Properties of dust at the Galactic center probed by AKARI far-infrared spectral mapping - Detection of a dust feature

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Table 1

Results of the two-temperature modified blackbody model fitting to the spectra in Figs. 2 and 8.

Spectrum	T_w (K)	T_c (K)	τ_90w^a	τ_90c^a


Figure 2a	51 ± 3	23.0 ± 0.3	(6 ± 1) × 10^-3	0.33 ± 0.01
Figure 2c	51 (fixed)	21.1 ± 0.2	(6.5 ± 0.1) × 10^-3	0.54 ± 0.02
Figure 2d	51 (fixed)	22.7 ± 0.2	(3.8 ± 0.1) × 10^-3	0.34 ± 0.01
Figure 8	51 (fixed)	19.7 ± 0.2	(5.2 ± 0.2) × 10^-3	0.49 ± 0.02, 0.10 ± 0.02^b

Notes.

^(a)

Optical depths at a wavelength of 90 μm for the warm and cold components.

^(b)

The second cold component whose emissivity corresponds to the large graphite population with the same temperature as the first cold component (see text for details).

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