Spectra of two archetypal dust-rich objects accompanying prominent AME, (a) the Perseus MC and (b) W 43, are fitted by our amorphous model. Dashed curves are the best-fitting thermal emission model from amorphous silicate dust, and dotted lines are the best-fitting free–free emission contribution. In both sets of data, contributions from the Galactic interstellar medium are subtracted. Although temperature fluctuation of the CMB is subtracted from the spectrum of W 43, it is not taken into account in the spectrum of the Perseus MC. Therefore, the CMB contribution is taken into account in the SED fit for the Perseus MC. As shown in table 2, the best CMB temperature fluctuation takes a negative value. The absolute value of the best-fitting CMB contribution is shown by dash–dotted line in panel (a). The solid curves show the total SEDs of the best-fitting models. The bottom panel inserted in each figure shows the data-to-model ratio.