A&A 405, 969-973 (2003)
DOI: 10.1051/0004-6361:20030733
G. Gentile 1 - F. Fraternali 2,3 - U. Klein 1 - P. Salucci 4
1 - Radioastronomisches Institut der Universität Bonn,
Auf dem Hügel 71, 53121, Bonn, Germany
2 - ASTRON, PO Box 2, 7990 AA Dwingeloo, The Netherlands
3 - Kapteyn Astronomical Institute, Postbus 800, 9700 AV, Groningen, The Netherlands
4 - SISSA, via Beirut 4, 34013, Trieste, Italy
Received 10 March 2003 / Accepted 6 May 2003
Abstract
We present 3-D modelling of the distribution and kinematics of
the neutral hydrogen in the spiral galaxy ESO 123-G23. The optical appearance
of this galaxy is an almost perfectly edge-on disk, while the neutral hydrogen is found
to extend vertically out to about 15 kpc on either side of the galactic plane.
The H I layer and the major features of the H I data cube
can be successfully explained by a model dominated by a strong
(about 30)
line-of-sight warp. Other
models were tried, including a flare model and a two-component model, but they clearly
do not reproduce the data.
This is the
first unambiguous detection of a galactic warp that has the maximum deviation from the
central plane almost along the line-of-sight.
No evidence for the presence of any
companion galaxy is found in the H I data cube.
Line-of-sight warps in edge-on galaxies are probably
frequent, but escape detection as they are too weak. Moreover they may
easily be mistaken as flares or "thick disks''. A 3-D modelling of the H I
layer as the one presented here is needed in order to distinguish between
these possibilities.
Key words: galaxies: individual: ESO 123-G23 - galaxies: kinematics and dynamics - galaxies: structure
The outer parts of the disks of spiral galaxies are frequently warped (Bosma 1991; García-Ruiz et al. 2002). Warps are best seen with H I observations, since the neutral hydrogen extends out to much larger radii than the optical disk. H I warps obey some general rules, one of them being that they usually start around R25 (Briggs 1990). The measured angle between the inner plane and the outermost observed H I ring spans a wide range of values, from a few degrees to a few tens in some exceptional cases. Of the various possible orientations that warps can have, one is considered as "unfavourable'', as the warp becomes less visible: this is when the largest deviation from the central plane occurs along the line-of-sight.
The origin of warps is still poorly understood. Different models have been proposed, for instance: the precession of a disk embedded in a flattened dark halo, misaligned with the disk itself (e.g. Toomre 1983), or the accretion of gas with angular momentum different from that of the disk (e.g. Ostriker & Binney 1989), but none is completely satisfactory.
In an ongoing project to study the dark matter distribution of spiral galaxies
a sample was culled from the list of Persic and Salucci (1995)
selecting the best determined optical rotation curves; the selection
criteria were: symmetry of the H
rotation curve, high angular extent,
high H I flux and low luminosity (Gentile et al., in prep.)
The aim was to combine these optical data
with H I measurements tracing the gravitational potentials much further out. One
of these galaxies, the edge-on spiral ESO 123-G23, turned out to look remarkable
in its H I distribution. Indeed the H I emission extends
far away (up to about 15 kpc) from either side of the plane.
Such a pattern can be produced by different phenomena including a flaring of the
outer disk, a thick layer of gas or a warp along the line-of-sight.
We have therefore modelled the H I layer of ESO 123-G23 considering these possibilities.
Our analysis shows that the correct explanation is a warping of the disk
along the line-of-sight. The other possibilities are
clearly ruled out.
![]() |
Figure 1:
Optical DSS image (grey scale) overlayed with the H I total
intensity map of the observed data cube (top) and of the line-of-sight warp model
(bottom). Contours are
![]() ![]() ![]() |
ESO 123-G23 is an edge-on spiral galaxy located at a distance of 38 Mpc
(H0=75 km s-1 Mpc -1). Not much was known about this galaxy
except that it exhibits a slight warp in the outer optical
disk (Reshetnikov & Combes 1999).
We have observed ESO 123-G23 in the H I line for
hours
using the Australia Telescope Compact Array
(ATCA)
and combining
the data from two array configurations (750D and 1.5A), providing a beam of 30
6
25
0 and a velocity resolution (after Hanning smoothing) of 6.6 km s-1.
In Fig. 1 (upper panel) we display an optical - H I overlay showing the peculiar
morphology of this galaxy: while the optical image resembles an almost perfectly edge-on disk,
the H I is much more extended perpendicularly to the major axis,
displaying what looks like a very inclined central disk and diffuse emission at
large (up to 15 kpc) projected distances from the optical disk;
this diffuse emission accounts for about 40% of the total H I mass.
The left column of Fig. 2 shows some channel maps of the H I
data cube.
