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A search for infrared stellar objects in a region in Carina
Chin.Astron.Astrophys.(199l)I5/3,270-274 A trans.lation of Acts Astrophys.Sin. (1991)11/Z, 137-142
A
SEARCH FOR1~
0 Pergamon Press plc Printed in Great Britain 0275-1062/91$10.00+.00
i!iiTELLAR OEMETS
IN A REGION IN WINA XIAO Zhen LI Jing Beijing Astronomical
Observatory,
Chinese Academy of
Sciences
AMTRACT This is the third paper of the series, giving the data on 89 infrared excess objects discovered in a region in Carina, of which 12 are identified with IRAS point sources.
Key words:
Photographic photometry-stellar excess objects.
colours-infrared
The aim, method and means of the present study have been set out in our two previous papers of the series [Z, 31. The present selected area is No. 128 in Carina in the UK-Schmidt Two-Coiour (R and I) Survey of Galactic Belt. The size of the region is 5.35’ x 5.35*. 5.5
..
5.0 4.5 ‘4 0 4 3.5 ‘3.0
ii:
-1700
-1500
-1300 Cosmae
Fig.
-I 100
2 Number-magnitude on I plate 13932
1 Received
-900
I
counts
1990 March 14; passed
Y
-Boo
Fig.
-600
-400
cosma‘
-200 K-1
3 Counts of colour from the plate-pair
by Referee:
1990 July
3.
0
index
2ao
Infrared
Search
271
TABLE 1 Astrometric B-binary,
Positions and Colour Indices Excess Objects in Carina
M-multiple,
D-diffuse,
DC-diffuse
of 89 Infrared around the image
NO.
NAME
I
DEC
RA (1950. 0)
R-l
TYPE DC
1
1203
LO 20
15.2
--59
09
36
1.8
7.
1609
10
10.1
-57
20
03
2.1
3
,607
10
7.9 55.0
-59
19
09
1.7
4
1207.
10
30
IO.5
-59
07
52
1.7
5
1600
10
30
13.1
-57
39
3*
1.5
6
1606
10
31
54.9
-57
11
35
3.0
B
7
1201
10
33
41.L
-59
06
47
1.5
B
0
1604
10
35
49.4
-57
27
46
1.9
29
B,DC
9
1603
IO
35
59.4
-50
02
46
2.6
B
10
1601
10
36
39.7.
-57
14
0,
2.6
B
11
1601
IO
37
17.0
-57
15 06
1.5
DC
12
303
10
39
46.1
-62
19
52
1.5
B,DC
13
,511
10 40
58.0
-56
00
13
3.0
14
,511
LO 4,
39.1
-57
43
45
1.6
B
15
1510
10
41
55.4
-57
30
7.4
2.7
DC
16
1509
10
43
50.6
-5s
04
38
2.5
B,DC
17
1506
10
44
5*.*
-57
59
04
1.5
IO
301
10
45
19.6
-61
57
35
1.7
B
19
1506
10
45
11.9
-56
15 30
2.5
DC
10
1505
10
46
26.7
-56
11
46
2.5
21
1504
10
47
58.0
_ 57
36
43
1.7
11
1503
10
46
24.9
-56
16
45
1.6
23
L50,
10
46
40.7.
-56
19
44
2.9
24
1502
10
46
47.3
-56
17
44
2.5
25
301
10
49
05.9
-61
31
43
1.5
16
1416
10
50
01.3
-57
19
49
3.0
27
211
LO 50
17.7
-6,
51
56
1.5
18
1415
10
50
36.2
-57
51
46
1.6
19
,414
I”
50
49.7.
