- CSIRO Publishing

A CATALOGUE OF RADIO SOURCES BETWEEN DECLINATIONS
-20 0 AND -50 0
By B. Y. MILLS,*t
o.
B. SLEE,* and E.
R. HILL*
[1vlanuscript received June 15. 1960J
Summary
A catalogue has been prepared of the radio sources observed between declinations
_20 0 and _50 0 , using the Sydney cross-type radio telescope at a wavelength of 3·5 m ;
a total of 892 sources is listed. This supplements an earlier catalogue in the declination
zone
10° to _20°. In addition to the positions and intensities of the sources, angular
sizes of 50 of the strongest are given: several are found to have a size less than 15" arc.
As before, identifications with bright optical objects have been sought, and a number of
galaxies of apparently abnormal radio emission listed. Statistical analyses of the
distribution of the radio sources give results very similar to those obtained using the
earlier catalogue. \Vithin the uncertainty in the data, the distribution appears uniform
in depth and there is a siguificantly greater number of sources of large apparent size than
expected from chance blending effects.
+
1. INTRODUCTION
Analysis has been continuing of the records taken with the Sydney 3·5 m
cross-type radio telescope. A catalogue of radio sources has now been prepared
between declinations -20 0 and -50 0 to add to the previously published catalogue
between +10 0 and -20 0 (Mills, Slee, and Hill 1958); the zone between -50 0
and -80°, which will complete the series, is in preparation. In the present
catalogue a total of 892 radio sources is listed in the area of 2·66 steradians.
The source density, 336 per steradian, is somewhat less than the previous figure
of 356 per steradian, but not significantly so in view of the inclusion
in the catalogue of the brightest regions of the Milky Way and the brightest
southern extragalactic source: these cause a marked reduction in the listings
of faint sources in their vicinity because of increased background temperatur(ls
and side-lobe effects.
The catalogue has been examined in the same manner as the earlier one for
identifications with optical objects and for the statistics of the radio source
distribution. Since the present data add little to the earlier conclusions and
since more data will be available soon from the final catalogue zone, these results
are discussed only briefly.
The present catalogue differs from the earlier one in that angular sizes are
given for about 50 sources unresolvable with the pencil-beam aerial. These
have been obtained with the newly developed angular size interferometer
(Goddard, Watkinson, and Mills 1960). Since the sizes of many more sources
* Division
t Present
of Radiophysics, C.S.I.R.O., University Grounds, Chippendale, N.S.W.
Address: :School of Physics, University of Sydney.
COSMIC RADIO SOURCES BETWEEN DECLINATIONS -20 AND -50°
0
677
in the catalogue will be available shortly, the analysis and discussion of the
results is postponed. It is interesting, however, that a number of radio sources
are listed which could not be resolved by the instrument. These have been
estimated to be smaller than 10-15" arc.
II. THE CATALOGUE
Preparation of the catalogue follows the methods described in two earlier
papers (Mills and Slee 1957; Mills, Slee, and Hill 1958); subsequently these
papers will be referred to as paper I and paper II respectively. The catalogue
is divided into three zones covering declinations -20° to -30°, -30° to -40°,
and -40° to -50°; they are given in Tables 1, 2, and 3. The previously used
scheme of reference numbers has been adopted in which the first two digits of
the number denote the hour of the Right Ascension; these are followed by the
sign of the declination and the tens digit measured in degrees and, finally, an
italicized serial number arranged in order of increasing Right Ascension within
the 1-hr period. Only the latter italicized numbers are given in the tables, as
the others are evident; for example in Table 1, the second source would be
referred to in the text as 00-22.
As before, the probable error in the final digit of a position is indicated by
a superscript. The positions given are directly as measured, with allowances
only for precession. In the catalogue of paper II the sources of highest accuracy
for which the estimated probable error in R.A. was ±0·1 m were corrected by
+4 8 • This correction was based on the differences between the apparent radio
and optical positions of six bright ide~tified galaxies. However, two of these
galaxies are of large angular size and complex structure so that differences are
probably not significant, a~d in two other cases our uncorrected positions were
confirmed by other observers. It therefore appears probable that the systematic
error in our positions is negligible and no such con:ections have been applied in
the present catalogue. Radio sources resolved by the aerial beam have been
treated as before, both their peak flux density and their integrated flux density
being given, the former in parentheses. In general, only sources with apparent
angular size less than 2° have been included in the catalogue, two exceptions
being the well-established sources at the galactic centre, 17 -213, and
Centaurus A, 13-42. When the size of a source has been measured using the
angular size interferometer it is given in the footnotes in units of seconds of arc.
These are "equivalent" sizes and refer to a circularly symmetric source of
Gaussian brightness distribution which has the same ratio of visibilities at spacings
of 30)" and 2920)" (Goddard, Watkinson, and Mills 1960). The measurements
are preliminary and are likely to be improved later. Possible identifications
with bright nebulae are also given in the footnotes; when the NGC number
is in parentheses there appears to be no reason for thinking that this is other
than an accidental coincidence in position. These and other possible identifications are discussed briefly in the next section.
A small portion of the catalogue is included in an area examined by Rishbeth
(1958), who gave contour diagrams and a short catalogue of radio sources in the
Vela-Puppis region near 08 h R.A. In general our catalogues agree quite closely,
678
B. Y. MILLS, O. B. SLEE, AND E. R. IDLL
TABLE
1
SOURCES BETWEEN DECLINATIONS
-20 0
AND
_30 0
Sources which may be " extended", that is, resolvable, are indicated by a dagger. A colon has
been placed beside uncertain flux densities. Angular sizes, where available, are indicated in the
footnotes. Details in Section II
Position (1950)
Ref.
No.
R.A.
h m
00
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
16
17
18
19
20
21
22
23
24
Dec.
S.
0
,
Position (1950)
Ref.
No.
R.A.
h m
01
01.2 3
02·P
07.1 8
10.03
16'OS
17.7 3
20.7 2
21·2'
21.9 3
22·0"
24·3'
24.3 4
25.3 4
29.9 3
30.54
33.22
35.2 6
35.52
36.94
38·P
42·0"
45·}2
54.44
56.53
22 408
23 227
28 556
23 43 7
22 37 7
20 406
25 22 6
21 158
29 434
26 16"
20 477
27 51 8
282F
24 32 5
22 09 7
20 184
26 41"
23 12 6
29 247
27 47 8
22 215
25 38'
26 23 7
29 21 8
00·}2
00.6 3
06.2 8
10.63
13.73
13.9 3
13.9 5
17.94
22.44
22
27
29
22
23
21
28
27
25
01
1
2
3
4
5
6
7
8
9
Flux
Density
(10- 26
W m- 2 (C/S)-1)
II4
43 6
06 7
19"
01 6
07 5
41"
25 8
25 7
6
10
8
8
13
13
21
14t
33(1)
17t
7
5
9
7
8
19
5
10
8
6
9
29(2)
9
8
35(3)
16
9
9t
8
24 (18)
12
7
9
10
11
12
13
14
15
16
17
18
19
02
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
16
17
18
19
20
21
22
Flux
Density
(10-26
W m- 2 (C/S)-1)
Dec.
S.
0
,
24.2 3
28.7 2
34·1'
35·9'
39·2'
39.6 3
43.3 4
48·7"
50.04
55.0 5
22 28 7
26 27 5
24 05 8
23 05 8
25 57 7
272F
24 166
29 444
27 23 7
21 097
02.84
05.2 3
08.5 4
09.34
16.43
21.5 3
22.2 3
24.1 6
26.8 5
29.9 4
31.44
33.5 2
39.84
42.6 3
44.03
45·4"
46·7"
53·4'
54.2 2
54·7"
54.7 3
59· 8'
23
22
28
23
24
28
23
23
24
20
23
29
28
21
23
29
20
22
23
20
26
29
8
18
6
5
7
16
12
63 (43)
II
10
10
16
8t
9
15
508
327
OF
48 6
59 5
316
2}6
58 7
03 7
43 7
43 6
II6
12 8
568
57 7
28 7
427
09 7
326
466
187
18 6
n
19
10(4)
9(4)
II
17
8
7
9
8
lOt
14
9
28
13
7
8
I
(1)
(2)
(3)
(4)
~20·.
