{'fraction_non_alphanumeric': 0.028808380619816675, 'fraction_numerical': 0.01920558707987778, 'mean_word_length': 4.7443609022556394, 'pattern_counts': {'":': 0, '<': 0, '<?xml version=': 0, '>': 0, 'https://': 0, 'lorem ipsum': 0, 'www.': 0, 'xml': 0}, 'pii_count': 0, 'substrings_counts': 0, 'word_list_counts': {'cursed_substrings.json': 0, 'profanity_word_list.json': 0, 'sexual_word_list.json': 0, 'zh_pornsignals.json': 0}}
The new gravitational lens candidate Q 1208+1011 and the importance of high quality data.

The ESO Key Programme "Gravitational Lensing: Quasars and Radio Galaxies" has been described by Surdej et al., 1989. One of the aims of this programme consists in identifying multiply imaged sources within a large sample of highly luminous quasars (HLQs). Indeed, both the so-called magnification bias and the redshift dependence of the optical depth for lensing point towards apparently bright and very distant objects as the best gravitational lens candidates. For this purpose, we acquire CCD images of these objects (hopefully under good seeing conditions) and carefully inspect the recorded frames, in search for multiple components or galaxies superimposed on the quasar image. This visual inspection is, however, only a first step: we have now begun a systematic analysis of these CCD images using more sophisticated imageprocessing techniques, including deconvolution and point-spread function (PSF) subtraction. Up to now, we have analysed a sample of 153 quasars for which R-band images had been obtained. Most of these data come from the direct CCD camera at the 2.2-m telescope, from EFOSC at the 3.6-m and from the direct camera which was mounted at the N T during its test period. Some of the results have been presented in September 1991 by Magain et al. (1992a) while a more complete statistical evaluation of gravitational lensing effects on HLQ images is in preparation (Surdej at al. 1992b). The histogram of the image full width at half maximum (FWHM) is illustrated in Figure 1 for the 153 objects considered. The sharp peak at 0.7 arcsec corresponds to observations carried out at the ESO NlT, observations which took place only when the seeing was very good. The observations obtained during our regular observing runs correspond to the broader peak around 1.2 arcsec. The average seeing FWHM amounts to 1.0 arcsec for the whole sample. These 153 HLQs were systematically inspected visually, in search for possible nonstellar images (extension, fuzz, . . .) or for companions, either stellar or diffuse. In addition, the PSF was subtracted from the quasar image whenever possible. The residuals were then examined for a possible superposition of a galaxy or of a stellar image.