Luminosities and mass-loss rates of SMC and LMC AGB stars and red supergiants

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Volume 506 / No 3 (November II 2009)

A&A, 506 3 (2009) 1277-1296

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Table 4:

Fit results of the M-star sample for the first few entries.
Name	Spectral	grain	L	$\dot{M}$	fit?	$T_{\rm c}$	fit?	$R_{\rm out}$	$\tau_{0.5}$	$\tau_{10}$
	type (K)	type	( $L_{\odot}$ )	( $M_{\odot }$ yr^-1)		(K)
msxlmc1677	m8	VK	2773703	2.63e-06	1	802	1	10000.0	0.249	0.056
msxlmc1677	m5	sil75alox20fe5	3194712	2.06e-06	1	918	1	10000.0	0.106	0.034
hd271832	m6	VK	1787262	2.00e-08	0	900	0	10000.0	0.003	0.001
hd271832	m6	sil65alox30fe5	1791278	1.60e-08	0	900	0	10000.0	0.001	0.000
msxlmc1686	m10	DP 0.8 alox 0.2	1215022	9.42e-07	1	1000	0	10000.0	0.134	0.032
msxlmc1686	m10	sil55alox40fe5	1235338	6.02e-07	1	900	0	10000.0	0.056	0.018
rsmen	m9	VK	724206	5.23e-07	1	1000	0	10000.0	0.156	0.035
rsmen	m9	sil65alox30fe5	747279	5.74e-07	1	900	0	10000.0	0.073	0.024

Grain type refer to: VK = Volk & Kwok (1988), DL = Draine & Lee (1984), Suh = Suh (1999), OHM = Ossenkopf et al. (1992), DP = David & Pegourie (1995), and combinations of DP with Aluminium Oxide (AlOx). The types marked silXaloxYfeZ, refer to X-percent olivine, Y-percent AlOx, and Z-percent metallic iron (see Sect. 3 for details).

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