NGC 253.
,.",30'.
Sources 02-28, 02-29 form perhaps one extended source.
COSMIC RADIO SOURCES BETWEEN DECLINATIONS
TABLE
Position (1950)
Ref.
No.
R.A.
h m
03
1
2
3
4
5
6
7
8
9
10
11
12
13
14
04.1 4
05.2 4
13.8 2
25·5"
27 ·2"
30· 7"
37·2"
37.6 5
38.1 4
45.4 2
46·7'
49.7 2
52.1 4
58· 74
Deo.
0
s. ,
1
3
4
5
6
7
8
9
10
11
12
13
14
15
16
17
18
19
20
21
22
23
I
06-3"
06· 7"
12·9"
13·7"
14· 7"
20.3 4
22·5'
26.7 4
27·9"
30·4"
30.73
30.94
32· 7"
34.6 5
34·8"
36.7 5
37 -IS
42· 71
45·9"
50·4"
52·9"
53·3"
56.5 4
Position (1950)
Ref.
No.
h m
HO)
>45 n •
679
0
s.,
05
24
22
27
23
26
27
28
24
21
29
21
27
25
24
08"
31"
146
07 7
08'
23 7
46 5
148
407
26 5
37 7
57 5
45'
386
7
17
23
15(5)
14
8
9
8
14 (9)
15
9
53(6)
24
22
29
21
22
26
20
27
28
23
29
24
25
20
22
27
24
28
20
28
22
20
23
15"
52 6
40"
04 7
07 8
33 4
04 6
03 6
07 5
347
49 6
447
336
45 8
32 6
21"
398
18"
40 5
367
04 5
36'
43 7
1
2
3
4
5
6
7
8
9
10
11
12
llt
9
14
10
17
26
8
II
7
15t
12
7
13
8
8
5
01.9 5
03.6 2
08·4"
19·0"
25.5 4
28.6 4
40·9'
41·14
41·9"
43·2"
49· 7"
52.9 4
25
28
22
20
23
20
24
27
21
26
21
22
51"
414
06 6
31 6
21'
55'
16 6
28 6
08 6
27"
20"
47 8
02.84
04·6"
15·9"
19 -14
19·4"
20·1"
21·0"
24.5 4
30.44
34.7 1
37·4"
37 ·7"
51·0"
51.2 4
55·5"
56.9 1
28
20
28
24
27
26
25
20
27
20
27
28
21
22
26
24
56 6
13"
16 7
08 8
21 6
05 7
18'
35 7
166
37 4
36'
406
206
32'
40 7
13"
8
60 (30)
19t
19:(8)
9
8
13
7
10
12
8
9
06
1
2
3
4
5
6
'1
8
9
10
11
12
13
14
15
16
10
8
8
82(')
19
12
38 (21)
18
7
Possible oonfusion with IAU 03S3A side lobe.
40n.
(7) 35 n •
(8) Possible oonfusion with IAU 05S4A side lobe.
(9) (NGC 2217).
(5)
-50 0
Flux
Density
(10- 26
W m- 2 (O/S)-I)
Dec.
R.A.
I
(6)
AND
I (Oontinued)
Flux
Density
(10- 26
W m- 2 (O/S)-I)
04
2
-20 0
7
23
9
9
9(9)
7
llt
II
12
85 (67)
17
17
9
8
16159(10)
I
----------
680
B. Y. MILLS, O. B. SLEE, AND E. R. HILL
TABLE
I
Ref.
No.
Position (1950)
II
---I
R.A.
I h
m
I
1 (Oontinued)
Flux
Density
Dec.
(1O~'6
S.
W m-' (C/8)-I)
0
,
Position (1950)
Ref.
No.
h m
----
04· 23
06· 9 3
09· O'
15· 43
16·}3
20·}3
21· 9 3
24· 73
25.5 3
7
8
9
10
11
25· 8'
27.2 3
39.2 4
40· 7 3
50.5 4
50.9 4
54.4 4
12
13
14
15
16
10
11
12
13
14
15
16
17
18
1.9
I
I
43· 9'
50· 8 4
50· 9 3
55.3 3
56.4 3
59.6 2
0
22
29
20
24
26
21
23
24
20
28
22
24
28
21
26
23
58 6
14'
34 4
57 6
28 6
55 6
28'
51 6
39 6
45 7
06 5
18 8
15 8
47 8
20'
28 8
6
45 (22)(11)
71 (33)(11)
17
18t
11
15t
10
10
15t
16t
38 (24)
13
8
13
7
23
24
29
20
23
21
24
26
27
22
26
23
29
22
22
20
21
27
'I"
~D
33 8
48'
46 6
15 5
13 7
308
49 8
00 7
01 6
19'
308
306
35'
37 8
52 7
366
18 7
18 6
49 5
7
10
16
26
11
8t
11
9
16
9
14t
15
12 (12 )
9
8
19
7
13
54 (13 )
,
m~'
(C/S)-I)
--~~-
1
2
3
4
/;
6
7
8
9
10
11
12
13
14
05·7'
20.4 5
21'5 3
24· 54
26· 24
30· 73
35· 3 4
36.5 3
42.7 5
47.4 2
51.03
56.03
56· 6 3
59· 6 3
29
27
21
25
29
20
28
25
27
24
23
28
20
23
21 8
247
05 8
57 8
48 6
07 7
50 8
40 6
50 8
59 8
48 6
55 8
25 8
38 6
02· 8 2
06.5 4
08.5 4
10· 9 3
12· 53
24· 6 3
30· 8 3
35· 54
35· 94
35.93
21
30
28
27
23
29
23
24
28
26
23
28
22
20
26
27
3IS
00 6
308
50 8
386
46 6
37'
50 8
58 7
10 6
20'
46'
107
19'
00'
43 8
I
9
8
7
10
13
12
16:t
12
8
19
9
30 (18)(11)
6
15
10
1
2
3
4
5
6
7
8
9
10
11
12
13
14
J/)
16
40·1'
42· 73
43.0 4
48.9 4
53· 2 3
li3. ;)4
-.~-------------
Perhaps several sources.
(12) Perhaps one extended source with 08-37.
(13) 32".
(14) <10".
(15) A doubtful source.
(16) Perhaps a background irregularity.
Ill)
(10~'6
W
09
08
12· 3 3
12· 9 3
18· 3 3
25.1 2
25.1 4
26.7 5
33.1 4
34.53
34· 83
35· 7 4
42.7 5
43·0'
43· 43
Dec.
S.
07
1
2
3
4
5
6
1
2
3
4
5
6
7
8
.9
RA.
Flux
Density
48 (14 )
10
8(15)
12
10
9
18t
8
10
15
12
14t
9(16)
10
11
13t
OOSMIC RADIO SOUROJ;jS BETWEEN DEOLINATIONS
TABLE
I
Position (1950)
Ref. I
No. I
R.A.
I
I
i
I
1
2
3
4
5
6
7
8
9
h m
11
03.2 3
03.3 3
08.1 3
15.9 3
I
I
I
27·1"
29· 6 3
38.1 2
39.0 2
49· 8 2
51· 7 4
52.1 3
55· 74
I
1
I
2
I
08.4 3
09· 8 5
18.5 3
19· 24
22· 74
25.1 3
32.9 2
37.7 4
38· 3 3
40.9 3
45.0 4
51· 7 2
55· 8 4
56.63
59· 0 3
I
I
I
8
9
I
10 I
11
12 II
13
14
1.5
I
I
I
-I
1
2
3
4
5
6
I
I
I
I
II
24
20
22
25
28
26
26
28
30
28
28
22
33'
51 6
55'
53 6
56'
184
30 5
00"
08 8
11'
07 8
S.
25
26
27
26
25
20
24
20
23
27
28
29
25
23
20
02"
56 ' •
40'
46'
51 8
52 6
57 4
10'
19 6
27 6
58 6
03 4
25'
08 6
09 5
I
I
I
I
I
53 s
00 6
004
58'
32 6
05'
8 (16 )
Hi
16
7
8
9
\l
10
19t
8
28
27
7
9
13
15
1
2
3
4
14t
7
10
lOt
15t
12
28:
!l
Ht
17t
18
47 117 )
8
27:
16
11
I
15
61" 8 )
H
36"9 )
14
I
(17) ~351/.
t""..o'15".
