Most of the detected sources were mapped in the ammonia lines.
In Fig. 1 (click here)
we present the grey-scale maps of the (1, 1)
emission. The
positions of the
masers
(taken mainly from Palagi et al. 1993),
IRAS point sources as well as near-IR
sources from the CIO catalogue (Gezari et al. 1993) are
indicated. We plot the following maps for
most detected sources: maps of
(1, 1) line
intensity integrated over
the main group of the hfs components and (1, 1) maps for the blue- and red-side
velocity intervals which represent 1/3 of the total velocity range each.
Thus, these maps give an
impression of the source kinematics.
To determine the total velocity range a composite spectrum was constructed
for each source by overlaying all the measured (1, 1) spectra in one plot.
Then, by visual inspection of this composite spectrum the velocity range
was determined as the interval where a noticeable emission in the main
group was present
above the
level (corresponding to
). For several
sources CS J=2-1 maps from Paper II are overlayed on the ammonia maps.
In Table 2 (click here) we present peak values of the
(1, 1)
integrated line intensites and locations of the peaks as given by the
GAG routines. In Cols. (5) and (6) of Table 2 (click here) the
lower and upper boundaries of the velocity ranges used for integrating
the line intensities (
and
) are indicated.
The (1, 1) and (2, 2) line parameters at the grid positions
closest to the peaks of the ammonia emission are presented in
Table 3 (click here). The typical rms noise was
on the
scale.
The non-detected sources are listed in Table 4 (click here).
In addition, in Tables 5-14 we give some results describing the structure
of the sources: velocities and line widths for the (1, 1) lines at the
observed positions (obtained from the fitting procedure) as well as
estimates of the column densities and kinetic temperatures.
The latter are presented only for those positions where reliable estimates
of the optical depth in the (1, 1) line could be obtained.
This source shows a very unusual HCN emission spectrum in
which the main component (F=2-1) is practically absent (Zinchenko
et al. 1993). Zinchenko et al. suggested that this effect can be
caused by a foreground absorbing cloud with a velocity blue-shifted
by relative to the HCN emitting core. In our
(1, 1) spectra (Fig. 2 (click here)) a weak additional component
can be seen.
Source | ![]() | ![]() | ![]() | ![]() | ![]() |
(![]() | (![]() | (Kkms![]() | (kms![]() | (kms![]() | |
S 76 E | 0 | 0 | 12.9 | 29.4 | 35.1 |
S 86 | 0 | -40 | 5.3 | 26.0 | 30.0 |
S 87 | 10 | 40 | 7.6 | 20.0 | 27.0 |
S 88 B | 50 | 40 | 1.2 | 20.0 | 24.0 |
S 145 | 0 | 0 | 1.6 | -11.3 | -7.5 |
S 199 | 10 | 10 | 2.2 | -39.5 | -36.5 |
S 231 | 10 | 30 | 7.0 | -19.5 | -13.5 |
S 255 | 0 | 80 | 4.7 | 4.8 | 10.8 |
RNO 1B | 0 | 0 | 9.6 | -19.6 | -15.1 |
BFS 48 | 0 | 0 | 5.9 | -11.5 | -7.0 |
|
In Fig. 3 (click here) we plot the average (1, 1) spectrum
in this source and the
residual
(1, 1)
spectrum obtained
by subtracting the single gaussian
pattern fit from the
average spectrum. It clearly shows a weak
line with a central
velocity of
and a width of
. This detection
strongly supports the hypothesis of the foreground cloud mentioned
above. There is no sign of this feature in the
(2, 2) spectra,
which implies an upper limit on the kinetic temperature of
.
The inspection of our data shows that the intensity of this component
grows from our central position towards the south-west. However,
the fact that this component is especially pronounced in the average
spectrum indicates that its spatial extension is not much less than the
size of the mapped region.
