3 Measurements

The measurement lasted for approximately 15 minutes for each star observed.
The principle of the measurements is called *point run* which is
normally used as an angular adjusting procedure for the telescope. For such a
point run a certain area of the camera is covered with a prechosen
virtual point grid. On each coordinate of this grid the star is
subsequently focused and the anode current of each photomultiplier
is read out and recorded. At the beginning and at the end of
such runs, the central pixel is pointed to the star.
In this pilot study stars were only projected onto approximately
15 photomultiplier tubes of the central region of the camera. The
grid had a dimension of 15 15 points. Covering the whole camera
surface by the calibration procedure is a trivial problem of more
measuring time.
The selected stars (see Sect. 2) which have been used and some
characteristic data are listed in Table 1.

Flamsteed/Bayer | HR No. | Right | Declination | Spectral | Effective | ||

Designation | Ascension | Type | Temperature | ||||

4 |
CrB | 5778 |
15^{h} 32^{m} 44.9^{s} |
B6 Vnn | 14000 K | ||

22 | Her | 6092 |
16^{h} 19^{m} 36.3^{s} |
B5 IV | 15000 K | ||

68 | Her | 6431 |
17^{h} 17^{m} 19.4^{s} |
B3 III | 17000 K | ||

85 | Her | 6588 |
17^{h} 39^{m} 20.3^{s} |
B3 IV | 19000 K | ||

67 | Oph | 6714 |
18^{h} 00^{m} 25.2^{s} |
B5 Ib | 13500 K | ||

102 | Her | 6787 |
18^{h} 08^{m} 34.0^{s} |
B2 IV | 21000 K | ||

10 | Lyr | 7106 |
18^{h} 49^{m} 54.8^{s} |
B7 Vpe (shell) | 13000 K | ||

20 | Lyr | 7298 |
19^{h} 13^{m} 36.3^{s} |
B2.5 IV | 19000 K | ||

8 | Cyg | 7426 |
19^{h} 31^{m} 36.3^{s} |
B3 IV | 18000 K | ||

12 | Vul | 7565 |
19^{h} 51^{m} 04.0^{s} |
B2.5 Ve | 19000 K | ||

59 | v832 | Cyg | 8047 |
20^{h} 59^{m} 40.4^{s} |
B1.5 Vnne | 23000 K | |

66 | Cyg | 8146 |
21^{h} 17^{m} 44.0^{s} |
B2 Ve | 22000 K | ||

10 | Lac | 8622 |
22^{h} 39^{m} 03.5^{s} |
O9 V | 33000 K | ||

81 | Cyg | 8335 |
21^{h} 46^{m} 37.6^{s} |
B2.5 III | 18000 K |

Copyright The European Southern Observatory (ESO)