NGC 5236.
(20) <; 12".
(21) Superimposed on background irregularity.
(8)
(19)
(22) >30".
681
Flux
Density
(10- 26
W m- 2
,
(C/S)-l)
-----
13
-
20
25
22
24
29
21
-~---
-~---
13
02· 73
03.5 5
09·0'
12· 24
34· 73
36.93
"
h In
5:2 5
-50 0
Dec.
R.A.
(C/S)-l)
12
i
3
4
5
6
7
Ref.
No.
--
I
I
II
,
11
10
12
0
T 111-2
I
Position (1950)
(10- 26
Dec.
S.
AND
1 (Continued)
Flux
Density
I
-20 0
45.9 4
50· 74
55· 74
56.7 3
25
23
23
21
14'
388
358
55 6
17:
9
9
8t
14
/;
6
7
8
9
27 18 5
03· 8 2
08.0 3
22 27'
08· 8 3 I 27 29'
I
09· 8 3
20 18 B
10.9 5
23 38'
14·1"
21 24 5
19· 53
29 18 B
20.2 3
27 14 5
20· 6 3
24 52 6
21· 74
29 42 6
22.0 4
23 48'
25.6 3
21 47'0
39.03
26 28 5
39.03 ! 24 38'
54· 73
28 21"
I
10
11
12
13
14
1.5
.9
10
11
12
13
14
14
26
17
18 (11)111)
24
9:
7
I
15
1
2
3
4
5
6
7
8
20
8:
13
12:
19
17
15
40 (20 )
03.8 3
05.1 4
05· 8 4
07.0 3
07.9 5
1l·H3
18.0 5
25· 24
26· 74
26· 8 4
44.3 4
50·0'
56.2 3
56.43
22
26
2H
20
25
22
28
26
27
20
22
25
21
24
20'
27 6
23 5
13 6
15'
22 6
13 6
42 6
38 6
lOS
42'
10'
35 5
05"
lO
H
35 (20)
9
7 (16 )
H12!)
7
11
18t
8
13
12
36 (22 )
18
I
682
B. Y. MILLS, O. B. SLEE, AND E. R. HILL
TABLE
1 (Continued)
~--~
Position (1950)
Ref.
No.
R.A.
h m
Dec.
S.
0
,
10
11
12
!
I
II
Flux
Density
(10- 26
W m- 2 (C/S)-l)
10
11
12
13
14
15
16
17
I
I
I
(23)
0
,
28
20
23
28
26
23
21
25
22
25
20
28
50 5
21 6
53'
006 I
50 6
388
33'
25 10
22 5
40 B
13 6
43'
35
20
14
18
27
10(15)
01· 7"
08.2 3
09.5 2
09.9 3
10· 8 2
13·2'
17.9 3
22.1 6
22.4 4
23.0 5
27.81
37.0 4
43· 79
52· 24
52.4 4
57.41
24
20
23
28
25
29
28
20
26
28
21
21
28
21
23
23
28
24'
56 6
18 5
00'
00 5
50'
56 B
19B
50 6
05 6
29 3
33'
4112
30'
05 6
26 3
003
15(15)
8
19
22
14
11
25(15)
19
42(23)
24
47(24)
38
32(15)
17
18
14t(15)
110(25)
21
4500(26)
194 (87)
82t
900(27)
35(28)
02· 71
02·8'
04.0 2
05· 83
12· 8 3
14.9 5
16.23
1
2
3
4
,5
6
7
8
9
22·5"
23· 8"
24· 83
33· 6 3
48· 53
50.9 5
10
11
12
13
14
53·0'
21
26
20
27
24
22
25
20
24
29
23
25
26
22
23 3
03'
10'
00'
09 5
40 6
45 6
05'
03'
106
59'
57 6
52'
27 6
Flux
Density
(10- 26
W m- 2 (C/S)-l)
23
25
26
24
21
20
25
26
24
22
27
28
21
33 5
09 5
58 5
49 6
41'
37'
44 5
40 6
08 6
22 6
05 6
01"
47 6
253(29)
19(15)
70
34
114 (71)(16, "0)
24
30t
70 (27)
31
26
39
23(16)
22(16)
10(16)
19
1
2
3
4
5
6
7
8
9
10
11
12
13
00·1"
04.0 3
12.83
13· 6 3
16.43
20.4 3
25· 6 3
29.2 4
33.46
34.9 3
42· 6 3
46.4 4
50.4 4
> 30".
>40".
(25) Kepler's Supernova-size >45".
(26) lAD 17S2A, complex distribution-only the integrated flux is gi'):en.
(2') >65".
(28) ...-,,30".
(29) >60".
(30) >40".
(2.)
I
18
01.9 3
05·0'
18.2 5
19· 2 3
28' 73
35.96
36·6'
39.6 4
43·4"
53.3 4
53.63
59.3 3
59·9"
Dec.
S.
R.A.
h m
I
17
1
2
3
4
5
6
7
8
9
Position (1950)
Ref.
No.
I
16
1
2
3
4
5
6
7
8
9
I
35t
17
53t
35
18
8
21t
42
9
11
12
18
11
coslInc RADIO SOURCES BETWEEN DECLINA'l'IONS
TABLE
Position (1950)
Ref_
No_
R.A_
I
h m
8
9
10
11
12
13
14
15
16
S_
0
,
8
9
10
11
12
13
14
15
Position (1950)
Ref_
No_
Deo_
S_
R.A_
h m
I
02- 83
15-13
18-3 4
21-1 4
24-3 4
24-54
27-4 3
29-9 3
34- 8 3
35-7 3
38- 83
40- 6 3
45-2 3
53-0 3
58-7 2
59- 9'
25
29
22
21
20
21
29
23
24
20
27
26
24
20
28
21
03 6
40 7
23 7
II"
34 6
44 5
40 7
005
188
16 7
57 6
43 5
16 7
07 5
13 4
05 7
04- 61
06-23
13- 6 3
15-33
18-93
23-14
24- 93
26-6 3
28· 3 3
34· 7 3
36· 3 3
36· 7 3
50-0'
50· 73
59· 9'
25
23
21
25
26
23
29
22
20
20
25
27
20
28
28
393
55 6
lIS
07 6
45 6
58 7
247
55 7
54 5
(31) <;20"_
> 50"_
(32)
-50 0
7(15)
11
8
11
9
18
9 (15 )
22
6
9
12
18t
12
25
59:(31)
8(16)
57 6
59 6
58 6
03 7
108
366
100(32)
2lt
24
15
17
9
10
9
16
11
15
8
15
12
10
683
1 (Continued)
Flux
Density
(10- 2 •
W m- 2 (O/S)-l)
21
1
2
3
4
5
6
7
AND
0
,
Flux
Density
(10- 26
W m- 2 (O/S)-l)
I
20
1
2
3
4
5
6
7
Deo_
-20 0
22
1
2
3
4
5
6
7
8
9
10
11
14- 7 4
16-73
22-8 4
26-5 3
32-7 4
45-9 4
46-5 4
47-3 3
48-14
55- 3 3
59-43
23
24
26
23
22
23
26
02 6
23 6
53 7
19 5
17 6
015
55 6
23 (14)
11
9
9
9
9
8
13
7
9
8
03- 8 3
07-14
10-9 4
17 -13
17 -53
18- 1"
22-93
26-4 3
27 -54
42- 53
45- 8 3
46- 73
47 - 93
49-8 3
51-93
55.4 4
25
28
21
27
22
24
23
21
25
24
28
26
25
23
22
21
26 6
20 6
57 6
386
136
25 5
20 6
25 5
22 6
10 5
20 6
25 7
16 4
19 6
25 6
30 7
13
7
8
23
13
12t
12
20
27 (16)
10
15
6
16
7
7
11
28 23 6
20 50 7
27 32 8
29 301
23
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
16
684
B. Y. MILLS, O. B. SLEE, AND E. R. HILL
TABLE
2
SOURCES BETWEEN DECLINATIONS
-30 0
AND
--40 0
Sources which may be" extended ", that is, resolvable, are indicated by a dagger. A colon has
been placed beside uncertain flux densities. Angular sizes, where available, are indicated in the
footnotes. Details in Section II
Position (1950)
Ref.