-57
31
04
2.6
M
30
1413
10
51
27.2
-56
06
0,
1.6
B
31
111
10
51
35.7
-62
33
55
1.0
DC
32
1411
LO 57. OL.6
-57
25
L7
a.5
33
L4lO
LO 52
19.4
--I7
36
22
2.6
B
34
1409
LO 53
16.8
-57
19
4,
L.7
Y
B
35
110
10
53
43.6
-62
07
58
3.1
B
36
1407
10
54
04.3
-50
13 22
3.0
DC
37
209
10
54
06.7
-62
04
02
2.8
D
38
1406
10
54
30.4
-57
14
53
1.9
DC
39
206
10
54
40.6
-61
37
54
2.6
3A
40
1411
10
55
02.2
-56
07
42
2.6
4,
207
10
55
IS.,
-62
04
27
2.7
42
106
10
55
56.6
-67.
17
04
1.5
e
43
1405
LO 56
26.7
-56
07
41
2.6
B,D
44
1404
10
56
31.6
-57
29
05
1.7
PA
45
105
10
56
53.6
-61
15
08
1.5
XIAO Zhen and LI Jing
272
TABLE 1 (contd.)
No.
l-
DEC
RA
NAME
(1950.
0)
-
R-1
TYPE
46
204
10
57
16.6
-61
56
20
2.8
BJX
47
1402
10
57
33.3
-57
55
oa
3.1
B
41
1403
10
57
30.9
-57
34
42
2.7
B
49
203
IP
57
44.0
-6,
46
46
2.7
B.
SO
202
IO
sa
13.4
-6,
39
50
3.2
Y
St
1307
10
5a
54.2
-57
42
33
2.9
B,DC
52
60,
i0
59
16.3
-60
55
55
2.6
B
53
201
II
00
01.7
-62
la
54
2.6
I4
517
I,
00
10.3
-60
05
43
2.6
B
55
1306
11
00
32.2
-5a
28
2a
2.5
D
56
516
11
00
33.6
-6,
06
02
2.6
B
51
140
II
01
04.0
-62
16
la
2.5
58
515
11
01
06.8
-59
53
36
2.6
B
59
139
11
01
12.6
-61
29
12
2.6
M
60
514
1,
0,
41.4
-60
11
39
2.6
61
513
1,
02
09.0
-61
01
13
2.5
D
62
512
11
02
31.6
-60
59
42
1.9
H
63
137
I,
02
41.9
-6,
47
50
2.6
64
511
11
02
45.1
-60
49
25
2.6
B
65
907
L,
02
54.9
-56
46
26
2.7
DC
66
510
,I
03
11.0
-61
05
03
2.9
B
67
136
11
03
15.7
-61
12
30
2.6
B
66
906
11
03
22.3
-59
15
22
2.9
D
69
1305
11
03
29.3
-57
12
22
3.1
B
70
509
II
03
35.6
-60
35
03
2.5
M
7,
905
I,
0,
11.7
-58
28
29
2.7
72
,506
,I
04
53.5
-60
4a
24
2.7
M
73
129
1,
05
01.7
-6,
26
24
2.5
B
74
13,
L,
05
03.3
-6,
07
00
2.6
B
75
1304
11
05
26.2
-57
08
55
2.7
B
76
904
II
05
36.a
-59
16
,I
2.0
B
77
1303
11
06
31.0
-57
39
12
1.5
B
78
507
1,
06
42.9
-60
22
52
2.5
B
79
903
I,
06
43.9
-59
12
35
2.6
M
80
506
11
06
44.3
-60
39
10
2.6
B
a,
505
IL
07
,,.a
-60
53
05
2.5
M
a*
,302
I!
