The observations were carried out with the ESO 1.4 m CAT telescope in
June and July 1993, and March 1994. In July, the short camera was used
in the blue arm, with a resolution of 30000, corresponding to 
and the [O III] 5007 Å line was observed. In June 1993 and March
1994 the 
line and neighbouring [N II] 6548, 6583 Å lines
were observed, using a resolution of 60000. For the higher
resolution is partly offset by the larger thermal broadening.
Integration times varied from a few to 30 minutes depending on the
line flux. The faintest nebulae could not be observed because they
were not visible on the finder due to the brightness of the Moon at
both epochs. The slit had a width of 
and a length
of 
. No flux calibration was performed. The
wavelength calibration was done with ThAr spectra, and also checked by
observing well-known planetary nebulae as velocity standards.
The data reduction involved flat fielding, summation of the spectrum
over the slit and wavelength calibration. The velocity scale was
corrected for the Earth's motion to obtain heliocentric
velocities. The radial velocity for the [O III] measurements was
determined from a first-moment analysis over the line profile. For
the measurements of and the [NII] lines (plus in a few cases
the nearby HeII 6560.1 Å line) the central velocity between the two
peaks was used instead. The uncertainty in the velocities is caused
mainly by the method of averaging. The velocity profile is typically
wide at half peak intensity. When it is symmetric, the
central velocity is easy to define, but often one peak is somewhat
stronger than the other or distortions can be caused by a bipolar
outflow in combination with an off-centre slit. A different method to
obtain velocities is to fit the wings of the line: Spyromilio
(1995) finds that this works well, with the wings (defined as
line-to-continuum ration less than 10% of the line peak) being more
symmetric than the central part of the profile. This method cannot be
easily used for our data because one wing is distorted at a low level
due to charge-transfer deficiencies of the CCD. The total uncertainty
in the velocities was derived by comparing with previous
determinations of bright nebulae, for which agreement was found within
. Agreement to within 
is found between the
and [O III] measurements (reduced in different ways) for all 13
objects in common, with a mean (systematic) deviation of
. This indicates that within the adopted uncertainty, the
velocities do not depend on the method of averaging. Higher resolution
will not improve this accuracy, which is dominated by the internal
motions of the nebulae affecting the moment calculation. In most cases
the lines are resolved: detailed analysis of the profiles will be
given in Gesicki et al. (1997).
The results are presented in Table 1 (click here). The numbering convention is the one introduced by Acker et al. (1992) which has superseded the previous Perek & Kohoutek (1967) scheme. Velocities are averaged over all available measurements.
Two objects in Table 1 (click here) (004.8-22.7 and 006.8-19.8) have velocities and positions in agreement with the newly discovered Sagittarius Dwarf galaxy and are probably members of this dwarf spheroidal orbiting our Galaxy (Zijlstra & Walsh 1996) at a distance of 25 kpc. A third object in the same direction (003.8-17.1, HB8) also has a large indicated distance but a much different velocity.