No.
R.A.
hm
Dec.
S.
0
,
Flux
Density
(10- 26
W m-' (C/8)-I)
Position (1950)
Ref.
No.
h m
11
12
13
14
15
16
17
01
1
2
3
4
5
6
7
8
9
-
(1)
00.2 3
02·7'
06.9 3
09.8 4
12.93
14·1"
14.53
23·1"
25.3 4
32.9 5
33· 73
34.3 3
36.2 2
37·1"
41·9"
51.6 3
53.5 5
31 136
36 50S
32 21 s
33 16 7
38 27 6
31 284
36 41 6
33 07'
39 21 6
33 41'
37 47 6
30417
39 24 6
33 06'
35 38 4
36 38 5
38 03 6
00.6 3
03.3 3
07.2 3
07.3 3
07.9 3
12·2'
12.7 6
19.9 3
24·7"
31 366
38 25 6
37 02 6
39 20 6
35 01"
32 30'
31 21 s
37 49 5
364F
17
8
14t
12
19
17
10
11
12
13
14
15
0
,
I
30.43
31·6'
41.2 3
44.3 3
54.2 3
57.9 3
38
36
39
37
36
31
316
44 3
48 5
317
23 5
10'
10
56t(5)
15(6)
04.5 3
10·0'
16·0'
18.83
24.5 3
25.03
38.5 4
45.3 3
59· 53
37 52 S
3431"
36 45 5
38 21 6
3051"
34 05 6
31 136
35 34'
34 36 6
10
13
29t(S)
19
14
9
8
10
13t
20· 6 2
32.6 4
36·2"
36· 73
42·8'
44·9"
45·7'
55·1"
57·1'
37 23 3
39 09 6
35 35 5
32 01'
31 16'
34 35 4
35 18 7
3021"
37 02 6
9
16
26(7)
7
20
8
9t
9
9
30(0
02
13
15
12(')t
1
2
3
4
5
6
7
8
9
12
9
8
10
30 (15)(3)
17 (4 )
10 (4 )
19
10
1
2
3
4
5
6
7
8
9
11
03
15 H •
NGC 300.
(3) Perhaps several sources.
I') Sources 01-36, 01-37 perhaps form one extended source.
(5) >45 H •
(6) A doubtful source.
(2)
(7)
Dec.
S.
01
00
1
2
3
4
5
6
7
8
9
10
R.A.
Flux
Density
(10-. 6
W m-' (C/S)-I)
<15 H •
>40H.
(0) Fornax A;
IAU 03S3A.
(10) NGC 1399 (NGC 1404).
(11) >45H •
IS)
NGC 1316 (NGC 1317).
950 (825)(9)
10
23(10)
14
H
33(11)
8
12
14
COSMIC RADIO SOURCES BETWEEN DECLINATIONS
TABLE
Position (1950)
Ref.
No.
R.A.
Dec.
S.
h m
0
,
Flux
Density
(10- 26
W m- 2 (C/S)-1)
Position (1950)
Ref.
No.
06
32
31
34
31
33
36
39
31
36
34
33
39
35
30
31
06'
11 6
33 4
01"
26 6
38 4
57 6
09 6
11 6
45"
00 6
12 6
53 6
16 5
58'
11
12t
16
6
12t
35 (12 )
03.8 4
04.6 4
04.6 4
04.9 2
11.5 2
21.43
22.9 3
24.9 3
34.23
38.1 3
41·9"
45· 84
46.3 3
50·0'
52.0 4
54·3'
58.2 5
59.3 2
59.8 2
38
37
32
37
30
36
32
30
37
33
38
30
33
35
36
32
31
38
39
55'
517
21"
01 6
34 5
24 6
48 6
55'
23'
4010
42 8
01"
04 6
06 6
317
14'
01 8
40'
49 5
8
13
6 (14 )
7(6)
14
10
8
6
8
18
10
78 (43)113)
9
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
05
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
16
17
18
19
R.A.
h m
05.3 3
06.3 3
10.62
19.8 5
20.5 2
27·12
31·1'
37.83
38.54
41.3 4
43·8'
45.0 5
46.4 3
54.5 2
55.43
Dec.
S.
,
0
E
Sources
Sources
Perhaps
Sources
-50 0
34
32
35
30
39
35
37
35
36
39
36
39
34
32
34
274
20"
24"
46'
32'
06"
115
26 4
38 6
16 6
05 8
56 4
196
40 8
348
22
17t
9
8
8
7
18
26
13t
8
7
26
9
9
5
00.0 3
00.9 4
06.0 4
07.6 3
15.33
17.2 4
18.9 2
19.03
25.8 3
27.6 3
29· 74
35.83
36.03
37.93
49.4 4
50.3 4
51·8'
53· 8 4
55.0 4
31
33
39
35
36
31
34
35
35
30
32
37
30
36
38
35
31
35
30
33'
3410
586
53 6
27 5
40 8
15'
01"
40'
108
03'
59 5
21 6
20'
45 8
06 8
06 8
40 8
21"
14t
11
12
15
18t
9
18(17)
9 (1 7)
07
29
66:(15)
18
8
9
30 (16)116)
8
7
14 (16 )
13
10(6)
14
9
16
20
685
Flux
Density
(10- 26
W m- 2 (C/S)-1)
01.1 2
02.2 3
02.4 3
07.8 4
14.3 4
14.3 4
17.9 2
25.5 2
30.7 4
31.1 4
40.7 3
46· 72
50.2 3
50.2 3
58· 8 4
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
16
17
18
19
(12) <: 10".
11') Perhaps two sources.
(14) (NGC 1800).
(15) 20".
(16)
(1')
(18)
(19)
AND
2 (Oontinued)
04
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
-20 0
05-310, 05-313 perhaps form one extended source.
07-37, 07-38 perhaps form one extended source.
extended or superimposed on galactic emission feature.
07-317, 07-319 perhaps form one ext,ended source.
9
8
14
21 (18)
19
lIt
24 (13)
8t
9(19)
7
15(19)
686
B. Y. MILLS, O. B. SLEE, AND E. R. HILL
TABLE 2
Position (1950)
Ref.
No.
RA.
hm
Dec.
S.
0
,
Flux
Density
(10- 26
W m- S (C/S)-1)
(CcrrWinued)
Position (1950)
Ref.
No.
h m
08
7
8
9
10
11
12
13
38 5031 427
30 31'
325F
34 21 6
39 428
30 396
33 396
35 43 7
34 386
33 407
31 508
34 308
38 (19)
19 (10 )
20
30 (20)IS1)
10
17
12 (22 )
17
8t
9t
11
9
6
7
8
9
10
11
12
01·9"
02.6 3
21.06
21.1 2
34·7'
38.83
41.5 3
42.3 3
44·0'
45.3 2
50.03
51.43
36
38
32
39
32
39
30
35
33
36
38
39
487
346
IF
56 6
25 8
166
25 7
407
006
51·
3510
26 7
02.23
03·5'
11·5'
14·3"
16·5'
17.73
29.3 2
30.82
35·2'
43.9 3
45·}8
36 587
32 308
31 458
30 08 6
313F
32 486
35 586
34096
39 507
38 00·
35 54 6
10
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
0
S.
,
15
25t
9:
9
14
8
8
8
8
11
25 (12)
17
9 (23 )
14
lO
11
14
19t
25 (15)
20
6
7
9
51.73
52.33
56.3 2
59.53
34
37
35
31
03 6
26 5
52007
12t
18 (12)
12
00.3 3
23·0'
23.5 3
25.8 3
27.1 2
35·1'
35·5'
36.03
43·4'
43.5 2
44·P
46.5 3
48·7'
50.8 2
55.53
32
37
35
32
34
39
36
31
35
31
33
37
35
34
31
108
008
126
186
20 7
02·
558
58·
206
41·
146
58 7
408
49 6
306
8
7
17
01.2 3
05.43
18.43
32.3 3
40.2 3
41·8"
43.2 3
54·2"
56.2 3
59.6 3
35
33
36
33
38
36
35
30
33
36
376
43 7
56 7
28 7
406
00'0
00'0
09146
546
05.3 6
09·0'
33.92
46·9'
59·1'
30037
36517
33 42 6
39 007
32 45 8
7
10
11
12
13
14
15
lot
11
11
8
28
9 12')
27
16
11
8 (2 4)
10 (24 )
13
12
1
2
3
4
5
6
7
8
9
10
13t
17
14t
22t
lIt
6
7
28
18
14
13
1
2
3
4
5
(20) Perhaps part of 08-34.