07
44.9
-5a
05
42
2.a
a3
902
11
08
15.6
-59
01
56
2.5
a4
901
I,
08
23.3
-59
19
26
3.1
B
a5
503
I,
06
47.4
-60
20
Ia
2.6
B,D
a6
502
I,
Oa
52.2
-59
40
04
2.6
87
106
1,
10
17.5
-6,
42
03
2.5
aa
loa
I,
10
19.4
-6,
34
34
2.5
a9
107
I,
10
21.1
-61
4,
2,
2.7
B
3.4
Infrared
273
Search
The plate centre is (1950.0 epoch) a= 10”46’, 6= -6O”OO’; 1 = 288.0*, b= -1.0’. Plate R4359 has a limiting magnitude L* 2-e auS nbc Jg&~cc u 19. Members of the galactic clusters in Carina, Tr15, NGC3324, NCC3293 and 9o 10 [4-7f rsde up the standard magnitude sequence. Image brightness measured by the CCMOS two-diaensionai digitieed scanner is expressed in units of Cosmag. For the four cluster standards, least-squares fitted calibration curves between Cosmag R and U and between Cosmag I and I had rms errors of iO.40 and fO.12, respectively. The famous nebula n Carinae is in the region, it covers alwst the whole Area 128. It is a complex comprising giant ionized regions, stellar dark nebulosity and supernova associations, galactic clusters, remrants. Its presence greatly reduced the photometric accuracy in R, but its effect on I was less. Using the VAX 11/780 computer of Beijing Observatory we counted the stars according to Cosmag R and Cosmag I down to the plate limit. The number of stars counted is 392676 on Plate R4359 and 271265 on 13932. Figs. 1 and 2 show the number magnitude distributions; the counts can be considered umplete and reliable down to Cosnag R to Rw 19.0 and ,.. -1340 and Cos=ag I _ -1040, corresponding 1~17.5. We followed the method of measuring the colour index R-I in our previous paper [2]. The criterion for identification in position is an error box of siee 6.7” x 6.7”, corresponding to a linear dimension of 1000 pm. Fig. 3 is the number distribution of the colour index; it is similar to the distributions in the Vela and Ara regions (2, 31. We again use R - I ;)r 2.5 as the criterion for infrared excess. Accordingly, we found a total of 89 infrared excess objects in this
TABLE 2 Astrometric Infrared
positions, Colour Indices and Infrared Fluxes of 12 Excess Objects identified with IRAS Point Sources (flux
density
in Jy,
L=upper limit)
NAHE
-llIO3-614111 10 21.2-61 It 23 2.670 1.020 11103-6141II 10 21.2-61 41 23 2.670 1.020 10573-6156IO 57 19.0--61S6 21 1.3300.5S3 10552-6204IO 55 16.0-62 04 17 0.4250.292L iO537-620710 53 43.9-62 07 9610.6009.040 'LO433-6157 IO 45 20.0-61 57 36 0.7550.375 10292-590910 29 lS.4-59 09 36 4.060 2.640 IIOf?-SOOS11 Of 44.7-58 05 36 0.9ll 0.391 1OS75--5751 10 57 32.9-37 Sf 0, 3.2400.9,) IDILL-5943IO 41 39.9-57 43 39 0.500 0.795 10374--171s 10 37 28.3-57 I5 07 0.666 0.961L 10302--1739 10 30 14.2-57 39 52 4.360 2.790
-
106 5.660 08.OlOL 9.72OL77.29OL 204 207 2.390 15.42OL 2fO 1.7OOL17.92OL 302
II 10 17.S 10 57 18.6 10 55 10.1 10 SJ 43.6 10 45 19.6
274
XIAO Zhen and LI Jing
area of 28.5 square degrees in Carina. TABLE 1 gives the positions and ueasured colour indices of these 89 objects. In the sane area the WAS survey lists 665 IRAS point sources. With au error box of 60" x 60" as criterion for identification[l], we had 12 identifications.The efficiency of identifyingoptical counterparts is 1.8X, a factor of 2 higher than the 0.9% we had for the Vela region. Their coordinates and identificationcharts are given TABLE 4 aud Fig. 4.
Fig. 4
The finding charts for the 12 infrared excess objects identified with IUAS point sources
ACKNOWLEDGEMENT LI Jing thanks Professor M. S. Longair for support for this work during his visit to Edinburgh and thanks R. 9. Stobie and colleagues in the Plate Library for providing the original UK Schmidt Near Infrared Survey plates and arranging the seasureseut on COSMOS.
