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The observations were made at 80 MHz and 160 MHz with HPBW in RA of 3.70' and 1.85' respectively. The beamwidth in Dec is wider by sec(30.3 + Dec). This list brings together all CCA measurements of flux density, position, spectral index and angular size, with limiting flux densities of 4 Jy at 80 MHz and 2 Jy at 160 MHz. References to the original Culgoora publications are given for each source.
The sources were selected for CCA observations from the Parkes, 4C and Ohio catalogues if an extrapolation of the then existing spectral data indicated that the 80 MHz flux density would be > 5 Jy. In addition, about 300 additional sources were added from lists of special classes of objects such as those discovered at higher frequencies from surveys of the galactic plane, lists of pulsars and supernova remnants, from a list of nearby bright galaxies and finally from a CCA survey of 353 Abell clusters of galaxies. An area of 16'x16' was surveyed about the centres of 3500 fields, resulting in a total survey area of about 0.1 sr at 80 MHz.
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name IAU name
9 A1 --- nFlag Flagged '*' or '#'
11- 12 I2 h RAh Right Ascension B1950 (hours)
14- 15 I2 min RAm Right Ascension B1950 (minutes)
17- 20 F4.1 s RAs Right Ascension B1950 (seconds)
22 A1 --- DE- Declination B1950 (sign)
23- 24 I2 deg DEd Declination B1950 (degrees)
26- 27 I2 arcmin DEm Declination B1950 (arcminutes)
29- 30 I2 arcsec DEs Declination B1950 (arcseconds)
32- 36 F5.1 deg l Galactic longitude (degrees)
38- 42 F5.1 deg b Galactic latitude (degrees)
44- 49 F6.1 Jy F160 Flux density (Jy) at 160 MHz
51 A1 --- '<' '<' if 80 MHz flux density is an upper limit
52- 56 I5 Jy F80 Flux density (Jy) at 80 MHz
58- 62 F5.2 --- Alpha Spectral index between 80 and 160 MHz
64- 74 A11 --- Ref References to original Culgoora publications
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NAME | RA (1950)| DEC |GLONG| GLAT|160FLX| 80FLX| SPEC| CUL |
| h m s | d ' ''| | | (Jy) | (Jy) |INDEX| REFS |
---------|----------|---------|-----|-----|------|------|-----|-----------|
0000-177 00 00 48.9 -17 44 02 71.5 -75.3 11.8 22 -0.90 1,3
0000-362 00 00 39.0 -36 14 16 349.2 -76.5 8.1 19 -1.23 2,3
0001+128 00 01 06.2 +12 51 31 105.4 -48.1 9.1 22 -1.27 2,3
0002+125* 00 02 11.5 +12 31 52 105.6 -48.5 9.1 20 -1.14 1,3,5
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General
1. COLUMN name
This column contains the B1950 name of the source, using IAU
recommended standards. The first four characters are the hours and
minutes of right ascension, and the last four the signed declination
in tenths of a degree (truncated). The source names in the original
Culgoora-1,2,3 Lists contained the signed declination in degrees
(truncated). An asterisk (*) following the source name denotes that
this is the centroid of two or more components, which can be located
in the maps and tables of references 3,4 and 5 below. The components
are not always parts of the same source. The flag '#' indicates that
the Culgoora position was lost, but the source can confidently be
identified with a source whose coordinates are given in the publication
listed in the reference column.
2. COLUMNS ra_1950 dec_1950
These columns contain the B1950 right ascension and declination of the
source. The 160 MHz position is given if
available, otherwise the 80 MHz position. The positional calibration
was obtained by observing at 2-hourly intervals strong unresolved sources
with accurate high-frequency positions. Position errors are tabulated
for various flux ranges and numbers of observations in the original
Culgoora-1,2,3 Lists. The positions of sources with contour maps at
160 MHz are the centroids of the brightness distributions.
Positions of other sources were found
by fitting a one-dimensional Gaussian to the hour angle drift response
and another Gaussian across the declination channels.
3. COLUMNS gal_long gal_lat
These columns contain the galactic longitude and latitude of the source in
degrees.
