Table A.4: IRAS photometry points at 12, 25, 60 and $850~\mu$ m. Note however that in some cases the $100~\mu$ m is an upper limit (L); these observations are probably contaminated by interstellar cirrus clouds. For RV Tau the $100~\mu$ m data point is a lower limit (:).
Name F₁₂(Jy) F₂₅(Jy) F₆₀(Jy) F₁₀₀(Jy)

TW Cam 8.25 5.60 1.84 1.79L

RV Tau
22.52 18.05 6.50 2.44:

SU Gem
7.91 5.68 2.19 11.99L

UY CMa
3.49 2.46 0.57 1.00L

U Mon
124.30 88.43 26.59 9.54

AC Her
41.43 65.33 21.37 8.04

R Sct
20.83 9.26 8.20 140.30L

**Table A.4:** IRAS photometry points at 12, 25, 60 and $850~\mu$ m. Note however that in some cases the $100~\mu$ m is an upper limit (L); these observations are probably contaminated by interstellar cirrus clouds. For RV Tau the $100~\mu$ m data point is a lower limit (:).
Name	F₁₂(Jy)	F₂₅(Jy)	F₆₀(Jy)	F₁₀₀(Jy)
TW Cam	8.25	5.60	1.84	1.79L
RV Tau	22.52	18.05	6.50	2.44:
SU Gem	7.91	5.68	2.19	11.99L
UY CMa	3.49	2.46	0.57	1.00L
U Mon	124.30	88.43	26.59	9.54
AC Her	41.43	65.33	21.37	8.04
R Sct	20.83	9.26	8.20	140.30L

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