Every fourth channel is shown, so the displayed maps are spaced by about
26 km s-1. The central channel map, at a velocity of 2855.4 km s-1, is the one closer
to the systemic velocity. The channel maps of ESO 123-G23 show the emission from a central edge-on disk,
plus fainter emission from regions above and below the plane.
Such an emission is more visible in the central channels, close to systemic velocity.
This may indicate either a lower rotation velocity
of the gas above the plane or a lower inclination angle (i.e. towards face-on) of
the outer parts of the disk.
A warp in position angle is visible, especially at
v = 2723.5 and
2987.3 km s-1, and it is quite symmetric.
ESO 123-G23 is reported to have no optical companion of
size between
/2 and 2
within a radius of 10
(Karachentsev 1993). An inspection of the H I data cube did
not disclose any companion in H I either.
The total size of the data cube is
(dimensions of the
primary beam)
km s-1. The position-velocity diagram along the
major axis is shown in Fig. 3 (upper panel), where the east side of
the galaxy is slightly more extended but no clear kinematical lopsidedness is visible.
On the p-v diagram is overlapped (dots) the rotation curve of the galaxy (see Sect. 3).
We considered three phenomena that might mimic the observed H I structure and kinematics: a) a line-of-sight warp; b) a large flare in the outer part of the disk; and c) a two-component structure, thin + thick (slowly rotating) disk, similar to that proposed for NGC 891 (Swaters et al. 1997) and NGC 2403 (Fraternali et al. 2001). These phenomena have in common the fact of displaying emission away from the thin disk and are hard to disentangle except via detailed 3D modelling of the H I layer.
The parameters that the models had in common were: the radial surface density distribution,
derived using the Lucy method (Warmels 1988); the H I velocity
dispersion, chosen to go from 12 km s-1 in
the inner parts to 7 km s-1 in the outer parts (Kamphuis 1993),
in order to have values as realistic as possible; a constant value
of 10 km s-1 would not have affected much the results, while values different from 10 km s-1by more than 5 km s-1 would not give a good account of the observed data cube;
the shape of the vertical distribution of the H I layer, chosen to
be Gaussian with different scale-heights for the various models
(the choice of other distribution shapes does not
significantly change the results); the position angle
as a function of radius, taken to slightly change counter-clockwise
after
(
15 kpc), and then to significantly (10
)
change clockwise
further out (see third panel of Fig. 5).
By trying models with different values of the position angle we estimate an accuracy
of about 2
(errorbars in Fig. 5), beyond which the disagreement with
the observations is flagrant.
The rotation curve was derived with the WAMET (WArped Modified Envelope Tracing)
method (Gentile et al. 2002; Vergani et al. 2002),
a modification of the Envelope Tracing
method (Sofue & Rubin 2001); a detailed description of this method will
be given in a forthcoming paper (Gentile et al., in prep.). Only small
corrections (<5 km s-1) were necessary to refine the rotation curve derived with our WAMET method. These corrections were made in order
to give a better representation of the observed H I data cube.
This method, however, like the methods that derive the rotation curve
from the position-velocity diagram, provides the product
.
Therefore we have to account for the inclination, that can vary with radius
within the same model.
For the inner parts of the galaxy we used, in all the models, an inclination
angle of 85
,
a value similar to optical estimates (e.g. the Lyon-Meudon
Extragalactic Database, LEDA, gives an inclination of 82.3
).
In the warp
model the inclination angle was lowered by up to 30
beyond R25 in order to
fit the observations (see second panel in Fig. 5).
With the same procedure we used for the position angle, we estimated an error
for the inclination angle of 5
.
The rotation curve was obtained with the WAMET method with the assumed values for the inclination angle.
The FWHM of the Gaussian vertical distribution of the H I
was chosen to be 300 pc.
The flare model differs from the warp model in having a constant inclination
of 85
and a rotation curve obtained with such a constant value.
The FWHM of the H I vertical distribution is 300 pc inside R25 increasing to a value
of 25 kpc at
.
Such an unrealistic value is necessary to reproduce
the H I distribution (lower contours) visible in the total H I map
(Fig. 1, upper panel).
Finally the two-component model is the sum of a thin and a thick disk in analogy to the
previously cited models proposed for NGC 891 and NGC 2403. In this model the thin disk has a
rotation velocity taken from the WAMET method with a constant inclination and
a thickness of 300 pc (FWHM). For the thick disk (40% of the total H I mass) the rotation
velocity was lowered by 30 km s-1 with respect to the thin disk and the thickness of the
H I layer was taken to be 20 kpc (FWHM).
Similarly to the flare model, this last unrealistic value is necessary to reproduce
the total H I distribution. For both the flare and the two-component model
a different choice of the inclination does not improve the agreement with the
observed data cube.