Figure 2: The (1, 1) and (2, 2) lines measured at the central
position in S 76 E
Figure 3: The average (1, 1) spectrum in S 76 E and the residual
spectrum obtained by subtraction of the single
gaussian pattern
from the average spectrum
| (1, 1) | (2, 2) | |||||||||
Source | ![]() | ![]() | ![]() | ![]() | ![]() | ![]() | ![]() | ![]() | ![]() | ![]() | |
(![]() | (![]() | (K) | (kms![]() | (kms![]() | (K) | (kms![]() | (kms![]() | (K) | |||
S 76 E | 0 | 0 | 3.96(07) | 32.04(01) | 2.70(0.03) | 0.83(0.05) | 2.63(22) | 32.09(02) | 2.91(0.09) | 27.2(1.3) | |
S 86 | 0 | -40 | 2.65(21) | 28.01(02) | 1.48(0.07) | 1.46(0.27) | 1.87(44) | 28.06(05) | 1.62(0.17) | 26.0(3.5) | |
S 87 | 0 | 40 | 2.93(16) | 23.65(02) | 1.48(0.05) | 1.45(0.19) | 1.96(07) | 23.65(30) | 1.61(1.03) | 25.0(3.0) | |
0 | 40 | 1.31(16) | 21.14(02) | 0.81(0.11) | 2.15(0.73) | 0.72(07) | 21.25(30) | 0.89(1.03) | 18.8(3.5) | ||
S 88 B | 40 | 40 | 0.45(14) | 21.58(16) | 2.50(0.39) | 0.38(06) | 21.43(21) | 2.28(0.45) | 38(10) | ||
S 145 | 0 | 0 | 1.08(09) | -9.77(04) | 1.22(0.13) | 0.45(08) | -9.96(13) | 1.71(0.39) | 22(04) | ||
S 199 | 0 | 0 | 1.23(12) | -38.17(03) | 1.48(0.09) | 0.66(0.28) | 0.81(07) | -38.19(05) | 1.55(0.15) | 27.9(2.1) | |
S 201 | 40 | 0 | 0.76(13) | -37.74(09) | 1.16(0.23) | 0.41(11) | -37.91(25) | 2.32(0.73) | 54(27) | ||
S 231 | 30 | 35 | 2.43(10) | -16.37(02) | 2.16(0.06) | 0.97(0.13) | 1.61(22) | -16.24(03) | 1.90(0.11) | 26.5(2.1) | |
S 255 | 0 | 80 | 1.64(11) | 8.65(03) | 2.41(0.09) | 0.85(0.19) | 0.90(04) | 8.69(05) | 2.61(0.15) | 23.0(1.0) | |
40 | -40 | 1.34(14) | 6.55(04) | 1.83(0.11) | 0.54(0.28) | 0.75(06) | 6.60(08) | 1.91(0.21) | 24.7(2.5) | ||
RNO 1 B | 0 | 0 | 3.85(16) | -17.65(02) | 2.09(0.05) | 0.98(0.13) | 1.93(46) | -17.74(04) | 2.21(0.18) | 21.1(2.3) | |
BFS 48 | 0 | 0 | 2.53(17) | -9.36(03) | 1.85(0.07) | 1.35(0.23) | 1.16(32) | -9.36(08) | 1.99(0.21) | 18.7(2.2) | |
|
Source | ![]() |
(K) | |
S 74 | 0.16 |
S 90 | 0.16 |
S 93 | 0.17 |
S 100 | 0.23 |
S 146 | 0.20 |
S 161 B | 0.20 |
|
It is worth noting that S 76 E is the strongest source of ammonia emission in our sample. The maps in different velocity intervals reveal a slight velocity gradient approximately in the north-south direction.
Our data clearly show the presence of two kinematically distinct
components which overlap partly spatially
(Figs. 1 (click here), 4 (click here)).
Similar structure has
been seen in some other lines (e.g. Barsony 1989) including
(Stutzki et al. 1984). However, to our knowledge
the source has not been mapped in the ammonia lines yet. A submillimeter
continuum map at
(Jenness et al. 1995) shows a
morphology which is very similar to our ammonia map.
Figure 4: The (1, 1) and (2, 2) lines measured at the
position (0,40
) in S 87
This cloud was subject to detailed investigations in various molecular lines including the ammonia lines by Estalella et al. (1993) and Yang et al. (1991, 1995). Our ammonia data are very similar to the results obtained by Estalella et al. and we present them here just for the sake of the homogeneity for statistical analysis.
In Table 3 (click here) we present the values of
the kinetic temperatures at the grid positions closest to the peaks of
the ammonia emission. We estimate the uncertainties of these values in
in most cases. The exceptions are
S 88 B, S 145 and S 201 where the lines are too weak.
For them we give kinetic temperatures derived in the optically thin
approximation from the ratio of the (2, 2) and (1, 1) line areas
(Harju et al.
1993).
The sizes, masses, mean densities, average line widths and virial masses determined in the way described in Sect. 2.3 (click here) are presented in Table 15 (click here).
Source | L | ![]() | M | ![]() | ![]() |
(pc) | (cm![]() | (![]() | (kms![]() | (![]() | |
S 76E | 0.91 | 4.26 | 700 | 2.63 | 660 |
S 86 | 0.64 | 4.12 | 180 | 1.52 | 160 |
S 87 | 0.94 | 4.08 | 530 | 3.30 | 1080 |
S 88 B | 1.10 | 3.02 | 74 | 2.42 | 680 |
S 145 | 0.40 | 3.63 | 14 | 1.22 | 62 |
S 199 | 1.28 | 3.31 | 230 | 1.36 | 250 |
S 231 | 1.24 | 3.84 | 690 | 1.96 | 500 |
S 255 | 1.43 | 3.60 | 600 | 3.00 | 1350 |
RNO1B | 0.48 | 4.42 | 150 | 1.65 | 140 |
BFS 48 | 0.75 | 4.10 | 270 | 1.85 | 270 |
|
The comparison with the CS J=2-1 results from Paper II for S 76 E, S 199
and S 255 shows that the ammonia lines are narrower
than the CS lines. The source sizes are
times smaller in
ammonia. The core masses are correspondingly smaller. But the mean
densities are similar. This is similar to the results of such comparison
for other clouds in Paper II.