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HQM is an optical broad-band photometric monitoring program carried out since September 1988. We use a CCD camera at the MPIA 1.2$\,$m telescope. Fully automatic photometric reduction relative to stars in the frames is done within a few minutes after each exposure, thus interesting brightness changes can be followed in detail. The typical photometric error is 1--2\,\% for a 17.5\,mag quasar. We here present lightcurves of 14 known violently variable sources and compare them with literature data. For two BL\,Lac objects, 1E\,1229+645 and 4C\,56.27 (1823+568), this paper is the first variability study. We have also carried out POSS photometry to obtain indications for variability on a longer timescale., Comment: 10 pages, Latex laa-Style (A&A 1990), Astron. & Astrophys (Supplements) in press, HH-HQM-JS-94-3

HQM is an optical broad-band photometric monitoring program carried out since September 1988. We use a CCD camera at the MPIA 1.2$\,$m telescope. Fully automatic photometric reduction relative to stars in the frames is done within a few minutes after each exposure, thus interesting brightness changes can be followed in detail. The typical photometric error is 1--2\,\% for a 17.5\,mag quasar. We here present lightcurves of 14 known violently variable sources and compare them with literature data. For two BL\,Lac objects, 1E\,1229+645 and 4C\,56.27 (1823+568), this paper is the first variability study. We have also carried out POSS photometry to obtain indications for variability on a longer timescale., Comment: 10 pages, Latex laa-Style (A&A 1990), Astron. & Astrophys (Supplements) in press, HH-HQM-JS-94-3