4. COLUMNS flux_160 flux_flg flux_80
The F160 and F80 columns contain the integrated flux densities
of the source at 160 MHz and 80 MHz respectively. The flux_flg column
contains a '<' if the 80 MHz flux density is an upper limit. A
recalibration of the flux scales was carried out by Slee & Siegman
(1988). This resulted in our increasing the flux density by an average
of 10% at 80 MHz and 12% at 160 MHz. The 160 MHz flux densities of
sources with contour maps (entries in the angular size columns) were
obtained by integrating the brightness contours.
5. COLUMN sp_index
This column contains the power-law spectral index between 80 and 160 MHz.
A negative spectral index implys that flux density is decreasing with
frequency.
6. COLUMN cul_ref
This column contains numbers that refer to the original Culgoora publications
that contain data about this source. The reference codes are as follows:
1 Slee & Higgins 1973, AuJPh Astrophys. Suppl. 27 (Culgoora-1 List)
2 Slee & Higgins 1975, AuJPh Astrophys. Suppl. 36 (Culgoora-2 List)
3 Slee 1977, AuJPh Astrophys. Suppl. 43. (Culgoora-3 List)
4 Slee & Siegman 1983, Proc. ASA 5, 114 (Cluster Survey)
5 Slee, Siegman, & Mulhall 1982, Proc. ASA 4, 278 (Culgoora-3 Analysis)
6 Slee & Quinn 1979, Proc. ASA 3, 332 (Cluster Survey)
7 Slee 1972, Astrophys. Lett. 12, 75 (Bright Galaxies at 80 MHz)
8 Dulk & Slee 1972, AuJPh 25, 429 (Supernova Remnants)
9 Slee & Sheridan 1975, Proc. ASA 2,1 (Cen-A & Pictor-A)
10 Dulk & Slee 1974, Nature 248, 33 (Sgr-A at 160 MHz)
11 Becker, White & Edwards 1991, ApJS, 75, 1 (0736+016,2330+091,2349+135)
12 Owen, White & Burns 1992, ApJS, 80, 501 (1005+007)
13 Douglas 1980 (Texas Survey) (2335+000)
Additional data in these papers include 80 MHz positions, optical
identifications and beam broadening from the one-dimensional Gaussian
fitting. The Culgoora-1,2,3 papers also contain tables listing the expected
errors in flux density and position. References 3 and 4 contain the 160 MHz
contour maps for many sources. Reference numbers 11,12,13 do not refer to
Culgoora publications, but refer to papers containing sources that can be
confidently identified with five sources, whose Culgoora positions have been
lost.
References
Becker, R.H., White, R.L. & Edwards, A.L. 1991, ApJS, 75, 1
Douglas, J.N. 1980, BAAS 19, 1048 (Texas Survey, on-line version of EOLS)
Dulk, G.A. & Slee, O.B. 1974, Nature, 248, 33
Dulk, G.A. & Slee, O.B. 1972, Aust. J. Phys., 25, 429
Owen, F.N., White, R.A, & Burns, J.O. 1992, ApJS, 80, 501
Slee, O.B. 1972, Astrophys. Lett., 12, 75
Slee, O.B. & Higgins, C.S. 1973, Aust. J. Phys. Astrophys. Suppl. No. 27
Slee, O.B. & Higgins, C.S. 1975, Aust. J. Phys. Astrophys. Suppl. No. 36
Slee, O.B. 1977, Aust. J. Phys. Astrophys. Suppl. No. 43
Slee, O.B. & Quinn, P.J. 1979, Proc. Astron. Soc. Aust., 3, 332
Slee, O.B., Siegman, B.C. & Mulhall, P.S. 1982, Proc. Astron. Soc. Aust.,4, 278
Slee, O.B. & Siegman, B.C. 1983, Proc. Astron. Soc. Aust., 5, 114
Slee, O.B. & Siegman, B.C. 1988, MNRAS 235, 1313
Slee, O.B. & Sheridan, K.V. 1975, Proc. Astron. Soc. Aust., 2,1
Additional Information
The basic table was formed by electronically scanning the Culgoora-3 list.
Each line was later checked by visual comparison with the unscanned list
and scanning errors were corrected manually. Additional sources were added
manually from other references in