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Spectroscopy of 11 QSO candidates
Chin.Astron.Astrophys.9 (1985)343-346 2 /l?f85l 291293
Pergamon Press. Printed in Great Britain 02751062/85$10.00+.00
Act.Astrophys.Sin.
SPECTROSCOPY
OF 11 QSO CANDIDATES*
CHEN Jian-sheng
Beijing
Observatory,
Academia
Sinica
ABSTRACT Eleven QSO candidates have been confirmed from the UKST prism plate of the field 0112-35. Their redshifts, finding charts and the spectra are presented. Among these IIQSOs, 6 are in 3 pairs with angular separation less than 4 arcmin; one is in a QSO-galaxy pair.
1.
INTRODUCTION
An objective -prism plate of the field 011235 was recently obtained and examined for QSO candidates by Savage et al. (1984). We were interested in some of these candidates, in particular, as possible members of close QSO pairs and QSO-galaxy pairs. These are of special interest in absorption line studies (e.g. Shaver and Robertson, 1983; Boksenberg, A. and Sargent, W.L.W. 1978). We obtained spectra of several of the QSO candidates listed in Savage et al. (1984), and of other objects on the plates, some of which lie outside the area scanned by Savage etal. 11 QSOs have been confirmed and their spectra and redshifts are given in this paper.
2.
OBSERVATIONS AND RESULTS
The observations were made in September and October 1982 and October 1983 with the 3.6mtelescope atoLa Silla, and the IDS. A dispersion of 224A/mm was used, which, with an aperture of 2", resulted in a spectral resolution of 13- 15 A(FWHM). 11 of the QSO candidates have been confirmed as QSOs. They are listed in TABLE 1, and their spectra are shown in Plate 1. The quoted redshifts are accurate to 0.001 (rms). Five of them were not listed by Savage et al., so their finding charts are given here (Plate 2). One of these objects listed by Savage et al. does not appear to be a QSO: 0101-351. Among these11 QSOs there are 3 QSO pairs with separations less than 4 arcmin. One QSO-galaxy pair and a single QSO with rich absorption lines.
3.
COMMENTS ON INDIVIDUAL OBJECTS
0059-3450 and 0059-3456 A projected QSO pair separated by 190". 0059-3450 shows emission lines of MgII, [OII],Hg,Hy, Ho and [OBI] and 0059-3456 shows CIV, CIIIand M&I. 0100-351 A projected QSO-galaxy pair with separation of 10". The spectrum shows CID and MGIIemission lines. 0105-338 and 0105-3384 A projected QSO pair with separation of 210". 0105-338 shows CIIIand CIV emission lines while 0105-3384 shows ICYCIV, CJIIemission lines. 0106-350 The emission lines identified are CIV and CID. 0107-3310 Many strong emission lines: MgVB, M@ > strong Balmer lines and [OIII]. 0109-355 Emission lines include Ta+NV, SiIV, CIV and CID. The QSO is connected by a fuzzy object to the south-east which has no emission feature from the observation of 3.9mAAT IPCS and RGO spectrograph and shows to be a faint forground star from ES0 1.5m CCD observation. 0114-332 and 0114-331 A projected QSO pair with separation of 142", 0114-332 shows CIV, ClIIand MgIIemission lines and 0114-331 shows La and CIV emission lines. 0121-329 The emission lines identified are La+NV+CIV, and CBI. Many strong absorption lines in the long wavelength side of Lo emission are clearly seen from this low resolution spectrum.
ACKNOWLEDGEMENTS J.S. Chen acknowledges the hospitality of the European Southern Observatory during the year 1982-83 and Dr. *Based on UK Schmidt Telescope prism plate and observations made at the European Southern Observatory, La Silla, Chile.
CHEN
344
TABLE 1 Name
Confirmed
QSOs
Posotion (1950.0)
Comments
z
0059-3450*
00659-35t3
-34”30’
0059-3456*
00 59 35.9
-34 33 25
1.623
OlOO-351* 0105-338
01 00 46.3 01 05 15.0
-35 06 22 -33 49 17
1.413 I.898
0105-3384’
01 05 31.0
-33 50 21
2.437
0106-350
01 06 59.1
-35 01 18
2.000
13”
lll’p5
0.427
0107-3310
01 07 58.0
-33 06 06
0.472
0109-355*
01 09 07.5
-35 31 23
2.307
0114-332
01 14 43.2
-33
12 33
1.624
0114-331
01 14 53.2
-33
11 27
2.181
0121-329
01 21 18.1
-32 54 08
2.325
19?5 VSO-gnlaxj (separation
19f3
19rnE
REFERENCES [l]
Boksenberg,
[2]
Savage,
A., A.,
Sargent,
Trew,
up. J.,
W.L.W.,
A.S.,
Chen,
Robertson,
J.G.,
J-S.,
220
Weston,
(1978), A.,
42.
M.N.R.A.S.,
207
(1984), 393. [3]
Shaver,
O.V.,
Italiana,
54 (1983),
664.
Memorie
pair7 10”)
della Sociata
Astronomica
19?0
Quasar
345
Candidates
0059-3456
0
1
0105-3384
F ‘-0 In
/
1
I
I
0107-3310
1
/
“r-xi&-
4000
I
6000
,
0121-329
I
4000
6000
1
I
4000
WAVELFNGlH i!+,
Plate
1
IDS spectra QSOs
of the confirmed
I
6000
I
346
MEN
Plate 2
Finding charts for the QSOs in TABLE 1
which were not listed by Savage et al. (1984). The charts were made from the long exposure UKST plates; each chart is 7 arcmin square with north to the top and east to the right
Pergamon Press. Printed in Great Britain 02751062/85$10.00+.00
Act.Astrophys.Sin.