Extended parallel to galactic plane.
(22) Perhaps one extended source with 08-213.
(23) Perhaps a background irregularity.
(24) Sources 11-39, 11-313, 11-314 perhaps form one extended source.
(26) >50H , 14296.
(21)
lO
11
1
2
3
4
5
6
8
9
09
1
2
3
4
5
6
Dec.
lO
07.6 2
25·5'
27.2 3
28,532.32
40.8 3
43·0"
43·0·
45·4'
48·}3
50·5"
51·8'
59·8'
1
2
3
4
5
6
RA.
Flux
Density
(10-26
W m- 2 (C/S)-1)
12
9
70 (26 )
22
8 (6 )
COSMIC RADIO SOURCES BETWEEN DECLINATIONS
TABLE
Position (1950)
Ref.
No.
R.A.
h m
Dec.
S.
0
R.A.
h m
166
53 4
55 7
107
53"
546
28 6
224
107
20
57(26)
17
20
16
12(6)
04.2 3
07.43
17.63
22.43
30· 83
40.9 3
53·8'
39
30
39
37
31
38
35
22 6
307
366
207
21 6
37 6
56 7
14
9(6)
04·9'
10·9"
17.53
20.0 3
22.43
22.5 3
26.6 6
57.88
32
39
36
34
32
30
35
33
46 7
246
408
308
05 6
36 7
09 7
578
02·13
06·6'
31
37
38
35
38
546
10 5
23 4
40 5
147
14t
41
19
10
14
12(23)
21:('3)
10
19(6)
56 (28)16)
13
13
24
29t
11
19
17
1
2
3
4
5
Position (1950)
Ref.
No.
I
36
33
30
38
31
34
30
36
34
16
1
2
3
4
5
6
7
8
11·12
19.83
21.8 6
Dec.
S.
0
32
lOOt
500 (300)
75 (27)
687
Flux
Density
(10- 26
W m- 2 (C/S)-1)
I
6
7
8
9
10
18
1
2
3
4
5
6
7
8
9
19
1
2
3
4
5
26.2 3
26.7 2
28.3 2
36.62
39.93
34 45 5
3402'
32 43 5
30 50"
36 01 6
03.7 3
06.9 3
17.83
26·13
35.23
37· 73
48.6 3
49.43
58·6'
36
39
39
38
31
36
33
34
38
206
52"
115
115
51'
17 6
26 5
41'
246
9
9
41(28)
12.83
16.93
27.03
37.1 3
56.43
37
35
36
36
35
03 7
44 6
06 5
18
16
16
13
45 (80 )
04·5'
13.53
13·9'
14·0"
24·4'
29.83
32·3"
48.03
56.23
39
36
31
31
32
37
35
37
33
20
1
2
3
4
5
6
7
8
9
'U 5
49 4
00 8
05 7
446
00 7
015
406
04 5
07 6
00 7
75t
(B6) >45 N (NGC 5419).
>45N •
(28) <20N.
(28) Superimposed on background irregularity.
(80) Flux measurement uncertain due to Cygnus A side lobe ,...,20N •
(31) A doubtful source, perhaps extended or a background irregularity.
(32) <ION.
(27)
-50 0
2 (Continued)
Flux
Density
(10- 26
W m- B(C/S)-l)
00.63
01.53
18.83
21.7 3
28·13
29.63
40.33
51.3 2
51.43
15
1
2
3
4
5
6
7
AND
17
14
1
2
3
4
5
6
7
8
9
_20 0
60
120
95
165
31t
18
19
12(28)
15
17 (6 )
12
17t(31)
17
10
15t
18
7
41(81)
19t
9
688
B. Y. MILLS, O. B. SLEE, AND E. R. HILL
TABLE
Position (1950)
Ref.
No.
R.A.
Dec.
S.
h m
21
1
2
3
4
5
6
7
8
0
Flux
Density
(lO-28
W m-2 (C/S)-l)
(33)
Position (1950)
Ref.
No.
R.A.
Dec.
S.
h m
I
0
Flux
Density
(10- 28
W m-2 (C/S)-l)
I
22
00.3 3
07.9 3
10.44
14.63
16.04
28·1"
45·5"
57·3'
39
34
35
30
33
31
30
38
15.1 4
24.8 3
43.43
30 45 7
30 46 5
30 42 5
37 7
04 7
10·
36 8
357
22 5
23 6
046
12
14
8
15
8
13
14
1l(8)
22
1
2
3
2 (Oontinued)
>40".
8
10
12
4
5
48·4"
59.0 2
33 21 8
37 33 5
9
21
10.83
13·3"
34.23
34·3'
34.3 3
48.0 3
54.6 2
59.93
32
34
32
34
37
38
34
36
13
9
16
24
7(8)
23
1
2
3
4
5
6
7
8
26 7
317
56 6
58 6
38 8
39 6
59'
08 5
II
39(33)
18
COSMIC RADIO SOURCES BETWEEN DECLINATIONS
TABLE
-20 0
AND
-50 0
689
3
SOURCES BETWEEN DECLINATIONS
_40 0
AND
-50 0
Sources which may be" extended ", that is, resolvable, are indicated by a dagger. A colon has
been placed beside uncertain flux densities. Angular sizes, where available, are indicated in the
footnotes. Details in Section II
Position (1950)
Ref.
No.
R.A.
h m
00
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
01.6 3
03.8 3
08.2 2
17.2 3
17· 83
19·P
32· 74
34.2 3
36.64
39· 8'
43.7 2
44.0 4
48.8 4
50.1 4
52.93
Dec.
S.
0
,
03·2"
03· 63
07.4 4
12.9 4
14.03
15· 73
24.3 4
25·2"
31.43
39.53
39· 84
40.5 4
52.33
10
11
12
13
Position (1950)
Ref.
No.
R.A.
h m
02
48
42
44
41
49
47
45
49
41
44
42
49
44
43
49
23 6
50·
40 4
19 5
27 6
17 5
336
12 6
16 7
37 4
25 4
57 6
46 7
23 5
27 6
01
1
2
3
4
5
6
7
8
9
Flux
Density
(10- 26
W m- 2 (C/S)-l)
45
41
48
44
47
41
43
41
44
44
45
43
43
22 5
29 4
12 8
46 8
34 5
06 6
25 7
17 6
56 8
40 7
518
58 7
46 6
10
17
60 (31)(1)
13
9
13
9
8
7(2)
35(3)
52(4)
6
16
23
9
41(5)
25 (17)
5
8
34(6)
8(2)
8
33t
18
9
10
14
10
1
2
3
4
5
6
7
8
9
10
11
12
13
03
1
2
3
4
5
6
7
8
9
10
11
0
,
01.9 3
07.2 4
14.03
19.7 2
22· 63
24.2 4
27.4 3
30.5 2
34.63
40.2 3
43.5 3
55.03
55.3 4
44
42
48
45
42
43
40
41
43
42
45
44
48
02 5
00 5
03 5
33 5
03 7
15 8
147
22 5
49 6
03 7
07 5
05 7
49 5
9
16
65 (31)(7)
03.5 2
15.6 3
18.83
35· 53
38.43
38.53
42.0 2
43.64
51.2 3
53.03
54·P
46
44
45
41
40
47
44
45
41
43
48
427
006
20 7
28 5
37 6
46 5
20 6
46 7
23 5
04 8
244
8
10
19(9)
Perhaps two sources.
(2) A doubtful source.
(3) <15".
(4) >40".
(5) 23".
(6) >40".
(7) >40".
(8) Perhaps several sources.
(9) Measurement subject to side·lobe influence of IAU 03S3A.
(1)
Dec.
S.
Flux
Density
(10- 26
W m- 2 (C/S)-l)
lIt
17
7
24 (14)(8)
7
8
12
10
7
16t
14
10(2)
13
11
9
9
8
14
690
B. Y. MILLS, O. B. SLEE, AND E. R. HILL
TABLE
Position (1950)
Ref.
