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1979AuJPA..48....1Haynes+
Aust. J. Phys. Astrophys. Suppl., 1979, N.48, 1-30.
A catalog of 5 GHz Galactic plane sources
R.F. Haynes, J.L. Caswell and L.W.J. Simons
Abstract
A catalogue at 5 GHz of 915 sources in the Galactic plane is presented.
Sources with a peak beam brightness temperature of at least 0.2 K above
the surrounding background are included, except in confused regions;
a point source of 0.2 K corresconds to 0.26 Jy.
Recently we punlished the results of a 5 GHz galactic plane survey
(Haynes et al., 1978, Aust. J. Phys. Astrophys. Suppl., N.45, 1.) covering
the region l = 190 - 360 - 40^o for |b| < 2^o.
The Parkes 64 m radio telescope was equipped with a 5 GHz receiver.
The antenna half-power beamwidth was 4.1' and filtering of the data
reduced the resolution in the scanning direction to 4.4'.
Hydra A (PKS0915-11) was chosen as the standard source for calibration
purposes. It was assumed that Hydra A was a point source with a peak flux
density of 13 Jy at 5 GHz; this is equivalent to a mean beam brightness
temperature of 10.0 K for a beamwidth of 4.1x4.4'. The positional
accuracy is 30" (rms).
Table is a catalogue of 915 sources in the galactic plane between
l = 190 - 360 - 40^o |b| < 2^o. The l,b pair of galactic coordinates
is given in columns 3 and 4 and values for the peak brightness temperature
and flux density are given in column 5 and 6. The reader shold refer
to Section 3 for information relating to the determination of the flux
densities. Column 7 gives an estimate of the source extension in minutes
of arc. Extents are given for sources in nonconfused regions only.
Finally, in column 8, comments on each source are included where appropriate.
Identifications with known supernova remnants are included from the
compilation of Clark and Caswell (1976). Identifications with HII regions
are based principally on H109a recombination-line emission data, which
are mostly obtained from Wilson et al.(1970) but with some unpublished
Parkes onservations included also.
1. Introduction
Recently we published the results of a 5 GHz galactic plane survey
(Haynes et al. 1978) covering the region l=190 - 360 - 40 for
-2 2. 5GHz Continuum Survey
We first summarize those parameters of the 5 GHz survey that are relevant
to the source catalogue : The Parkes 64 m radiotelescope was equipped
with a 5 GHz receiver having a system temperature of -100 K and a
bandwidth of -500 MHz. Only one linearly polarized component was accepted.
The antenna half-power beamwidth was 4'.1 arc, and filtering of the data
reduced the resolution in the scanning direction to 4'.4 arc. Hydra A
(PKS 0915-11) was chosen as the standard source for calibration purposes.
It was assumed that Hydra was a point source with a peak flux density of
13 Jy at the operating frequency of 5 GHz; this is equivalent to a main
beam brightness temperature of 10.0 K for a beamwidth of 4'.1X4'.4 arc.
The survey maps (Haynes et al. 1978) portray the sky beam brightness
temperature with a typical uncertainly of 10%. The positional accuracy is
30" arc (r.m.s.)
4. Catalogue
Table 1 is a catalogue of 915 sources in the galactic plane between l=190-
360-40 for -2 <b <2. The l, b pair of galactic coordinates is given
in columns 1 and 2, and essentially constitutes the galactic source name.
The 1950
equatorial coordinates for each source are given in columns 3 and 4, and
values for the peak brightness temperature and flux density are given in
columns 5 and 6. The reader should refer to Section 3 for information
relating to the determination of the flux densities. Column 7 gives an
estimate of the source extension in minutes of arc. Extents are given for
source in nonconfused regions only. Finally, in column 8, comments on each
source are included where appropriate. Identifications with known
supernova remnants are included from the compilation of Clark and Caswell
(1976). Identifications with HII regions are based principally on H109alfa
recombination-line emission data, which are mostly obtained from Wilson et
al. (1970) but with some unpublished Parked observations included also.