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This article has an erratum: [https://doi.org/10.1051/0004-6361/200912982e]


   

Table 4:

Best fit parameters deduced from our full spectral fitting.

Name
$\chi^2$ $T_{\rm dust1}$ $T_{\rm dust2}$ Fraction $T_{\rm cont1}$ $T_{\rm cont2}$ Fraction
    (K) (K) $T_{\rm dust1}$ - $T_{\rm dust2}$ (K) (K) $T_{\rm cont1}$- $T_{\rm cont2}$

MACHO 79.5501.13
5.1 $ 180_{ 81}^{\rm 72}$ $ 843_{444 }^{\rm 145}$ $ 0.75_{0.75}^{\rm0.22}{-}0.25_{0.22}^{\rm0.75 }$ $ 458_{ 284}^{\rm 119}$ $ 743_{122}^{\rm 220}$ $ 0.62_{ 0.45}^{\rm0.28}{-}0.38_{0.28}^{\rm0.45}$
MACHO 82.8405.15 3.9 $ 490_{91 }^{\rm 106 }$ $ 737_{339 }^{\rm 207 }$ $ 0.78_{0.69 }^{\rm0.21 }{-}0.22_{0.21 }^{\rm0.69 }$ $ 279_{145}^{\rm 59}$ $ 563_{ 105}^{\rm 258 }$ $ 0.86_{0.24 }^{\rm0.1 }-0.14_{ 0.10}^{\rm0.24 }$

Name

  Olivine Pyroxene Forsterite Enstatite Continuum  
    small - large small - large small - large small - large    

MACHO 79.5501.13
$3_{ 3}^{\rm 37 }{-}4_{ 4}^{\rm 48}$ $28_{27}^{\rm 33}{-}12_{12}^{\rm 49}$ $8_{8}^{\rm 43}{-}29_{ 25}^{\rm 24}$ $ 8_{8}^{\rm 38}{-}8_{8}^{\rm 35}$ $87_{10}^{\rm 8}$    
MACHO 82.8405.15 $ 9_{ 9}^{\rm 34}{-}6_{6}^{\rm 60}$ $30_{27}^{\rm 32}{-}15_{14}^{\rm 48}$ $9_{8}^{\rm 22}{-}16_{14}^{\rm 31}$ $7_{7}^{\rm 32}{-}9_{8}^{\rm 28}$ $84_{11}^{\rm 10}$    

Note: Listed are the $\chi^2$, dust and continuum temperatures and their relative fractions. The abundances of small (0.1 $\mu $m) and large (2.0 $\mu $m) grains of the various dust species are given as fractions of the total mass, excluding the dust responsible for the continuum emission. The last column gives the continuum flux contribution, listed as a percentage of the total integrated flux over the full wavelength range. The errors were obtained using a monte-carlo simulation based on 100 equivalent spectra. Details of the modelling method are explained in Gielen et al. (2008).


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