By Gilbert Morgan Smith; et al
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At moderate resolution, the detections become more limited by detector noise, in which case increasing integration times would improve the detection limit. Restricting to times less than one hour, moderate resolution limits are about 5 mJy from 10 to 100 /xm. 7 Conclusions When the array of instruments described above arefinallyavailable for routine astronomical use, we can expect no more technological breakthroughs that will provide order of magnitude improvements. It was such large advances in one step that provided the motivations for going from single dish radio telescopes to the VLA, from VLBI to VLBA, from IUE to HST, from 4 m telescopes to NGTs, from HEAO to AXAF, and from IRAS to SIRTF.
Such a survey is especially sensitive to the blazars, or optically violent variables, which are quasar analogs to BL Lac objects. It appears that the relative number of quasars in this category is small (Impey & Brand 1982), even though their detectability is enhanced by beaming effects (Chapter 7). The great promise of surveys for variable quasars is to find enough that it will be possible to learn how quasar properties differ as a function of their variability. This is necessary to study the variability models properly, including possible effects of gravitational lensing (Chapter 4).
5 in the number of quasars found! So do not be harsh with observers whose results have large error bars. Even with a perfect detector, perfect skies, and perfect astronomer, another indeterminate source of uncertainty is also present. This is the obscuration of quasars by dust in our Galaxy, where obscuration varies as a function of position. Canonical formulae exist to take out this 'galactic extinction' as a function of position in the sky (Burstein & Heiles 1978). These results show that extinction can exist for quasars at a level up to a few tenths of a magnitude, introducing an uncertainty in quasar counts comparable to that discussed above.
A textbook of general botany by Gilbert Morgan Smith; et al