, J. Braine 
, M. Krause , R. Zylka ,
R. Wielebinski , and M. Guélin 
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69,
D-53121 Bonn, Germany
Observatoire de Bordeaux, URA 352, CNRS/INSU, B.P. 89,
F-33270 Floirac, France Institut de Radio Astronomie Millimétrique,
300 Rue de la Piscine, F-38406 Saint Martin d'Hères, France 
molecule and radio
continuum emission at 
.
The distribution of the molecular gas (as traced by CO) shows a maximum
in the central region and a ring or spiral arm at 
.
Further analysis of the major axis distribution reveals evidence for an
inner ring-like structure at 
.
The kinematics can be described by rigid rotation in the inner part,
a turnover at 
, and differential rotation with a
velocity of 230 km/s in the outer disk.
The observed continuum emission is mainly due to thermal radiation of
cold dust with an average temperature of 
,
with a small gradient from 20 K to 16 K from the center to the outer
disk. This cold dust component is necessary to explain our results.
The dust emission closely follows the molecular gas in the central
region, but is also detected at large radii where no CO can be seen
(Fig. 5).
In these regions the dust absorption cross section per H atom at
is estimated to be
,
a value similar to that in the outer parts of other galaxies.
From the emission we estimated a molecular mass
of NGC 5907 of 
, about 
smaller
than from the CO emission. By combining the CO and continuum data we
found that the CO-H 
-conversion ratio increases with galactocentric
radius, from 
at the centre to
at
.
Accepted for publication in A&A
Figure: Contour map of the continuum emission of NGC 5907 at
245 GHz, overlaid onto an optical image extracted from the Digitized Sky
Survey. The beam size of 15'' is indicated by the filled white circle in
the lower right corner. The rms noise depends on the location in the map;
on the galaxy it is about 1.5 mJy/beam area, contour levels are
4, 8, ..., 24 mJy/beam area