Table 2: The scaleheights of the thin disk, assuming a scalelength of $h_r=2.0~ {\rm kpc})$ and $h_1(h_r=3.5~ {\rm kpc})$ , respectively. The numbers in brackets are the corresponding values of $\chi ^2$ .
CADIS field $h_1(h_r=2.0 {\rm kpc})$ $h_1(h_r=3.5 {\rm kpc})$

1 h $249\pm25$ (0.92) $255\pm26$ (0.92)

9 h $336\pm40$ (1.21) $312\pm35$ (1.21)

13 h $249\pm24$ (0.62) $255\pm25$ (0.63)

16 h $321\pm33$ (0.41) $319\pm32$ (0.41)

23 h $319\pm33$ (1.23) $317\pm33$ (1.21)

**Table 2:** The scaleheights of the thin disk, assuming a scalelength of $h_r=2.0~ {\rm kpc})$ and $h_1(h_r=3.5~ {\rm kpc})$ , respectively. The numbers in brackets are the corresponding values of $\chi ^2$ .
CADIS field	$h_1(h_r=2.0 {\rm kpc})$	$h_1(h_r=3.5 {\rm kpc})$
1 h	$249\pm25$ (0.92)	$255\pm26$ (0.92)
9 h	$336\pm40$ (1.21)	$312\pm35$ (1.21)
13 h	$249\pm24$ (0.62)	$255\pm25$ (0.63)
16 h	$321\pm33$ (0.41)	$319\pm32$ (0.41)
23 h	$319\pm33$ (1.23)	$317\pm33$ (1.21)

Source LaTeX | All tables | In the text

	1 Introduction
	2 The Calar Alto Deep Imaging Survey
	3 The stellar density distribution
	4 Star counts - a direct measurement
	5 A Monte Carlo model of the Milky Way
	6 Summary and discussion
	References