Table 2:

SED fit parameters and results.

	T*	L*		R*
	(104 K)	( )	(K)	()		(km)	( )	(K)	()
R71 (inner/outer shell)	1.5	4.6	490/120	100	2/1.6	1011/1012	10-6 / 10-4		10-1
IRAS05280-6910	0.3	2.2	250	1700	30	1011	10-3	...	...
HD 36402	18	4.6	960	15	300	1010		...	...
HD 36402 IR1 (YSO2)	...	...	...	...	...	...	...	64/15 ()	10-12/>

Notes. Fitting results from 2-D UST. DUSTY fits for R71 and IRAS05280-6910 estimate outer shell MLRs 2 to 4 less than the 2-D UST results. IR1/YSO2 was fit with two modified blackbodies (64 K and 15 K). For R71, we use O-deficient silicate optical constants (Ossenkopf et al. 1992) at long wavelengths and astronomical silicate optical constants (Draine & Lee 1984) at  m. For IRAS05280-6910, we use Ossenkopf et al. (1992) O-deficient silicates and for HD 36402, we use amorphous carbon grains from Zubko et al. (1996). The 2-D UST models use a KMH grain size distribution (Kim et al. 1994) with and ( for IRAS05280-6910). Stellar parameters for R71 are consistent with those from Lennon et al. (1993). is the temperature of the coldest dust component. For IRAS5280-6910, is measured from the maser emission (20 km s^-1; Marshall et al. 2004). For R71, we use 10 km s^-1, but the velocity measured from the H profile indicates the inner shell velocity may be >10 larger (Stahl et al. 1986). For HD36402, a typical velocity for a WC4 star is assumed (3000 km s^-1; Willis et al. 2004).