SPECTROSCOPY
OF 11 QSO CANDIDATES*
CHEN Jian-sheng
Beijing
Observatory,
Academia
Sinica
ABSTRACT Eleven QSO candidates have been confirmed from the UKST prism plate of the field 0112-35. Their redshifts, finding charts and the spectra are presented. Among these IIQSOs, 6 are in 3 pairs with angular separation less than 4 arcmin; one is in a QSO-galaxy pair.
1.
INTRODUCTION
An objective -prism plate of the field 011235 was recently obtained and examined for QSO candidates by Savage et al. (1984). We were interested in some of these candidates, in particular, as possible members of close QSO pairs and QSO-galaxy pairs. These are of special interest in absorption line studies (e.g. Shaver and Robertson, 1983; Boksenberg, A. and Sargent, W.L.W. 1978). We obtained spectra of several of the QSO candidates listed in Savage et al. (1984), and of other objects on the plates, some of which lie outside the area scanned by Savage etal. 11 QSOs have been confirmed and their spectra and redshifts are given in this paper.
2.
OBSERVATIONS AND RESULTS
The observations were made in September and October 1982 and October 1983 with the 3.6mtelescope atoLa Silla, and the IDS. A dispersion of 224A/mm was used, which, with an aperture of 2", resulted in a spectral resolution of 13- 15 A(FWHM). 11 of the QSO candidates have been confirmed as QSOs. They are listed in TABLE 1, and their spectra are shown in Plate 1. The quoted redshifts are accurate to 0.001 (rms). Five of them were not listed by Savage et al., so their finding charts are given here (Plate 2). One of these objects listed by Savage et al. does not appear to be a QSO: 0101-351. Among these11 QSOs there are 3 QSO pairs with separations less than 4 arcmin. One QSO-galaxy pair and a single QSO with rich absorption lines.
3.
COMMENTS ON INDIVIDUAL OBJECTS
0059-3450 and 0059-3456 A projected QSO pair separated by 190". 0059-3450 shows emission lines of MgII, [OII],Hg,Hy, Ho and [OBI] and 0059-3456 shows CIV, CIIIand M&I. 0100-351 A projected QSO-galaxy pair with separation of 10". The spectrum shows CID and MGIIemission lines. 0105-338 and 0105-3384 A projected QSO pair with separation of 210". 0105-338 shows CIIIand CIV emission lines while 0105-3384 shows ICYCIV, CJIIemission lines. 0106-350 The emission lines identified are CIV and CID. 0107-3310 Many strong emission lines: MgVB, M@ > strong Balmer lines and [OIII]. 0109-355 Emission lines include Ta+NV, SiIV, CIV and CID. The QSO is connected by a fuzzy object to the south-east which has no emission feature from the observation of 3.9mAAT IPCS and RGO spectrograph and shows to be a faint forground star from ES0 1.5m CCD observation. 0114-332 and 0114-331 A projected QSO pair with separation of 142", 0114-332 shows CIV, ClIIand MgIIemission lines and 0114-331 shows La and CIV emission lines. 0121-329 The emission lines identified are La+NV+CIV, and CBI. Many strong absorption lines in the long wavelength side of Lo emission are clearly seen from this low resolution spectrum.
ACKNOWLEDGEMENTS J.S. Chen acknowledges the hospitality of the European Southern Observatory during the year 1982-83 and Dr. *Based on UK Schmidt Telescope prism plate and observations made at the European Southern Observatory, La Silla, Chile.
CHEN
344
TABLE 1 Name
Confirmed
QSOs
Posotion (1950.0)
Comments
z
0059-3450*
00659-35t3
-34”30’
0059-3456*
00 59 35.9
-34 33 25
1.623
OlOO-351* 0105-338
01 00 46.3 01 05 15.0
-35 06 22 -33 49 17
1.413 I.898
0105-3384’
01 05 31.0
-33 50 21
2.437
0106-350
01 06 59.1
-35 01 18
2.000
13”
lll’p5
0.427
0107-3310
01 07 58.0
-33 06 06
0.472
0109-355*
01 09 07.5
-35 31 23
2.307
0114-332
01 14 43.2
-33
12 33
1.624
0114-331
01 14 53.2
-33
11 27
2.181
0121-329
01 21 18.1
-32 54 08
2.325
19?5 VSO-gnlaxj (separation
19f3
19rnE
REFERENCES [l]
Boksenberg,
[2]
Savage,
A., A.,
Sargent,
Trew,
up. J.,
W.L.W.,
A.S.,
Chen,
Robertson,
J.G.,
J-S.,
220
Weston,
(1978), A.,
42.
M.N.R.A.S.,
207
(1984), 393. [3]
Shaver,
O.V.,
Italiana,
54 (1983),
664.
Memorie
pair7 10”)
della Sociata
Astronomica
19?0
Quasar
345
Candidates
0059-3456
0
1
0105-3384
F ‘-0 In
/
1
I
I
0107-3310
1
/
“r-xi&-
4000
I
6000
,
0121-329
I
4000
6000
1
I
4000
WAVELFNGlH i!+,
Plate
1
IDS spectra QSOs
of the confirmed
I
6000
I
346
MEN
Plate 2
Finding charts for the QSOs in TABLE 1
which were not listed by Savage et al. (1984). The charts were made from the long exposure UKST plates; each chart is 7 arcmin square with north to the top and east to the right