2MASS wide field extinction maps - III. The Taurus, Perseus, and California cloud complexes

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Table 1:

The average value of foreground stars found in the various complexes.
Complex	$N_{\rm fg}$	Area	$\rho_{\rm fg}$	Distance	VLBI Distance
		$\mbox{deg}^2$	$\mbox{deg}^{-2}$	pc	pc
Taurus	75	1.829	$\phantom{0}41 \pm 4\phantom{0}$	$153 \pm 8\phantom{0}$	$147.6 \pm 0.6$
Perseus	71	0.638	$111 \pm 13$	$240 \pm 13$	$235 \pm 18$
Perseus North	45	0.336	$134 \pm 20$	$260 \pm 18$
Perseus South	26	0.302	$\phantom{0}86 \pm 17$	$212 \pm 18$
California	119	0.270	$440 \pm 30$	$450 \pm 23$	-

Notes. The fourth column reports the measured distance and its 1- $\sigma$ error, as estimated from a comparison of the density of foreground stars with the Robin et al. (2003) Galactic model (see Fig. 10); the last column reports the two VLBI distances known from the literature (Loinard et al. 2007, for Taurus and Hirota et al. 2008, for Perseus).

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