Table 7: Fitting parameters of the SED of the IRS 13 sources. The spectral type of each source, as discussed in Sect. 4, is summarized in the last column.
Star Coef₁ T₁ K Coef₂ T₂ K $A_{\rm v}$ Sp. type

W 13.50 3600 4250 640 38.5 M3III

E1 0.800 $\geq$ 25 000 12 000 550 35 $\sim$ O5I

E2 0.620 $\geq$ 25 000 40 000 550 35 $\sim$ WN8

E4 0.140 $\geq$ 25 000 45 1550 35 $\sim$ O5IIIe

E3A 0.460 3800 33 000 610 35 d. WR^a

E3B 0.375 3800 29 000 580 35 d. WR^a

E5 0.070 6000 9800 630 35 d. WR^a

E6 0.013 $\geq$ 25 000 29 $\sim$ O5V

$\textstyle \parbox{8.5cm}{ $^a$\space Dusty Wolf-Rayet star.}$

**Table 7:** Fitting parameters of the SED of the IRS 13 sources. The spectral type of each source, as discussed in Sect. 4, is summarized in the last column.
Star	Coef₁	T₁ K	Coef₂	T₂ K	$A_{\rm v}$	Sp. type
W	13.50	3600	4250	640	38.5	M3III
E1	0.800	$\geq$ 25 000	12 000	550	35	$\sim$ O5I
E2	0.620	$\geq$ 25 000	40 000	550	35	$\sim$ WN8
E4	0.140	$\geq$ 25 000	45	1550	35	$\sim$ O5IIIe
E3A	0.460	3800	33 000	610	35	d. WR^a
E3B	0.375	3800	29 000	580	35	d. WR^a
E5	0.070	6000	9800	630	35	d. WR^a
E6	0.013	$\geq$ 25 000			29	$\sim$ O5V

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