J/other/PASA/17.92 CO emission towards Southern dark clouds (Otrupcek+ 2000)
Catalogue of J = 1-0 CO emission towards southern dark clouds.
Otrupcek R.E., Hartley M., Wang J.-S.
<Publications - Astron. Soc. Australia, 17, 92 (2000)>
=2000PASA...17...92O 2000PASA...17...92O
ADC_Keywords: Molecular clouds ; Carbon monoxide
Keywords: catalogues - ISM: clouds - ISM: molecules
Abstract:
Using the 22-m 'Mopra' antenna (near Coonabarabran, NSW) of the
Australia Telescope National Facility (ATNF), we have observed
emission from the 115-GHz J=1-0 transition of CO towards the centre of
each of the 1101 clouds listed in the Hartley et al. Catalogue of
Southern Dark Clouds (SDC, Cat. VII/191). The velocity range covered
was -96 to +70km/s, with a velocity resolution of 0.120km/s. CO was
detected at 1049 of the positions, with 367 spectra showing emission
at more than one radial velocity. Here we present the most
comprehensive general survey of the SDC catalogue, with the intensity,
velocity and half-width of the CO detection and a code describing the
profile shape. The presence of blue- or red-shifted wings in many
observations can provide a starting point in searches for star-forming
regions.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 80 1675 Southern dark cloud CO catalogue
mnp01.ps 81 432 PostScript version of table1, part. 1
mnp02.ps 81 975 PostScript version of table1, part. 2
mnp03.ps 81 1119 PostScript version of table1, part. 3
mnp04.ps 81 1070 PostScript version of table1, part. 4
mnp05.ps 81 1291 PostScript version of table1, part. 5
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See also:
VII/191 : Catalogue of Southern Dark Clouds (Hartley+ 1986)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Cloud designation in Galactic coordinates
13- 14 I2 h RAh Right ascension (1950)
16- 17 I2 min RAm Right ascension (1950)
19- 20 I2 s RAs Right ascension (1950)
22 A1 --- DE- Declination sign (1950)
23- 24 I2 deg DEd Declination (1950)
26- 29 F4.1 arcmin DEm Declination (1950)
32 A1 --- Den [A-C] Optical density code (1)
34- 38 F5.1 arcmin Size1 Largest angular size
40 A1 --- --- [x]
41- 45 F5.1 arcmin Size2 ? Second angular size
46 A1 --- n_Size2 [*] Note when no Size2 (2)
47- 50 F4.1 K T*A ? Antenna temperature at 115GHz J=1-0 transition
52- 56 F5.1 km/s Vlsr ? LSR velocity
58- 61 F4.1 km/s FWHM ? FWHM
63- 68 A6 --- Prof Profile shape description code (3)
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Note (1): Densities are represented by a 3-letter scale
with A being the most dense and C the least dense.
Note (2): Printed size:
For 279.0-16.1, the printed size was 16x x2
For 280.0- 7.7, the printed size was 16x x
For both, the size was remplaced by "16. x *" in table1.dat
Note (3): Description of the direction of the wings:
a: well-defined narrow Gaussian-shaped spectra with FWHM usually
<1.0km/s, an rms of fitted Gaussian <0.5K and, mostly, with
central velocity between -10 and +10km/s. They suggest a cold
cloud in a quiescent state, and the emission in these profiles
are most likely associated with the optical dark clouds
b: broad, rounded, non-Gaussian spectra with FWHM - usually
>2.0km/s. These profiles occurred across the velocity range but
were usually at velocities more negative than -10.0km/s. They
were often found in the direction of HII regions, or along the
line of sight of a spiral arm in the Galactic Plane (see
Robinson et al., 1988A&A...193...60R 1988A&A...193...60R)
c: straight-sided profiles with a square top, broader than class
'a', with an FWHM usually between 1.0 and 2.0km/s, an rms of
Gaussian fit >0.5km/s and a central velocity usually between
-10.0.and +10.0km/s. They suggest an optically thick dark cloud
(see Morris, 1975ApJ...197..603M 1975ApJ...197..603M), or a cloud with
turbulence or expansion. The occurrences of these profile shapes
should correlate highly with grade 'A' density clouds in the
SDC catalogue
d: Gaussian-shaped spectra, but with additional wings. Detections
usually lie in the velocity range of -20.0 to +20.0km/s. The
profile shapes could be caused by a blending of narrower
Gaussian features in the same line of sight with slightly
shifted velocities (as described in code 'e'). Where possible
we have fitted more than one Gaussian to the emission.
Alternatively, they might indicate outflows or bipolar
characteristics (Lada, 1985ARA&A..23..267L 1985ARA&A..23..267L), as are often found
in star-forming regions. The numbered sub-divisions denote the
direction of the wings
d-: blue-shifted wing (in the direction of decreasing velocity)
dd: wings on both sides of main component
d+: red-shifted wing (in the direction of increasing velocity)
e: blended Gaussian shape of several narrow components. If one
component has lower amplitude and is almost merged with another,
the result can look like a 'd'-shaped spectrum. If there are
several components of similar intensity, they can look like a
'c'- or even a 'b'-shaped spectrum
e 1: a complex emission shape that requires more than one Gaussian;
e 2: the components have separate fitted Gaussians that are numbered.
The description code applies to the combined emission.
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History:
Copied at http://www.atnf.csiro.au/pasa/17_1/otrupcek/
Some corrections made on 13-Jul-2004
(End) James Marcout, Patricia Bauer [CDS] 03-Oct-2000