No.
R.A.
hm
Dec.
S.
0
5
6
7
8
9
10
11
12
05
1
2
3
4
5
6
7
8
9
10
11
08.2 4
13.93
18·13
18·2"
25·13
34.23
36.53
37.83
38.23
55.43
55.63
55.6 3
47
42
40
41
49
49
47
45
43
40
43
46
06 8
446
086
358
06 6
50 7
366
006
315
30 5
06 6
20 7
02.0 5
11.94
18.31
25.83
31.53
34.83
45.2 3
46.2 3
46·2'
47·8"
47·8'
41
48
45
40
45
49
48
44
45
40
42
50 7
32 6
483
56 7
40 8
46 6
17 6
356
57 6
52'
03 8
06·13
07.34
12.28
16.68
19.88
20·1'
5
6
49
42
47
48
45
47
Ref.
No.
387
27 8
186
44 5
07 6
00 7
R.A.
h m
9(10)
17
11
11
8
12
13
9
12
13
12
9(2)
7
41(11)
570(19)
14
19(2)
16
15
13
17
31t(13)
7
06
1
2
3
4
Position (1950)
Flu~
Density
(10- 26
W m-2 (C/S)-l)
I
04
1
2
3
4
3 (Continued)
15t
9
27
9
12
7
0
I
06
7
8
9
10
11
12
13
12(2)
27.5 3
29.7 3
34.2 6
37.0 5
40·8'
43.03
35.04
41
43
41
49
46
43
41
58 6
49 7
158
27 8
06 8
558
538
00'1"
02.5 3
04.3 3
05.3 4
08.8 5
10·6'
28.1 4
29·8'
33·7'
35.03
47.3 3
48·13
48·1'
51·2'
47
45
42
41
48
46
48
46
44
48
40
44
45
43
307
22 5
46 6
08 5
26 7
22 8
09 6
45 6
07 7
56 7
36 5
00 7
36 7
04 7
18
25
19
10
8(2)
09.43
09.8 3
16·1"
20.9 3
33.7 2
54.94
57.6 2
59.33
49
43
47
42
45
41
47
43
387
05 7
07 7
52'
38 6
25 7
25 7
266
27
9
7
8
7(2)
13
7
07
1
2
3
4
5
6
7
8
9
10
11
12
13
14
8
8
9
11t
12
12
27(14)
12
18(14)
08
1
2
3
4
5
6
7
8
(10) Perhaps extended or several sources.
<;20H •
(12) Pictor A; IAU 05S4A 55".
(18) >30H •
(14) Sources 07-412. 07-414 perhaps form one extended source.
(15) Puppis A; !AU 08S4A.
(16) >55".
(11)
Dec.
S.
Flux
Density
(10- 26
W m- 2 (C/S)-l)
10
10(2)
690 (514)(15)
1100 (276)(16)
lOt
26t
17
COSMIC RADIO SOURCES BETWEEN DECLINATIONS
TABLE
Position (1950)
Ref.
No.
R.A.
Dec.
S.
h m
09
1
2
3
4
5
6
7
8
9
10
0
46
45
43
46
45
49
41
46
45
43
Flux
Density
(10- 26
W m- 2 (C/8)-1)
02.9 4
03.3 3
14·9'
17.93
19.1 4
19.2 4
24·7'
25.8 4
26.43
32.2 5
39.3 4
46·4'
52·2'
9
10
11
12
13
7
11
8t(·)
8
7
9
12t
15(8)
15
12
49
46
44
42
45
49
40
47
45
41
46
49
40
446
27 5
25 7
26 3
48 7
227
57 5
52 8
00 7
178
05 6
157
00 7
9t
8
9
51 (17)
10
10
13
8
8
12t
13
8
6
11
1
2
3
4
5
6
7
8
04·4"
06· 73
16·1"
23·0'
33.93
43.3 3
49.1 3
55.5 3
41
48
43
48
43
48
44
42
56 6
23 7
247
13 6
157
20 6
56 7
167
10.7 4
11· 53
41 43 7
44 56 6
9
11
13
3
4
5
6
7
14
28
21(2)
13
18
8
-50 0
691
S.
0
Flux
Density
(10- 26
W m-' (C/8)-1)
I
16.24
33.7 4
46.8 3
51.9 2
55.7 3
46
41
40
47
41
017
25 7
56 5
43 5
338
02.6 6
22·4'
38.33
47·1'
56'0 2
49
42
40
45
41
07 7
414
327
367
38 4
08.9 3
12.63
14·4'
17 ·6'
25.2 3
25.7 3
32·9'
42.43
45.0 3
45.1 4
47.0 3
50·0"
51·3"
57.5 2
59·9"
41
43
47
49
43
47
45
42
46
48
40
41
42
48
41
336
23 6
23 7
447
07 6
48 6
05 6
138
57 6
09 6
186
00 7
176
04 6
42 5
14
38t(2)
14
16t
04.43
07.6 4
27.4 2
32.4 5
38.7 3
41.2 3
45·9'
55.3 3
42
43
42
49
40
48
45
46
54 7
56 8
215
44 8
427
04 7
046
127
14t
14
100
21t
18
47 (25)
24(2)
50t(23)
19t
11
45(18)
14:t
16
20(19)
8700 (2170)('0)
9
100 (32)('1)
35:
14
1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
90: (30)(22)
29
10
15
33
10
14
9
19(2)
17t
55:
15
1
2
3
4
5
6
7
8
",,30" IAU 10B4A.
(18) <15" (NGC 4696).
(19) NGC 4945.
(20) Centaurus A; IAU 13B4A. NGC 5128.
(21) Possibly a galactic feature.
(22) Perhaps several sources, the interpretation is doubtful.
(23) >30".
(17)
Dec.
13
1
2
3
4
5
53 (19)
12
1
2
R.A.
h m
10
1
2
3
4
5
6
7
8
Position (1950)
Ref.
No.
I
37 8
07 6
347
42 8
147
53 7
227
50 8
16 7
27 6
AND
3 (Continued)
12
06.9 4
09· 73
12.63
27.0 4
27.8 6
43.2 4
46.4 3
49.3 5
51· 84
51.9 3
_20 0
692
B. Y. MILLS, O. B. SLEE, AND E. R. HILL
TABLE
Position (1950)
Ref.
No.
R.A.
h m
Dec.
0
S.
,
16
1
2
3
4
5
6
7
8
9
10
11
3 (Oontinued)
Flux
Density
(10- 26
W m- 2 (C/8)-1)
Position (1950)
Ref.
No.
h m
19(2)
26:(24)
76(25)
03.03
17.44
19·9'
24.9 4
25.1 4
33.2 3
36.3 3
51·1"
52.1 4
57.6 5
59·0'
44
45
49
48
42
40
46
44
42
46
41
25 8
517
28 7
40 7
10 8
32 7
31 4
00 6
25 6
22 8
18 5
03.8 3
10.43
14.43
14· 83
16.63
17.1 4
31.3 3
54.4 3
44
45
44
48
49
46
48
41
24 6
36 7
00 7
20 7
33 7
47 8
318
33 7
25
35
18t
25
29
18
12t
30t
04.6 5
12.8 5
39.8 2
40.9 3
43.9 3
44.6 5
53·2'
59· 63
45
48
48
40
49
43
43
41
28 6
20 7
36 5
277
49 7
06 7
00 8
25 5
77 (45)
16:
41 (27)
22
12
8
7
13
12.03
13.9 3
46 28 6
45 39 5
11
13
64
30t
25(2)
330(26)
55t
32
30:
90 (70)
4
5
6
7
8
4
5
6
7
8
19
1
2
0
S.
,
4
5
6
7
8
9
10
11
12
13
21.7 3
25.2 3
31.83
32.6 2
32.9 3
35.43
36·7'
40.4 3
45.6 3
51.7 3
53.0 3
43 01 6
41 23 7
49 53 5
46 25 3
48317
42 347
48 01 6
40 41 6
47 08 5
49 59 6
42 38 5
03.5 3
05· 8 3
17.6 5
20·5'
27.3 3
28.9 3
37.33
43.9 4
47.0 5
51.4 3
47
42
42
49
41
45
47
43
44
48
40 6
376
23 8
53 7
306
23'
52 6
376
48 5
22 6
9
15t
9
8
22
10
11
16
13
12
09·4'
10·2'
16·9'
22·3'
27.7 3
37.1 5
40.3 2
50.5 3
43
45
47
44
48
44
43
46
12 6
26"
50"
56 7
25 6
26 4
214
39 6
15
7
7
7
10
10
37(30)
17
17
9
141 (28)
8
8
7
38t(29)
11
14
31t
20
18
1
2
3
Dec.