Source | Name |  | Note | Adopted dist. |
( ) | (kpc) | |||
000.7-02.7 | M2-21 | -164.7 | 1 | |
| 000.9-04.8 | M3-23 | -152.9 | 2, 3 | 4.2 |
| 001.5-06.7 | SwSt1 | -16.1 | 1 | 4.7 |
| 001.7-04.6 | H1-56 | -116.3 | 1 | 10.4 |
| 002.0-06.2 | M2-33 | -126.0 | 1 | 8.0 |
| 002.0-13.4 | IC4776 | +16.8 | 1 | 3.5 |
| 002.1-02.2 | M3-20 | +24.1 | 1 | |
| 002.2-02.7 | M2-23 | +186.7 | 2 | 8.5 |
| 002.6+08.1 | H1-11 | +4.8 | 1, 2 | 6.7 |
| 002.6-03.4 | M1-37 | +220.5 | 2 | 8.1 |
| 002.7-04.8 | M1-42 | -86.5 | 2 | 4.5b |
| 003.2-06.2 | M2-36 | +73.0 | 1 | 6.4 |
| 003.7-04.6 | M2-30 | +155.8 | 1 | 7.7 |
| 003.8-17.1 | HB8 | -183.2 | 1 | 16.2 |
| 003.9-02.3 | M1-35 | +67.4 | 1, 2 | 4.3b |
| 004.0-03.0 | M2-29 | -112.0 | 1 | 9.3 |
| 004.2-04.3 | H1-60 | +24.8 | 1 | |
| 004.6+06.0 | H1-24 | +157.9 | 2 | 6.8a |
| 004.8-22.7 | He2-436 | +132.9 | 1 | 25.0 |
| 004.9+04.9 | M1-25 | +14.1 | 1 | 4.8 |
| 005.2+05.6 | M3-12 | +17.1 | 1, 2, 3 | 6.3 |
| 005.8-06.1 | NGC6620 | +69.8 | 1 | 6.1b |
| 006.0-03.6 | M2-31 | +151.7 | 2 | 4.8 |
| 006.1+08.3 | M1-20 | +60.3 | 1, 2 | 5.9 |
| 006.4+02.0 | M1-31 | +68.2 | 2 | 5.3a,b |
| 006.8+04.1 | M3-15 | +97.9 | 1, 2 | 3.9 |
| 006.8-19.8 | Wray16-423 | +133.1 | 1 | 25.0 |
| 008.2+06.8 | He2-260 | +21.5 | 2 | 11.5 |
| 008.3-01.1 | M1-40 | -34.2 | 1 | 2.8 |
| 009.4-09.8 | M3-32 | +58.7 | 1 | |
| 009.6-10.6 | M3-33 | +179.8 | 1 | 8.1 |
| 010.7-06.4 | IC4732 | -147.8 | 1 | 4.8 |
| 014.0-05.5 | V-V3-5 | -45.6 | 1 | |
| 331.3+16.8 | NGC5873 | -133.4 | 1 | 4.0 |
| 334.8-07.4 | SaSt2-12 | -63.0 | 2 | |
| 342.1+27.5 | Me2-1 | +44.4 | 2, 3 | 4.8 |
| 345.0-04.9 | CN1-3 | -80.0 | 1 | |
| 346.3-06.8 | FG-2 | +34.7 | 1 | |
| 347.4+05.8 | H1-2 | -105.0 | 1, 2 | 7.1 |
| 348.0-13.8 | IC4699 | -122.7 | 1 | 5.5 |
| 349.8+04.4 | M2-4 | -207.9 | 1 | 6.7 |
| 350.9+04.4 | H2-1 | -18.5 | 1 | 5.1a |
| 351.1+04.8 | M1-19 | -55.1 | 2 | 6.7 a |
| 351.6-06.2 | H1-37 | -23.2 | 1 | |
| 351.9+09.0 | PC-13 | -75.2 | 1 | |
| 352.1+05.1 | M2-8 | +25.1 | 2 | 6.9 |
| 352.9-07.5 | FG-3 | +0.5 | 1 | |
| 353.3+06.3 | M2-6 | -127.4 | 1, 2 | 8.4a |
| 353.5-04.9 | H1-36 | -118.8 | 1, 2, 3 | |
| 355.1-02.9 | H1-31 | +47.0 | 1 | 11.8 |
| 355.1-06.9 | M3-21 | -66.1 | 1 | 5.3 |
| 355.4-02.4 | M3-14 | -82.3 | 1 | 8.1a |
| 355.7-03.5 | H1-35 | +123.3 | 1, 2 | 5.1a |
| 355.9+03.6 | H1-9 | -157.6 | 2 | 9.4a |
Source | Name | | Note | Adopted distance |
| () | (kpc) | |||
356.2-04.4 | CN2-1 | -169.1 | 1, 2, 3 | 6.9a |
| 356.5-02.3 | M1-27 | -49.7 | 2 | 3.5 |
| 356.9+04.5 | M2-11 | +84.5 | 1 | 7.1a |
| 357.1+03.6 | M3-7 | -189.7 | 1 | |
| 357.2+07.4 | M4-3 | +132.1 | 1, 2 | 8.1 |
| 357.4-03.2 | M2-16 | +89.6 | 2, 3 | 6.9a |
| 357.4-03.5 | M2-18 | -21.3 | 2 | 9.2 |
| 358.2+03.6 | M3-10 | -131.4 | 1, 2, 3 | |
| 358.3-21.6 | IC1297 | +9.1 | 1 | |
| 358.5-04.2 | H1-46 | -44.3 | 1, 2 | 7.1 |
| 358.7-05.2 | H1-50 | +70.4 | 1 | 7.6 |
| 359.1-02.3 | M3-16 | +72.0 | 2 | 5.9 |
| 359.1-01.7 | M1-29 | -41.3 | 1, 2, 3 | 3.2 |
| 359.3-00.9 | HB5 | -22.9 | 1 | 1.3 |
| 359.7-02.6 | H1-40 | +63.8 | 1 | 7.8 |
| 359.8-07.2 | M2-32 | -53.6 | 1 | |
| 359.9-04.5 | M2-27 | +145.0 | 1, 2 | |
|
|
, [N II]; 3 HeII
a Using the angular size of Bedding & Zijlstra
(1994).