REFERENCES [ll Joint IRAS Science Harking Group, IRAS Cataiogue of Point Sources, 1984. [2] XIAO Zhen and LI Jing, Chin.Astron.Astropbys. 12/4 8 (1988) 182-189. (1988) 304-310. = Acta Astrophys.Sin. [3] XIAO Zhen and LI Jing, Cbin.Astron.Astrophys.14/3 (1990) 289-297 = Acta Astro&ys.Sin. lOf2 (1990) 128-136. (41 Feinstein A. et al., Astron. J. 85 (1980) 708. [5] Turner D. C. et al., Astrcn. J. 85 (1980) 1193. (61 Feinstein A. et al. Publ. Astron. Sot. Pacific 92 (1980) 266. [7] Feinstein-A., Pubi. Astron. Sot. Pacific 93 (1981) 202.
A
SEARCH FOR1~
0 Pergamon Press plc Printed in Great Britain 0275-1062/91$10.00+.00
i!iiTELLAR OEMETS
IN A REGION IN WINA XIAO Zhen LI Jing Beijing Astronomical
Observatory,
Chinese Academy of
Sciences
AMTRACT This is the third paper of the series, giving the data on 89 infrared excess objects discovered in a region in Carina, of which 12 are identified with IRAS point sources.
Key words:
Photographic photometry-stellar excess objects.
colours-infrared
The aim, method and means of the present study have been set out in our two previous papers of the series [Z, 31. The present selected area is No. 128 in Carina in the UK-Schmidt Two-Coiour (R and I) Survey of Galactic Belt. The size of the region is 5.35’ x 5.35*. 5.5
..
5.0 4.5 ‘4 0 4 3.5 ‘3.0
ii:
-1700
-1500
-1300 Cosmae
Fig.
-I 100
2 Number-magnitude on I plate 13932
1 Received
-900
I
counts
1990 March 14; passed
Y
-Boo
Fig.
-600
-400
cosma‘
-200 K-1
3 Counts of colour from the plate-pair
by Referee:
1990 July
3.
0
index
2ao
Infrared
Search
271
TABLE 1 Astrometric B-binary,
Positions and Colour Indices Excess Objects in Carina
M-multiple,
D-diffuse,
DC-diffuse
of 89 Infrared around the image
NO.
NAME
I
DEC
RA (1950. 0)
R-l
TYPE DC
1
1203
LO 20
15.2
--59
09
36
1.8
7.
1609
10
10.1
-57
20
03
2.1
3
,607
10
7.9 55.0
-59
19
09
1.7
4
1207.
10
30
IO.5
-59
07
52
1.7
5
1600
10
30
13.1
-57
39
3*
1.5
6
1606
10
31
54.9
-57
11
35
3.0
B
7
1201
10
33
41.L
-59
06
47
1.5
B
0
1604
10
35
49.4
-57
27
46
1.9
29
B,DC
9
1603
IO
35
59.4
-50
02
46
2.6
B
10
1601
10
36
39.7.
-57
14
0,
2.6
B
11
1601
IO
37
17.0
-57
15 06
1.5
DC
12
303
10
39
46.1
-62
19
52
1.5
B,DC
13
,511
10 40
58.0
-56
00
13
3.0
14
,511
LO 4,
39.1
-57
43
45
1.6
B
15
1510
10
41
55.4
-57
30
7.4
2.7
DC
16
1509
10
43
50.6
-5s
04
38
2.5
B,DC
17
1506
10
44
5*.*
-57
59
04
1.5
IO
301
10
45
19.6
-61
57
35
1.7
B
19
1506
10
45
11.9
-56
15 30
2.5
DC
10
1505
10
46
26.7
-56
11
46
2.5
21
1504
10
47
58.0
_ 57
36
43
1.7
11
1503
10
46
24.9
-56
16
45
1.6
23
L50,
10
46
40.7.
-56
19
44
2.9
24
1502
10
46
47.3
-56
17
44
2.5
25
301
10
49
05.9
-61
31
43
1.5
16
1416
10
50
01.3
-57
19
49
3.0
27
211
LO 50
17.7
-6,
51
56
1.5
18
1415
10
50
36.2
-57
51
46
1.6
19
,414
I”
50
49.7.