In Fig. 2 we show some channel maps of the data cube compared with the channel maps of the line-of-sight warp model, the flare model, and the two-component model (from left to right). This figure illustrates why the flare model and the two-component model have to be rejected: apart from their somewhat unphysical choice of parameters (although necessary to produce the vertical H I distribution), they cannot reproduce the observed channel maps. For instance, the flare model cannot reproduce at the same time the large north-south extension in the central channels and the relatively small north-south extension visible in the extreme channels ( v = 2723.5 and 2987.3 km s-1). The two-component model is not able to reproduce the "elbow'' present at v = 2749.9 and 2802.6 km s-1, which is also indicated on the receding side, at v = 2908.2 and 2960.9 km s-1.
The data are indeed fitted best by the model of a warp that shows maximum
deviation from the plane close to the line-of-sight;
Fig. 2 shows that
such a model reproduces in detail all the key features of the observed H I
data cube.
See the upper panel of Fig. 5 for the adopted rotation curve
for this model; the errors are the difference between the approaching and the
receding side, considering also a minimum error of
km s-1.
In the upper panel of Fig. 3 we show the derived rotation curve of ESO 123-G23
(separately for the two sides) projected
onto the observed position-velocity diagram,
and in the lower panel the adopted rotation curve (the average between the two sides) projected onto
the position-velocity diagram of the line-of-sight warp model.
It is remarkable that the de-warped rotation curve of this galaxy is in
good agreement with the Universal Rotation Curve of Persic et al. (1996)
while the raw
curve, instead, had a very unusual decrease of 30 km s-1 from 7 kpc to 15
kpc, never found in galaxies with the maximum circular velocity of ESO 123-G23.
Figure 4 shows the H I rings of the
line-of-sight warp model as seen by the observer
and Fig. 1 (lower panel) shows the total H I map obtained with
this model. The overall H I distribution is well reproduced.
We have also tried combinations of the various models, but the emission at
projected distances of up to 15 kpc from the central disk can be explained only
with the warp model, and combining the warp model with realistic values of
an outer flare and a thick disk gives irrelevant changes to the model.
![]() |
Figure 5:
Parameters adopted for the line-of-sight warp model. From top to bottom, these
are: rotation velocity, inclination and position angles, and the angles ![]() ![]() |
In order to describe the geometry of the warp,
as previously done by Schwarz (1985), we define the angle
between the plane of the inner disk and the plane of the warped ring, and the
angle
between the line of nodes (at the intersection of the plane of
the ring and the plane of the inner disk) and the line of intersection between
the plane of the sky and the plane of the inner disk. The uniqueness of this warp
now shows up in Fig. 5, bottom panel:
is always relatively
close to zero, meaning that the maximum tilt of rings is almost exactly along the
line-of-sight. We point out that a negative value of
means a position angle
varying clockwise and that in unwarped sections of a galaxy
is of course
not defined. The fourth panel from top of Fig. 5 shows the monotonically
increasing warp angle
as a function of radius.
There is, however, an ambiguity due to our assumption of a central inclination
of 85
and the unknown true orientation of the disk: the inclination varies from 85
to about 55
,
which could mean a variation of 30
or 40
,
depending on the viewing angle. If we look at both the central disk and
the outer rings "from above'' or
"from below'', the warp angle is about 30
;
if we look at one "from above'' and the
other "from below'', the warp angle is about 40
.
We plot the warp angles with the assumption of viewing the galaxy in such a way
that the warp is as weak as possible (30
);
considering the uncertainties in position angle and inclination, we estimate
that the minimum warp angle necessary to reproduce the data cube is about 25
.
Even with this
assumption, this warp remains exceptional: the warp angle, measured at the
last point, is very large. In fact it is larger for example than all the warp
angles found in the systematic study of galaxy disks in H I by García-Ruiz et al.
(2002). This is probably the reason why this warp is rendered
visible: for smaller angles a warp oriented along the line-of-sight is
almost invisible.
We have thus found very strong evidence for ESO 123-G23 to be an almost perfectly edge-on disk galaxy with a strong warp along the line-of-sight. This is demonstrated by the comparison of a series of models with the observations. We therefore report the first clear case of a galaxy with such a warp. We note that Becquaert & Combes (1997) interpreted the morphology and kinematics of the H I disk of NGC 891 in terms of a warp close to the line-of-sight. However, the fact that Swaters et al. (1997) interpreted their H I observations of NGC 891 predominantly in terms of a thin + (slowly rotating) thick disk shows that the case was not as evident as the present one. Statistically, the frequency of occurrence of line-of-sight warps should be much higher, while most of them remain undisclosed owing to their small warp angles. The only way to discriminate between different phenomena (warp, flare, etc.) is detailed modelling in the way described here.
Acknowledgements
We thank the referee, Rob Swaters, for valuable comments that improved the quality of this paper. We are grateful to Renzo Sancisi for giving us the first hints for this work. GG wants to thank Christian Brüns and Daniela Vergani for performing the first run of the observations. GG is also grateful for financial support of the Deutsche Forschungsgemeinschaft under number GRK 118 "The Magellanic System, Galaxy Interaction and the Evolution of Dwarf Galaxies''.