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Fig. A.1

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a) Heliocentric distance of C-rich AGB stars as a function of the AKARI 9 μm flux. The open squares and the open circles show previously measured distances for well-studied samples from Zhang et al. (2010, squares) and Le Bertre et al. (2003, circles), respectively. The black dots show distances estimated for our purified samples. The dashed curves indicate the luminosity distance for the objects of  [K]  −  [9]  = 14 mag and  [K]  −  [9]  = 1 mag, which correspond to the dust-rich case (dM/dt ~ 10-4   M yr-1) and the dust-poor case (dM/dt ~ 10-8   M yr-1), respectively (see Fig. A.2). The vertical lines indicate the faint flux end of our sample (270 mJy), which corresponds to the distance of 8    ±    2 kpc for the dust-poor members. b) The same plot as panel a), but for O-rich AGB stars.

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