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2. Data acquisition and reduction

In August 1991 and August 1994, 8 echelle observations of the quasar PKS 2126-158 were obtained at ESO (La Silla), with the NTT telescope and the EMMI instrument (see D'Odorico 1990). The ESO echelle #10 was used in the red arm of the instrument in combination with a grism cross-disperser. The seeing during the observations was typically between 0.8 and 1.3 arcsec.

The absolute flux calibration was carried out by observing the standard star EG274 (Stone & Baldwin 1983).

The data have been reduced in the context of the ECHELLE software package available in the 94NOV edition of MIDAS, the ESO data reduction system. Some improvements have been introduced with respect to the standard procedure. In particular, the spectra obtained from different observations are summed up without a previous rebinning but maintaining the original pixel sampling. For the wavelength calibration Thorium lamp spectra have been used. Wavelengths have then been corrected to vacuum heliocentric.

The weighted mean of the spectra is equivalent to
tex2html_wrap_inline2087 hours of integration time and it presents a resolution tex2html_wrap_inline1965. The s/n ratio per resolution element at the continuum level is doubled compared with the previous spectrum by GCFT: it ranges from tex2html_wrap_inline2093 to 44 in the interval 4380-5190 Å, while beyond the Lytex2html_wrap_inline1969 emission it has a roughly constant value of tex2html_wrap_inline2101.

In addition to these data, 8 long slit observations of the spectrum of PKS 2126-158 were obtained with an holographic grating (ESO #11) at the blue arm of the EMMI instrument. The reduction has been carried out with the LONG SLIT package of MIDAS, using an optimal extraction option. The resolution of these data is tex2html_wrap_inline2105.

The resulting spectrum has been used to check the reliability of the Lytex2html_wrap_inline1969 identification process by verifying the presence of the higher order Lyman series lines.

The journal of the observations is given in Table 1 (click here).

   

date exposure slit range CCD
(yy mm dd) (s) width (Å)
91 08 06 7200 tex2html_wrap_inline2109 4539-7055 FORD 2k
91 08 06 7200 tex2html_wrap_inline2109 4539-7055 FORD 2k
91 08 07 9130 tex2html_wrap_inline2109 4539-7055 FORD 2k
94 08 13 5380 tex2html_wrap_inline2121 4056-6635 TK 2k #36
94 08 13 7200 tex2html_wrap_inline2121 4056-6635 TK 2k #36
94 08 13 7200 tex2html_wrap_inline2121 4056-6635 TK 2k #36
94 08 15 7200 tex2html_wrap_inline2133 4279-6644 TK 2k #36
94 08 15 6645 tex2html_wrap_inline2133 4279-6644 TK 2k #36
94 08 14 2700 tex2html_wrap_inline2133 3822-3980 TK 1k #31
94 08 14 2700 tex2html_wrap_inline2121 3822-3980 TK 1k #31
94 08 14 2700 tex2html_wrap_inline2121 3686-3846 TK 1k #31
94 08 14 2700 tex2html_wrap_inline2121 3686-3846 TK 1k #31
94 08 15 3600 3825-3983 TK 1k #31
94 08 15 3600 3825-3983 TK 1k #31
94 08 15 3600 3687-3848 TK 1k #31
94 08 15 3000 3687-3848 TK 1k #31
Table 1: Journal of the observations


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