The plots of Fig. 6 show the kinematic and line
index profiles of the 35 Coma galaxies. The line of sight mean
velocity v(r), line of sight velocity dispersion ,
third
(H3(r)) and fourth (H4(r)) order coefficient of the Gauss-Hermite
decomposition of the line of sight velocity distributions are given,
as well as the profiles of the line indices Mgb,
,
[MgFe] and H
as a function of the radial distance r.
All profiles are folded with respect to the galaxy center (v and H3are folded antisymetrically).
The radial profiles of the Mg2 index are only shown for data from
run 3 and 6 (CA). No reasonable Mg2 profiles could be
derived from the McDonald (run 2 and 5) and MDM (run 1 and 4)
data since these spectra were strongly
distorted by the varying focus of the spectrograph and no satisfactory
correction could be applied. For the 11 galaxies observed at MDM the
additionally derived NaD line index profiles are also show in
Fig. 6. The shown H
indices are not corrected for
emission as suggested by G93 (see Sect. 4). The numerical
values of these radial profiles are also listed in
Tables 13 to 82 in Appendix B.
Different radial binnings for kinematic parameters and line indices occur for two reasons: On the one hand we used different wavelength range for the kinematic and the absorption index analysis. Hence a variation in the radial dependent S/N and consequently a different radial binning could occur. Additionally, for some galaxies the radial profile was focus corrected before deriving line indices. This also influences the radial S/N and hence the radial binning for the line index profiles.
For all 27 galaxies of the inner sample Jørgensen (1999, J99) lists
aperture corrected, central
and Mg2
values
from her own observations and the literature inside a standard
aperture of diameter of
.
For 26 of this galaxies she also gives equivalent central
H
indices as well as equivalent central Mgb and <Fe> indices for
20 of them.
Following Jørgensen et al. (1995b, JFK95b), we converted the
aperture radius
in the "slit-equivalent'' radius
using the formula
,
where b is the slit
width. With the given slit width in Table 3
is 1.2'', 1.7'' and 2.5'' for the CA, McD and MDM setup, respectively.
Overplotted in Fig. 6 we show these aperture corrected
mean values from J99 at the "slit-equivalent'' radii
.
No central values are available for the 8 galaxies of the outer sample.
In Sect. 6
we will discuss the comparison of our data
with those available in literature in details.
Comments on the radial profiles of some galaxies
are given in the following. Examples of the used classes of the H
emission strength are given in Fig. 5.
![]() |
Figure 6:
a) Radial profiles of the kinematical parameters
along the major axis (folded). From bottom to top:
line of sight mean velocity v(r), line of sight velocity dispersion
![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
Comments on single galaxies:
(1) cD Galaxy GMP 3329 (NGC 4874):
Weak, asymmetric NI emission contaminates the
Mgb index at r 5'' - 8''. Weak H
emission
contaminates the H
absorption index at r
8'' - 12''.
The mean H
index from J99 is significantly lower compared to our
profile.
(2) D Galaxy GMP 2921 (NGC 4889) Weak H
emission
contaminates the H
absorption index in the center and at r
8''. The Mgb peak at r
4'' is real as well as the differences of
the
Fe
index at different sides of the galaxy. There is no
evidence for further emission or systematic errors in the continuum shape.
(3) cD Galaxy GMP 4928 (NGC 4839) (SW):
A foreground object existing between +16''and +22'' has been excluded from the analysis. Weak H
emission contaminates the H
absorption index at radii > 25''.
(4) GMP 4822: Weak H
emission contaminates the
H
absorption index at radii > 6''.
(6) GMP 2390: This galaxy hosts a kinematically decoupled,
co-rotating core (see MSBW98).
Weak, asymmetric NI emission contaminates
the Mgb index inside 3''. Slight H
emission contaminates the
H
absorption index at radii > 10''.
(7) GMP 2795: Weak H
emission contaminates the
H
absorption index at 2'' - 4''.
The mean
from J99 is significantly lower compared to our
profile.
(8) GMP 3792: The inner "bump'' of the
Fe
index is caused by the varying focus of the spectrograph
and could
not be corrected sufficiently.
(9) GMP 2629: The mean H
index from J99 is
significantly higher compared to our profile, while
is significantly
lower.
(11) GMP 2000: Weak H
emission contaminates the
H
absorption index at 3'' - 6''.
(12) GMP 2413: Weak, asymmetric NI emission
contaminates the Mgb index at 1''. The inner "bump'' of the
Fe
index is caused by the varying focus of the spectrograph
and could not be corrected sufficiently.
(15) GMP 2417: The mean H
index from J99 is
significantly higher compared to our profile.
(18) GMP 4315: This galaxy shows strong and asymmetric
H
emission, which is demonstrated in Fig. 5a.
Since no OIII emission is detected at all, these data clearly demonstrate that
it is not possible to correct for H
emission via OIII by applying
the method suggested by G93.
(19) GMP 3073: The mean H
and
Fe
indices
from J99 are
significantly higher compared to our profiles.
(20) GMP 1853: The mean
and
Fe
indices
from J99 are
significantly higher compared to our profiles.
(21) GMP 3201: Weak H
emission contaminates the
H
absorption index at radii > 3.5''.
(22) GMP 3661: The Fe
index profiles
could not be corrected perfectly for the focus variation of the spectrograph.
(23) GMP 4679: The asymmetry in the Fe
index is real. There is no
evidence for emission or systematic errors in the continuum shape.
(24) GMP 3352: The Mgb and Fe
index
profiles could not perfectly be corrected for the focus variation of the
spectrograph.The mean H
index from J99 is significantly lower
compared to our profile.
(25) GMP 2535: Weak H
emission contaminates the
H
absorption index at radii > 4''.
(26) GMP 3958: The mean H
index
from J99 is
significantly higher compared to our profiles.
(27) GMP 2776: The mean Fe
index
from J99 is
significantly higher compared to our profiles.
(34) GMP 5568: This galaxy hosts a kinematically decoupled,
counter-rotating core (see MSBW98).
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