19
3
17
1
2
3
R.A.
Flux
Density
(10- 26
W m- 2 (C/8)-1)
(24) Possibly a background irregularity.
(25) >45".
(26) >45".
(27) >30
(28) 18".
(29) >30".
(30) >40".
H •
1
2
3
4
5
6
7
8
9
10
21
1
2
3
4
5
6
7
8
14
COSMIC RADIO SOURCES BETWEEN DECLINATIONS
TABLE
Position (1950)
Ref.
No.
R.A.
h m
Dec.
S.
0
,
Flux
Density
(10- 26
W m- 2 (O/S)-I)
Position (1950)
Ref.
No.
3
4
5
6
r
8
(81)
(3S)
R.A.
h m
Deo.
S.
0
,
Flux
Density
(10-26
W m- 2 (O/S)-I)
23
06.8 4
06.8 3
25.3 3
35.0 5
44.1 4
50·1"
56.83
57.08
2
693
3 (Oontinued)
22
1
-20° AND _50°
49
43
40
43
44
41
41
46
57 6
59 6
56 5
44 8
26 7
10 5
09 6
09 5
8
13
28
6
6:
42(31)
14
10
1
2
3
4
5
6
r
8
07.8 3
10'33
24.2 3
31.9 2
39.03
42.9 3
49.7 5
51.7 3
48
44
40
41
44
47
43
45
427
43 7
34 5
42'
507
25 8
24 8
26 7
ll:
10
15
50(3')
6
9
8
7(2')
30".
26'.
although we had available a number of " non-scanning" records of high sensitivity
not available to Rishbeth. His catalogue is valuable in that it is based on the
contour diagram, gives information about the shapes of some extended sources,
and includes several large concentrations not included in our cataloguing scheme.
There are, however, often large discordances in the flux densities of weaker
sources.
III. IDENTIFICATIONS
A search for identifications with bright optical objects has been carried out
as in papers I and II; the atlas of Becvar (1951) has again been used in this
search. Some of the area, north of declination -33°, is included in the National
Geographic Society-Palomar Observatory Sky Atlas. The previous catalogue
and a small portion of the present one has been compared with this Atlas in a
systematic way (Mills 1960) and no doubt a similar comparison of the remaining
common area will prove interesting, but it is outside the scope of the present
paper.
In contrast to the earlier work, no H II regions can be unambiguously
identified in the present catalogue; this arises partly as a result of their uneven
distribution and partly because the zone of the catalogue crosses the galactic
plane, in one of the two places, close to the galactic centre. Here the background
temperature is of the same order or higher than the electron temperatures in
the nebulae so that, if they are observed at all, they appear as "holes" in the
background emission: some of these are listed elsewhere (Mills 1959). Coincidences with planetary nebulae and globular clusters are again not significant:
there is a moderately close coincidence between the radio source 17 -21 and the
globular cluster NGC 6284, but this would be expected by chance. Two other
identifications with galactic objects are well known. These are Kepler's
supernova, identified with 17 -211 (Mills, Little, alid Sheridan 1956), and
694
B. Y. MffiLS, O. B. SLEE, AND E. R. HILL
08 -44 (Puppis A) identified by Baade and Minkowski (1954) with a galactic
nebulosity of a peculiar filamentary type.
There are numerous possible identifications with bright galaxies in the
catalogue. ,Those listed include all coincidences within 1 m in Right Ascension
and 20' in declination; there are 14 such coincidences and the chance expectation,
based on the numbers of catalogued galaxies and radio sources in the area, is
about 6. To reduce effects of chance we restrict attention to these coincidences
within om. 7 in Right Ascension and 13' in declination, as in paper II (these
numbers represent approximately twice the mean probable error in each
coordinate). There are 10 such coincidences with 3 expected by chance, but
since 5 of these were previously known the new information is not great. They
are listed in Table 4.
TABLE
4
POSsmLE IDENTIFICATIONS WITH BRIGHT GALAXIES
Radio
Source
00-221
03-31
03-31
03-33
06-25
12-46
13-41
13-42
13-33
13-25
Galaxy
m 1•9--mp
NGC
Type
253
1316
1317
1399
2217
4696 _
Sc
Sap
SBb
Eo
SBb
E1
1·2
-4·6
-6·6
-1·6
-0·5
-3·1
SBc
Ep
E
Sc
1·3
-3·9
-4·1
0·9
4945
5128
14296
5236
Notes
Fornax A
Probably a chance coincidence
The angular size of the radio source is
small. Probably a chance coincidence
Centaurus A, a well-known identification
The radio size supports the identification
,
Of the previously known systems we have three "normal" galaxies
NGC 253, NGC 4945, and NGC 5236, and two "radio" galaxies NGC 1316 and
NGC 5128. Two of the coincidences can almost certainly be ascribed to chance,
NGC 1317 and NGC 4696. In the former, the radio source is, by virtue of its
position and size, almost certainly associated with the neighbouring galaxy
NGC 1316; it would be a remarkable coincidence if NGC 1317 also were contributing to the radio emission. In the case of NGC 4696, which has been noted
also by Basinki, Bok, and Gottlieb (1959), the angular size, <15" arc, appears too
small. There are numerous fainter galaxies in the vicinity; but it appears
most likely that the radio source is considerably more distant than any of those
visible on the plate of Basinki, Bok, and Gottlieb. The galaxies NGC 1316 and
NGC 5128 have been discussed extensively in the literature and will not be
considered further in this paper (for the most recent results see Sheridan (1958)
and Wade (1959)).
It is interesting to see whether the above coincidences might be expected
assuming a radio" luminosity function" of the form suggested by Mills (1960).
In this, the probability of a galaxy, chosen at random, having a ratio of
COSMIC RADIO SOURCES BETWEEN DECLINATIONS
-20°
radio to optical emission, defined by m 1 •9 -mp , between
(where w=m1"9-mp) is given by
AND
_50 0
w-!
and
695
w+!
log P=l· 0 -0· 42W .
.Applying this result to the galaxies listed in the catalogue we have used, we
would expect 6 galaxies with m1"9-mp< -2 and 1 galaxy with m 1.9-mp< -4.
In fact there are 5 coincidences in the former category and 3 in the latter, a
satisfactory but not particularly significant agreement.
Two galaxies, NGC 300 and NGC 55, which are within the catalogue area,
had previously been listed as probably observed (Mills 1955) but are not in
Table 4. The former is listed in the footnotes to Table 2 as a possible coincidence
with the source 00 -317, that is, it is within 1 m in Right .Ascension and 20' in
declination. However, the identification is not certain because of a complex
brightness distribution in the region; this difficulty was noted previously. The
radio source associated with the latter galaxy is too faint for detection by the
methods used in preparing the catalogue and is not included; originally it was
necessary to average several records to observe it.
Finally, one should mention the two possible identifications found in the
previously mentioned comparison of part of the catalogue area with the Palomar
Sky .Atlas. These are the sources 17 -23 and 21-21; they are discussed
elsewhere (Mills 1960).
IV. STATISTICS
The question of the distribution of the radio sources has been discussed at
some length in papers I and II. The present results do not alter substantially
any of the earlier conclusions, so that a very brief discussion should be adequate
at this stage. More useful statistical investigations may be carried out when
the angular size data are complete.
Previously we had divided the analysis into two parts, the first concerned
with the two-dimensional distribution over the celestial sphere in an investigation
of possible clustering effects, the second with the distribution in depth of the
sources. These are not independent, but the division is convenient and will be
adhered to here.
(a) Clu8tering
Earlier analysis had provided some slight, but not conclusive, indications
of large-scale clustering of the radio sources. However, addition of the present
data weakens the case and, on confining attention to regions of the order of
10° to 30° across, no convincing evidence exists that the distribution is nonrandom.
