A QSO survey via optical variability and zero proper motion in the M 92 field. I. QSO candidates and selection effects

Details A QSO survey via optical variability and zero proper motion in the M 92 field. I. QSO candidates and selection effects A QSO survey via optical variability and zero proper motion in the M 92 field. I. QSO candidates and selection effects

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...373...38b&link_type=abstract

Astronomy and Astrophysics, v.373, p.38-55 (2001)

Statistics

10

Galaxies: Active, Galaxies: Seyfert, Galaxies: Statistics, Quasars: General, Globular Clusters: Individual: M 92

Scientific paper

The combination of variability and proper motion constraints (VPM search) is believed to provide an unconventional yet efficient search strategy for QSOs with selection effects quite different from conventional optical QSO surveys. Previous studies in a field of high galactic latitude have shown that the VPM method is indeed an efficient search strategy. In the present paper, we describe a further variability-proper motion (VPM) QSO survey on Tautenburg Schmidt plates. The survey is based on an exceptionally large number of 162 B plates centred on M 92 with a time-baseline of more than three decades. Further U and V plates are used to measure time-averaged colour indices, and morphology is evaluated on a deep R plate. Proper motions with Hipparcos -like accuracies as well as variability indices are derived for about 35 000 star-like objects down to B=20.5. With regard to both the number of plates and the number of objects to be investigated, this is the largest VPM survey performed so far. The present paper is focused on the description of the observational material, the data reduction, the definition of the selection parameters, and the construction of the QSO candidate sample. Furthermore, the selection effects of the VPM-method are discussed a priori. For the present survey, the selection effects are shown to be dominated by the magnitude-dependence of the photometric accuracy. Down to the limiting magnitude of the survey B_lim=19.7, we identify 62 high-priority QSO candidates and a further 57 candidates of medium priority. Spectroscopic follow-up observations have been performed for all these candidates as well as for additional selected candidates of lower priority; the confirmed QSOs will be presented and discussed in a forthcoming paper. Based on observations made with the 2~m telescope of the Thüringer Landessternwarte Tautenburg.

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