Table 4: Positions and beam size of the apertures used to extract the spatially resolved spectra along the main axis of the nebula, increasing numbers from north to south. The three last columns report the result of the best fit to the spectra by using thermal emission with temperature T_bb and opacities computed for various dust species.
Ap. Shift FWHM T_bb Silic. Al₂O₃

(mas) (mas) (K) (%) (%)

1
-1568 350 310 $\pm$ 50 75 $\pm$ 15 25 $\pm$ 15

2
-1176 330 390 $\pm$ 50 65 $\pm$ 10 35 $\pm$ 10

3
-784 200 460 $\pm$ 50 60 $\pm$ 10 40 $\pm$ 10

4
-392 200 600 $\pm$ 70 55 $\pm$ 5 45 $\pm$ 5

5
0 200 720 $\pm$ 80 55 $\pm$ 5 45 $\pm$ 5

6
392 200 570 $\pm$ 5 55 $\pm$ 5 45 $\pm$ 5

7
784 200 440 $\pm$ 50 55 $\pm$ 5 45 $\pm$ 5

8
1176 330 440 $\pm$ 50 50 $\pm$ 5 50 $\pm$ 5

9
1568 350 480 $\pm$ 60 45 $\pm$ 5 55 $\pm$ 5

**Table 4:** Positions and beam size of the apertures used to extract the spatially resolved spectra along the main axis of the nebula, increasing numbers from north to south. The three last columns report the result of the best fit to the spectra by using thermal emission with temperature T_bb and opacities computed for various dust species.
Ap.	Shift	FWHM	T_bb	Silic.	Al₂O₃
	(mas)	(mas)	(K)	(%)	(%)
1	-1568	350	310 $\pm$ 50	75 $\pm$ 15	25 $\pm$ 15
2	-1176	330	390 $\pm$ 50	65 $\pm$ 10	35 $\pm$ 10
3	-784	200	460 $\pm$ 50	60 $\pm$ 10	40 $\pm$ 10
4	-392	200	600 $\pm$ 70	55 $\pm$ 5	45 $\pm$ 5
5	0	200	720 $\pm$ 80	55 $\pm$ 5	45 $\pm$ 5
6	392	200	570 $\pm$ 5	55 $\pm$ 5	45 $\pm$ 5
7	784	200	440 $\pm$ 50	55 $\pm$ 5	45 $\pm$ 5
8	1176	330	440 $\pm$ 50	50 $\pm$ 5	50 $\pm$ 5
9	1568	350	480 $\pm$ 60	45 $\pm$ 5	55 $\pm$ 5

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations and data reduction
	3 Description of the images
	4 Dust composition and temperature
	5 Correlated flux
	6 Discussion
	7 Conclusion
	References