However, in the present catalogue a curious distribution arises, namely,
the density of radio sources over the last few hours of the catalogue is very much
less than over the first few. For example, the number of sources between OOh
and 02 h is 103 and between 22h and OOh only 56. The probability of this
difference arising by chance in a random distribution is less than 0·001. Since
the catalogue was prepared in a number of stages each commencing at OOh and
working through to 24 h , it seems possible that the result is an artefact. However,
696
B. Y. MILLS, O. B. SLEE, AND E. R. HILL
the catalogue of paper II was prepared in essentially the same manner and shows
no such effect and, in addition, a careful re-examination of the original records
supports the idea that the difference is real. The region of high source con.
centration includes the south galactic pole, but no reason is known why this
should provide a surplus of radio sources.
100
z
«
D
«
I,
II:
w
I-
If)
\
10
If)
w
U
II:
:J
\
\
\ / SLOPE
.
o
If)
\
SLOPE
10
20
= - ,. 5
40
-1·3
\
\
eo
=
\
160
\
320
Fig. I.-Counts of Class II radio sources.
In paper II the number of "extended" sources was compared with the
number of blends of radio sources expected on the basis of a random distribution.
It was concluded that there was a very significant difference, indicating that
either the sources were extended regions of comparatively low brightness, or
close blends of physically associated sources of small size. The present results
support this conclusion although, surprisingly, the proportion of extended
sources listed is much less than before. For example, between Right Ascensions
of 09 h to 15 h and 21 h to 15 h (i.e. at high galactic latitudes) the numbers of extended
sources with flux density greater than 40 X10-26 W m- 2 (C/S)-1 is 9, and with
COSMIC RADIO SOURCES BETWEEN DECLINATIONS
_20° AND -50°
697
flux density >20 X 10-26 W m- 2 (C/S)-1 is 19: the corresponding numbers
expected on the basis of the previous catalogue are 16 and 29 respectively.
Similarly, the number of sources with flux densities >20 X 10-26 W m- 2 (C/S)-1
listed as "perhaps extended" is now 7 compared with an expectation of 14 ;
however, the availability of data from the angular size interferometer has helped
to eliminate some doubtful examples. Since the chance blends above the same
flux density limits may, from the data of paper I, be expected to be 2 and 11
respectively, the previous conclusion, that these are inadequate to explain the
observations, is upheld.
(b) Source Counts
One of the most interesting questions arising from a study of the statistics
of radio sources is their distribution in depth, which is investigated by means of
counts of sources with fluxes above defined levels. Since there is a class of
galactic source fairly closely confined to the plane it is usual to divide the analysis
into two parts, dealing with the low latitude and high latitude sources separately.
We will follow this procedure here, but, since the information about the galactic
sources adds little or nothing to that presented in paper II and by Mills (1959),
we will discuss only the high latitude or Class II sources (sources for which
I b />12tO).
In Figure 1 is shown the count resulting from a combination of the present
catalogue and that in paper II. The actual numbers are listed in Table 5.
TABLE
5
THE NUMBERS OF CLASS II RADIO SOURCES ABOVE DEFINED FLUX DENSITIES
Flux density (10- 26 Wm- 2 (O/S)-I)
Number of sources, N
7
10
20
40
80
160
320
640
1658
1220
332
94
24
7
6
4
The total area used in making these counts is nearly 5 steradians (2' 72
steradians in paper II and 2 ·07 steradians in the present catalogue) and altogether
there are 1658 sources with flux density > 7 X 10-26 W m- 2 (C/S)-1 (the total
number of Class II sources in the areas is 1700). Previously, the counts had been
restricted at high intensities because of the fortuitous lack of such sources in the
area of the catalogue; now, however, it may be extended much further, the
range of flux density being nearly 100 : 1. The standard error in each point in
Figure 1 is indicated by vertical wings; it is equal to yN, where N is the number
of sources counted.
It has been shown in paper I that the counts need correction at low flux
densities because of the effects of random noise and finite aerial resolution.
Another effect was discovered when compiling the present catalogue, namely,
a systematic tendency to over-estimate the flux density of a source when the
signal-to-noise ratio is low. This appears quite distinct from the effects of noise
previously considered; it was detected by comparison of flux densities measured
on " scanning" and" non-scanning" records. The former have a noise level
698
B. Y. MILLS, O. B. SLEE, AND E. R. HILL
approximately double that of the latter and it was found that flux densities
around 10 x10- 26 W m- 2 (cjS)-l were, on the average, estimated higher on the
scanning records by a factor of about 30 per cent. For sources of double the
flux density the effect was still noticeable but much reduced. These differences
appear to arise because a source position is always selected for which the noise
fluctuations combine with the deflection due to the source to produce the greatest
apparent flux density. This position is, in general, displaced from the true
position, which, if known and adopted, would result in a lower estimate for the
flux density. The effect of this type of error on the source counts is not large;
this is fortunate, since it is difficult to assess an accurate correction without
re-examination of all the original records. The most likely correction for the
combined counts is a reduction of 30 per cent. for sources having fluxes near
10 X 10-26 W m- 2 (cjs)-I, and 10 per cent. for sources having fluxes near
20 X 10-26 W m- 2 (cjS)-l. In Figure 1 the crosses mark the corrected points,
using both the data of paper I and the above corrections.
A straight line of slope -1,5 is shown, drawn to fit the points as closely as
possible; the fit is very good. Since this is the slope to be expected with a
uniform distribution of source in a static Euclidean universe, the source counts
indicate no divergence from uniformity and no obvious cosmological effects.
It has been suggested by Mills (1960) that, among those sources which are
associated with external galaxies, a source count having a mean slope of about
-1·3 might be expected, if account is taken of red-shift effects. A line of this
slope is shown dotted; although the agreement is not particularly good, it is not
inconsistent in view of the uncertain corrections to be applied at low flux densities
and the statistical uncertainties at higher fluxes. It is known, however, that
not all the high latitude radio sources in the catalogues could belong to this
class (unless there is physical clustering of such sources) because of the inclusion
of apparently" extended" sources in the catalogue, as discussed earlier.
Finally, one should mention a slight difference in the counts if the two
catalogues are analysed separately, the numbers in the present catalogue being
systematically less at a given flux density. Part of the discrepancy at low flux
densities may be due to the availability of more non-scanning records in the
area of the present catalogue and consequently less systematic error in the weaker
fluxes, whence, for a given number of sources, the flux density will be lower.
The remainder may be the result of a small calibration difference; this is likely,
since the first catalogue includes zenith angles between 44° and 14°, the second
includes zenith angles between 16° and 0°. A difference of 10 per cent. in the
average calibrations in these areas would be adequate to explain the effect:
this is about the accuracy of the calibrations, as discussed by Little (1958).
V.
REFERENCES
BAADE, W., and MINKOWSKI, R. L. (1954).-Astrophys. J. 119: 215.
BASINKI, JANE, BOK, B. J., and GOTTLIEB, K. (1959).-" Paris Symposium on Radio Astronomy."
(Ed. R. N. Bracewell.) p. 514. (Stanford Univ. Press.)
BECVAR, A. (1951).-" Atlas Coeli Skalnate Pleso." (Prirodovedecke Vydavatelstvi: Prague.)
GODDARD, B. R., WATKINSON, A., and MILLS, B. Y. (1960).-Aust. J. Phys. 13: 665.
COSMIC RADIO SOURCES BETWEEN DECLINATIONS
-20 0
AND
_50 0
A. G. (1958).-Aust. J. Phys. 11: 70.
B. Y .. (1955).-Aust. J. Phys. 8: 368.
MILLS, B. Y. (1959).-Publ. Astr. Soo. Paoif. 71: 267.
MILLS, B. Y. (1960).-Aust. J. Phys. 13: 550.
MILLS, B. Y., LITTLE, A. G., and SHERIDAN, K. V. (1956).-Aust. J. Phys. 9: 84.
MILLS, B. Y., and SLEE, O. B. (1957).-Aust. J. Phys. 10: 162.
MILLS, B. Y., SLEE, O. B., and HILL, E. R. (1958).-Aust. J. Phys. 11: 360.
RISHBETH, H. (1958).-Aust. J. Phys. 11: 550.
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LITTLE,
MILLS,
699