The observational results are summarised in Table 2 and the maps are shown in
Figs. 1 to 6, where the intensity scale is
and velocities are shown relative to local standard of rest. Note that although the SEST maps are shown at
their observed spacings, the global integrated intensities (Table 2), like the OSO observations, are calculated for a map spacing of one
beam (as in Table 1).
Galaxy | Teles. | Date(s) | HCN
![]() |
CO
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CO
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|||
Centre | Global | Centre | Global | Centre | Global | |||
NGC 1068 | SEST | 9/00 & 11/00 | ![]() |
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NGC 1365 | SEST | 4/00 | ![]() |
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>300 |
NGC 2273 | OSO | 9/00 | ![]() |
<0.7 | ![]() |
![]() |
- | - |
NGC 4945 | SEST | 12/98 & 6/00 | ![]() |
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NGC 5033 | OSO | 9/00 | ![]() |
![]() |
![]() |
![]() |
- | - |
Circinus | SEST | 6/99, 4/00 & 6-7/00 | ![]() |
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NGC 6814 | SEST | 8/00 |
![]() |
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In Table 3 the luminosities are summmarised. These are
calculated by multiplying the average integrated intensity by the area
of the map (e.g. as in Sandqvist et al. 1995). Since there may be some
ambiguity due to how much area is actually mapped, we constrain
the value by multiplying the global integrated intensity at single beam spacing over the
estimated source size
, which gives a similar result as calculated by the average integrated intensity
over the mapped area.
Galaxy | D |
![]() |
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||||
Beam | Map | Beam | HCN Map | Map | Beam | Map | |||
NGC 1068 | 15 |
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0.91 | ![]() |
2.4 | 0.28 |
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7.4 | |
NGC 1365 | 20 |
![]() |
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6.8 |
NGC 2273 | 25 | ![]() |
<0.07 |
![]() |
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- | - | 0.66 |
NGC 4945 | 4 | ![]() |
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0.91 |
NGC 5033 | 12 |
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- | - | 0.53 |
Circinus | 4 |
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0.03 | ![]() |
0.62 | |
NGC 6814 | 21 |
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0.66 | |
Average | 14 | 0.04 | 0.08 | 0.4 | 0.8 | 1.4 | 0.2 | 1.6 | 2.5 |
Our value of the global CO luminosity (Table 3) is comparable
with that Planesas et al. (1989) who get, also from
single dish observations,
K km s-1 kpc2 over a
partial map spanning
(cf. Fig. 1). Both results are consistent with those
of Young et al. (1995), see Sect. 4.
Concerning HCN, note that
the central integrated intensity is similar to that obtained
previously at Onsala (
K km s-1, Curran et al. 2000), although, due to
the larger SEST beam, the central luminosity is slightly higher
(cf.
K km s-1 kpc2).
Our CO values agree well
with those previously published by Sandqvist et al. (1995);
1.7 103 K km s-1 kpc2 over the central beam and
5.3 103 K km s-1 kpc2 at 20'' spacing over
.
Again the central HCN result agrees well with our previous measurement of
K km s-1 kpc2 (Curran et al. 2000).
We are not aware of any large-scale maps of either CO or HCN in this
galaxy. The central CO value agrees well with that of
K km s-1 kpc2(Curran et al. 2000).
We adopt a distance of 3.7 Mpc (Mauersberger et al. 1996) (although
distance estimates to NGC 4945 vary somewhat, e.g. 6.7 Mpc according
to Dahlem et al. 1993, Forbes & Norris 1998). The choice of value has no effect on the
relative luminosities (i.e. ratios). Note that while the central CO
integrated intensity compares well with that obtained by
Mauersberger et al. (1996) (
450 K km s-1), the global value from
this data is around 3 times greater than actually published by Dahlem et al.(1993) (
K km s-1), Table 2.
The central HCN integrated intensity compares well with that of Curran et al. (2001b)
( K km s-1).
Again we are not aware of any large-scale maps, although both the CO and HCN
luminosities agree with those previously determined,
i.e.
and
K km s-1 kpc2, respectively (Curran et al. 2000).
Note that due to the relatively close proximity and vastness of this galaxy, we may be far from having global CO values and that the "structure'' in our map may be due to some structure within the galaxy, e.g. spiral arms (Thean et al. 1997 and references therein).
The new values agree well with those from the maps of 1988 and 1993
(see Curran et al. 1998), i.e. 0.3 103 K km s-1 kpc2 for both the CO
and
transitions.
Concerning the HCN, the central integrated intensity agrees (within
uncertainties) with that of Curran et al. (2001b), i.e.
K
km s-1. Note that (blue-shifted) HCN may also be detected at
-60'' along the minor axis, which corresponds to the (approaching) NW molecular
outflow (Curran et al. 1999) and where a tentative detection of HCO+ has
been made (see Curran 2000a).
With no large-scale maps available, again the CO luminosity agrees with that previously obtained,
i.e.
K km s-1 kpc2, although due to the weak
emission (a central integrated intensity of
0.5 K km s-1, Curran et al. 2000),
no HCN was detected over the time allocated to map this molecule
.
Copyright ESO 2001