The spectral energy distributions of very long-period Cepheids in the Milky Way, the Magellanic Clouds, M31, and M33

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Table 2

Results of the fitting of dust models.

Identifier	T_eff (K)	Luminosity (L_⊙)	$χ_{r}^{2}$ $\chi_{\rm r}^2$	T_d (K)	τ_v	BIC	BIC	BIC
M31-PSO010.63	4625	33 948 ± 1425	36.1	343 ± 47	0.793 ± 0.096	725	712	78 137
M31-GDR369249	4375	24 688 ± 1516	41.3	609 ± 148	0.495 ± 0.154	738	781	2529
M31-VRJ004357	4000	28 105 ± 2006	27.0	557 ± 226	0.626 ± 0.244	453	430	964
M31-PSO011.09	5500	23 672 ± 1377	55.7	471 ± 60	0.760 ± 0.127	1296	1349	29 370
M31-VRJ004434	5000	37 394 ± 1545	83.1	330 ± 45	1.037 ± 0.100	2188	2414	232 000
M33-013312	5125	29 199 ± 5011	201.8	446 ± 197	1.161 ± 0.412	3556	3805	6002
LMC-CEP-0619	4875	47 329 ± 1315	54.8	925 ± 111	0.082 ± 0.015	1730	1750	29 766
II Car	3600	9312 ± 592	164.3	1858 ± 502	0.527 ± 0.218	3014	4077	5276

Notes. Column 1. The identifier used in this paper. Column 2. (Photometric) effective temperature with error bar from the SED fitting. Column 3. Luminosity with internal error bar from the SED fitting (for the fixed distance). Column 4. Reduced chi-squared of the fit. Column 5. Dust temperature at the inner radius. Column 6. Dust optical depth in the V band. The errors in T_d and τ_v are scaled to $χ_{r}^{2}$ $\chi_{\rm r}^2$ = 1. Column 7. BIC of this model. Column 8. BIC of the model without dust and removing outliers (the model in Table A.2). Column 9. BIC of a model without dust and including all data points.

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