-57
31
04
2.6
M
30
1413
10
51
27.2
-56
06
0,
1.6
B
31
111
10
51
35.7
-62
33
55
1.0
DC
32
1411
LO 57. OL.6
-57
25
L7
a.5
33
L4lO
LO 52
19.4
--I7
36
22
2.6
B
34
1409
LO 53
16.8
-57
19
4,
L.7
Y
B
35
110
10
53
43.6
-62
07
58
3.1
B
36
1407
10
54
04.3
-50
13 22
3.0
DC
37
209
10
54
06.7
-62
04
02
2.8
D
38
1406
10
54
30.4
-57
14
53
1.9
DC
39
206
10
54
40.6
-61
37
54
2.6
3A
40
1411
10
55
02.2
-56
07
42
2.6
4,
207
10
55
IS.,
-62
04
27
2.7
42
106
10
55
56.6
-67.
17
04
1.5
e
43
1405
LO 56
26.7
-56
07
41
2.6
B,D
44
1404
10
56
31.6
-57
29
05
1.7
PA
45
105
10
56
53.6
-61
15
08
1.5
XIAO Zhen and LI Jing
272
TABLE 1 (contd.)
No.
l-
DEC
RA
NAME
(1950.
0)
-
R-1
TYPE
46
204
10
57
16.6
-61
56
20
2.8
BJX
47
1402
10
57
33.3
-57
55
oa
3.1
B
41
1403
10
57
30.9
-57
34
42
2.7
B
49
203
IP
57
44.0
-6,
46
46
2.7
B.
SO
202
IO
sa
13.4
-6,
39
50
3.2
Y
St
1307
10
5a
54.2
-57
42
33
2.9
B,DC
52
60,
i0
59
16.3
-60
55
55
2.6
B
53
201
II
00
01.7
-62
la
54
2.6
I4
517
I,
00
10.3
-60
05
43
2.6
B
55
1306
11
00
32.2
-5a
28
2a
2.5
D
56
516
11
00
33.6
-6,
06
02
2.6
B
51
140
II
01
04.0
-62
16
la
2.5
58
515
11
01
06.8
-59
53
36
2.6
B
59
139
11
01
12.6
-61
29
12
2.6
M
60
514
1,
0,
41.4
-60
11
39
2.6
61
513
1,
02
09.0
-61
01
13
2.5
D
62
512
11
02
31.6
-60
59
42
1.9
H
63
137
I,
02
41.9
-6,
47
50
2.6
64
511
11
02
45.1
-60
49
25
2.6
B
65
907
L,
02
54.9
-56
46
26
2.7
DC
66
510
,I
03
11.0
-61
05
03
2.9
B
67
136
11
03
15.7
-61
12
30
2.6
B
66
906
11
03
22.3
-59
15
22
2.9
D
69
1305
11
03
29.3
-57
12
22
3.1
B
70
509
II
03
35.6
-60
35
03
2.5
M
7,
905
I,
0,
11.7
-58
28
29
2.7
72
,506
,I
04
53.5
-60
4a
24
2.7
M
73
129
1,
05
01.7
-6,
26
24
2.5
B
74
13,
L,
05
03.3
-6,
07
00
2.6
B
75
1304
11
05
26.2
-57
08
55
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Infrared
273
Search
The plate centre is (1950.0 epoch) a= 10”46’, 6= -6O”OO’; 1 = 288.0*, b= -1.0’. Plate R4359 has a limiting magnitude L* 2-e auS nbc Jg&~cc u 19. Members of the galactic clusters in Carina, Tr15, NGC3324, NCC3293 and 9o 10 [4-7f rsde up the standard magnitude sequence. Image brightness measured by the CCMOS two-diaensionai digitieed scanner is expressed in units of Cosmag. For the four cluster standards, least-squares fitted calibration curves between Cosmag R and U and between Cosmag I and I had rms errors of iO.40 and fO.12, respectively. The famous nebula n Carinae is in the region, it covers alwst the whole Area 128. It is a complex comprising giant ionized regions, stellar dark nebulosity and supernova associations, galactic clusters, remrants. Its presence greatly reduced the photometric accuracy in R, but its effect on I was less. Using the VAX 11/780 computer of Beijing Observatory we counted the stars according to Cosmag R and Cosmag I down to the plate limit. The number of stars counted is 392676 on Plate R4359 and 271265 on 13932. Figs. 1 and 2 show the number magnitude