionized gas kinematics extends to about 80'' ( kpc) on the
receding NE side and to about 55'' (
kpc) on the approaching SW side.
We found that our gas rotational velocity data agrees within the errors with
the measurements obtained by P&B along
their spectrum G
and deprojected to our position angle.
We obtain more detailed measurements in the central region where the velocity
gradient is strong (
350
for
).
The velocity dispersion of the gas shows within the bulge a peaked trend for
|r|<5 with a maximum value of about 130
. In the outer region dominated
by the disk component the velocity dispersion is found to be constant at a
value of about 50
. Similar peaked velocity dispersion profiles are also
found in bulges of elliptical
(e.g. Zeilinger et al. 1996) and lenticular
galaxies (e.g. Bertola et al. 1995). For 15''<|r|<25'' the gas velocity
curve is very asymmetric as shown by the comparison with the empirical
circular velocity curve. In this radial range the gas velocity along the
receding side is about 20
lower than the circular velocity. It is about
60
higher along the approaching side. An abrupt change in the slope of
the gas velocity curve and a local maximum in the gas velocity dispersion is
also observed at about 17''. No emission is detected for 25''<r<50''.
The stellar kinematics data extend from about 35'' ( kpc) on the
NE side to near the centre of the galaxy. The velocities of the stars follow
closely the trend of the velocities of the gas. The stellar velocity
dispersion profile is peaked with a central value of about 200
. At larger
radii it drops off to a value of about 70
along the NE side. For the
SW side it was not possible to measure the stellar kinematics due to the
poor S/N ratio of the absorption lines.
The stellar kinematics of the bulge is found to be consistent with a hot
stellar system ( at
). The fact that
the velocity dispersion of the gaseous component is of the same order as
that of the stellar one indicates a significant contribution of random motions
to the dynamical support of the gas as dicussed by
Bertola et al. (1995) for
a sample of S0 galaxies.
The kinematics of ionized gas and stars measured along the NGC 6221
is shown in Fig. 6.
The gas kinematics is observed to about 70'' (
The stellar velocity curve is close to the gaseous one. Except for
-10''<r<-3'' the stellar velocity dispersion remains higher than the
gaseous one of about 20 . The stellar data are as extended as the gas
data in the NE side and limited to about 35'' (
kpc). The SW side
is characterized by regions without emission lines and with low S/N
absoption lines. This produces the large errors in the measurement of the
velocity of the gas and makes impossible to determine the stellar kinematics.
The kinematics of ionized gas and stars measured along the NGC 6221 optical minor axis are shown in Fig. 7.
The gas kinematics is measured to about 65'' (
In spite of the fact that the minor axis differs by about from
the bar position angle, the virtual absence of
projected circular motions at this angle
makes it possible to study in great detail how the bar affects the dynamics
of gas and stars. The non-circular motions have an observed maximum amplitude
of about 100
, which is found to be in agreement with the rather general
predictions by
Roberts et al. (1979), who estimate velocities in the
range of 50
to 150
for bar-induced radial components of gas
flow.
From the analysis of Fig. 2 a projected radial extent of 20''-25''
is estimated for the bar component, and this is found to
be in agreement with the kinematical data. The gaseous velocity dispersion
profile in the region of the bar is found to be constant with a value of
about 70
distinctly different from the two preceding
position angles (i.e. at
and
) where
the profile was peaked at the centre. Outside the bar region the gas
velocity dispersion is lower than 50
.
From the above, we can explain the "wavy pattern" in the gas velocity curve
along the minor axis as follows. For the central |r|<6'' the velocity of
the gas shows a negative gradient because it follows the x1 family orbits,
a little further out the gradient is inverted on both sides of the velocity
curve. This can be explained if we consider that beyond the position of the
outer ILR (located at a deprojected radius ) the gas follows the
x2 family orbits out to the corotation radius (at a deprojected radius
). Outside the corotation the bar influence declines and the
velocity of the gas tends to the systemic velocity, at least on the NW side.
The star kinematics is measured up to a distance of about 45'' ( kpc)
in the NW side and up to about 7'' (
kpc) in the SE side.
The velocity curve for the stars agrees within the error limits with the
circular velocity. At this angle the velocity dispersion appears significantly
higher for the stars than for the gas. The stellar velocity dispersion is
higher than 90
at all radii peaking to about 150
in the
centre.
For the SE side (r>10'') of the spectra it was not possible to obtain
measurements of the stellar kinematics.
The kinematics of ionized gas and stars measured along the NGC 6221
are shown in Fig. 8. From the photometrical data we deduced
that this is the position angle of the major axis of NGC 6221 bar.
The gas kinematics extends to about 55'' (
The stellar kinematics is observed to about 50'' ( kpc) on the NW
side and to about 40'' (
kpc) on the SE side. The stars rotate more
slowly than gas with a higher velocity dispersion at all radii. This has a
central maximum of about 160
, and remains
higher than 80
at larger
radii.
The kinematics of ionized gas and stars measured along the NGC 6221
are shown in Fig. 9.
The gas kinematics is measured up to 80'' (
The stellar kinematics is observed to about 50'' ( kpc) on either
side of the centre. The stars rotate with similar velocity to the gaseous
component. They also show the same velocity dispersion profile as the gas.
The S/N ratio for the absorption lines is very low for the SE side where
the stellar kinematics is measured only at about 50'' from the centre.
With the empirical curve of the circular velocity V(R) derived in the
Sect. 3.3 we are able to calculate the angular velocity
and the epicyclic frequency
where R is
the distance from the centre deprojected on the galaxy plane.
In Fig. 10 the curves
,
and
are plotted
in the inner 70'' (
kpc) from the centre.
If we assume the observed ring of ionized gas to be at the outer ILR
we derive the pattern speed of the bar from the condition
.We have
(
kpc) and we find for the bar of NGC 6221
that
kpc-1 taking in account all the uncertainties.
For this value of
there is another intersection with the curve
giving the location of the inner ILR.
The radius of the inner ILR is small (
kpc),
and its precise location is uncertain as it is comparable to the seeing
resolution of our observation.
Corotation is located at the radius where the bar pattern
speed and the angular velocity are equal,
i.e.
.We find that the corotation radius is at a distance
(
kpc) from the centre. This is consistent with Fig. 2 where the bar
seems to finish between 20'' and 25'' corresponding to about 28''-35''
if deprojected onto the galaxy plane.
No outer Lindblad resonance (OLR) is found in the radial range of the observe
gas kinematics
because the condition is not satisfied for any
value of the radius R.
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