Table 4: The estimated total colour excess E(B-V) and the optical depth estimates in the V-band. $\tau _{V,E(B-V)}$ is determined from the SED minimalization and gives the total line-of-sight extinction. The contribution from the ISM is given in Col. 3 assuming the distance range given in Table 5. $\tau_{V,{\rm dust~model}}$ was determined by integrating the spherically symmetric dust model and in the last column the mean optical depth is given, determined by the energy ratio from the dust excess over the optical fluxes.
Name E(B-V) $\tau_V$

E(B-V) ISM model mean

TW Cam $0.3\pm0.3$ 0.86 $\rm 2.68^{3.27}_{2.10}$ 0.62 0.60

RV Tau
$0.4\pm0.3$ 1.14 $\rm 1.75^{1.75}_{1.75}$ 0.61 0.56

SU Gem
$0.8\pm0.3$ 2.28 $\rm 1.04^{1.47}_{1.04}$ 0.55 0.42

UY CMa
$0.0\pm0.3$ 0.00 $\rm0.00^{0.00}_{0.00}$ 0.75 0.46

U Mon
$0.3\pm0.3$ 0.00 $\rm0.51^{0.56}_{0.35}$ 0.22 0.07

AC Her
$0.3\pm0.3$ 0.86 $\rm0.62^{0.63}_{0.48}$ 0.27 0.01

R Sct
$0.0\pm0.3$ 0.00 $\rm 1.28^{1.51}_{0.98}$ 0.03 0.02

**Table 4:** The estimated total colour excess E(B-V) and the optical depth estimates in the V-band. $\tau _{V,E(B-V)}$ is determined from the SED minimalization and gives the total line-of-sight extinction. The contribution from the ISM is given in Col. 3 assuming the distance range given in Table 5. $\tau_{V,{\rm dust~model}}$ was determined by integrating the spherically symmetric dust model and in the last column the mean optical depth is given, determined by the energy ratio from the dust excess over the optical fluxes.
Name	E(B-V)	$\tau_V$
		E(B-V)	ISM	model	mean
TW Cam	$0.3\pm0.3$	0.86	$\rm 2.68^{3.27}_{2.10}$	0.62	0.60
RV Tau	$0.4\pm0.3$	1.14	$\rm 1.75^{1.75}_{1.75}$	0.61	0.56
SU Gem	$0.8\pm0.3$	2.28	$\rm 1.04^{1.47}_{1.04}$	0.55	0.42
UY CMa	$0.0\pm0.3$	0.00	$\rm0.00^{0.00}_{0.00}$	0.75	0.46
U Mon	$0.3\pm0.3$	0.00	$\rm0.51^{0.56}_{0.35}$	0.22	0.07
AC Her	$0.3\pm0.3$	0.86	$\rm0.62^{0.63}_{0.48}$	0.27	0.01
R Sct	$0.0\pm0.3$	0.00	$\rm 1.28^{1.51}_{0.98}$	0.03	0.02

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations and data reduction: 850 ${\mu }$ m SCUBA data
	3 Spectral Energy Distributions (SEDs)
	4 An optically thin dust fit
	5 Discussion: Characteristics of the dust excess
	6 Conclusions
	References
	Online Material
	Appendix A: Photometric data