All Figures

Figure 1: a) Differential counts for simulated uniform space distribution. Dots: no measurement error. Open circles: errors with  mag. The straight line has the slope 0.6. At faint magnitudes the counts with error in the measured magnitudes become artificially distorted. The Eddington bias is seen at magnitudes brighter than 15.5. b) Counts for uniform space distribution. Open circles: measurement errors with randomly chosen , or 0.9 mag. Triangles: The measured magnitude of each galaxy is changed by the Eddington shift, then counted. The solid line is the initial regression line as in  a).

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In the text

	Figure 2: vs. m diagrams showing differential counts for a simulated space distribution thinning outwards with D = 2.2. The relation with the slope 0.44 was generated with no measurement error. The behaviour of  is shown at the bottom of the diagrams. In  a)  increases linearly. In  b) a constant  is followed by an exponential increase.
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In the text

	Figure 3: vs. m diagrams showing differential counts for a uniform space distribution. Dots mean no measurement error. Other symbols refer to errors increasing as in Fig. 2b.
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In the text

	Figure 4: a) The counts within 10 < B < 16 for the all-sky LEDA galaxies with deg. Those with assigned (triangle) and (open circle) have been shown separately. b) The counts after each galaxy has been Eddington shifted, using the slope = 0.44. The sum of the counts follows tightly the slope 0.44 above B = 10.5 up to 13.5. For problematic fainter magnitudes we show the uncorrected total counts.
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In the text