distributions; the counts can be considered umplete and reliable down to Cosnag R to Rw 19.0 and ,.. -1340 and Cos=ag I _ -1040, corresponding 1~17.5. We followed the method of measuring the colour index R-I in our previous paper [2]. The criterion for identification in position is an error box of siee 6.7” x 6.7”, corresponding to a linear dimension of 1000 pm. Fig. 3 is the number distribution of the colour index; it is similar to the distributions in the Vela and Ara regions (2, 31. We again use R - I ;)r 2.5 as the criterion for infrared excess. Accordingly, we found a total of 89 infrared excess objects in this
TABLE 2 Astrometric Infrared
positions, Colour Indices and Infrared Fluxes of 12 Excess Objects identified with IRAS Point Sources (flux
density
in Jy,
L=upper limit)
NAHE
-llIO3-614111 10 21.2-61 It 23 2.670 1.020 11103-6141II 10 21.2-61 41 23 2.670 1.020 10573-6156IO 57 19.0--61S6 21 1.3300.5S3 10552-6204IO 55 16.0-62 04 17 0.4250.292L iO537-620710 53 43.9-62 07 9610.6009.040 'LO433-6157 IO 45 20.0-61 57 36 0.7550.375 10292-590910 29 lS.4-59 09 36 4.060 2.640 IIOf?-SOOS11 Of 44.7-58 05 36 0.9ll 0.391 1OS75--5751 10 57 32.9-37 Sf 0, 3.2400.9,) IDILL-5943IO 41 39.9-57 43 39 0.500 0.795 10374--171s 10 37 28.3-57 I5 07 0.666 0.961L 10302--1739 10 30 14.2-57 39 52 4.360 2.790
-
106 5.660 08.OlOL 9.72OL77.29OL 204 207 2.390 15.42OL 2fO 1.7OOL17.92OL 302
II 10 17.S 10 57 18.6 10 55 10.1 10 SJ 43.6 10 45 19.6
274
XIAO Zhen and LI Jing
area of 28.5 square degrees in Carina. TABLE 1 gives the positions and ueasured colour indices of these 89 objects. In the sane area the WAS survey lists 665 IRAS point sources. With au error box of 60" x 60" as criterion for identification[l], we had 12 identifications.The efficiency of identifyingoptical counterparts is 1.8X, a factor of 2 higher than the 0.9% we had for the Vela region. Their coordinates and identificationcharts are given TABLE 4 aud Fig. 4.
Fig. 4
The finding charts for the 12 infrared excess objects identified with IUAS point sources
ACKNOWLEDGEMENT LI Jing thanks Professor M. S. Longair for support for this work during his visit to Edinburgh and thanks R. 9. Stobie and colleagues in the Plate Library for providing the original UK Schmidt Near Infrared Survey plates and arranging the seasureseut on COSMOS.
REFERENCES [ll Joint IRAS Science Harking Group, IRAS Cataiogue of Point Sources, 1984. [2] XIAO Zhen and LI Jing, Chin.Astron.Astropbys. 12/4 8 (1988) 182-189. (1988) 304-310. = Acta Astrophys.Sin. [3] XIAO Zhen and LI Jing, Cbin.Astron.Astrophys.14/3 (1990) 289-297 = Acta Astro&ys.Sin. lOf2 (1990) 128-136. (41 Feinstein A. et al., Astron. J. 85 (1980) 708. [5] Turner D. C. et al., Astrcn. J. 85 (1980) 1193. (61 Feinstein A. et al. Publ. Astron. Sot. Pacific 92 (1980) 266. [7] Feinstein-A., Pubi. Astron. Sot. Pacific 93 (1981) 202.