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The Bochum Milky Way Surface Photometry: An Overview

  • Theodor Schmidt-Kaler (a1)

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Photoelectric photometry is inherently much more accurate than photographic work. But large time variations of airglow, inaccurate elimination of bright stars, and the problematic adding-up of different scans may destroy this advantage in the case of surface photometry. On the other hand, the low internal accuracy of photographic photometry and its problematic nonlinearity can be overcome by a sufficient number of plates and by careful photoelectric calibrations. Such measures allow us to take full advantage of the high homogeneity of super-wide-angle photographs over extremely large areas, their global calibration, and their direct imaging. When I started this work, no charge-coupled device or similar device was available. But even today, with such detectors problems would arise for surface photometry in flat-fielding, zero-points, and bright star elimination. Our camera (Schlosser and Schmidt-Kaler 1977) followed the Henyey-Greenstein design with a f/4.3 Zeiss UV-Sonnar lens (with constant focus from 2000 Å up to 10000 Å) and f/0.4 spherical mirror of 30 cm ⊘, giving an effective f=18 mm. The angular resolution, limited by optics and plate, is 4′ in the center, 7′ in the average, and about 20′ at the edges of the field of view (=140°).

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References

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Hoffmann, B., Kimeswenger, S., Schlosser, W., Schmidt-Kaler, Th., Seidensticker, K. J. 1989, in Proc. IAU 139, Galactic and Extragalactic Background Radiation, ed. Bowyer, S. and Leinert, Ch., Dordrecht, Kluwer Academic Pulisher.
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The Bochum Milky Way Surface Photometry: An Overview

  • Theodor Schmidt-Kaler (a1)

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