Astron. Astrophys. 350, 379-380 (1999)

3. Results

The inspection of our spectra revealed broad emission lines typical for non-stellar objects (Figs. 1-3). However, an analysis of the FWHMs, in both the DSS frames and our photometric data, yielded point source characteristics for all three targets, letting us suspect a QSO nature. Also the measured color indices (Table 2) show values typical for quasars. The redshifts have been measured from several emission lines after identifying one reference emission line in each spectrum. The remaining lines were identified afterwards based on the comparison with the known rest wavelengths for the one low- and the two intermediate-redshifted objects (see Table 2).

Fig. 1. Spectrum of CTCV J0322-4653. Telluric features are marked by .

Fig. 2. Spectrum of CTCV J1322-2101. Telluric features are marked by .

Fig. 3. Spectrum of CTCV J 1329-1920. Telluric features are marked by , additional artifacts are marked by .

Table 2. Positions, photometrically and spectrophotometrically derived magnitudes¹, color-indices, and derived redshifts

For the low redshift QSO, CTCV J1322-2101, only an R magnitude could be determined due to the limited spectral range covered. However, assuming an upper color limit of 0.4, this indicates that the object is probably brighter than 23.

Motivated by the low redshift value of CTCV J 1322-2101, additional near-infrared data were obtained in the K´ band in order to check whether the host galaxy could be detected. No evidence for any extended emission around the object at the level of sensitivity was found. Furthermore, the measured FWHM from the photometry was consistent with stellar values and much smaller than the FWHM of the faint galaxy that is located SE of the QSO.

From all studied quasars discovered by the Calán-Tololo objective prism survey, only very few quasars with redshifts 0.3 have been found. Our finding would be the only high-luminosity quasar () with 0.2 in this survey (Maza et al. 1996, and references therein).

© European Southern Observatory (ESO) 1999

Online publication: October 4, 1999
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