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Table 3:

SED fitting results.

O-rich stars
                           

Name
$T_{\rm eff}$ $T_{\rm c}$ $\mathbf{\tau}_{\lambda}$ n D $V_{\rm gas}$ L ( ${\times}10^{4}$) $\dot{M}$ ($\times $10-6) $M_{\rm d}$ ( ${\times}10^{-5}$) M ( $\times 10^{-3}$) Am. Silicate Alumina Fe $\dot{M}_{\rm ref}$ ( ${\times}10^{-6}$)
  [K] [K]     [kpc] [km s-1] $L_{\hbox{$\odot$ }}$ [ $M_{\hbox{$\odot$ }}$/yr] [ $M_{\hbox{$\odot$ }}$] [ $M_{\hbox{$\odot$ }}$] [%] [%] [%] [ $M_{\hbox{$\odot$ }}/$yr]
WX Psc 2500 1010 9 -2.0 0.75a 20b 1.1 13 17 36 98 Ossen.   02 0.3-8b
o Cet 2600 1000 0.12 -1.9 0.128c 8b 1.4 0.11 0.11 0.11 100 Dorsch.     0.5k
VY CMa 2500 1100 13 -2.1 1.14r 47b 27.5 203 600 (...) 98 Ossen.   02 100n-300o
IRAS 16342-3814 2600 1000 480 -2.2 2i 46h 0.04 319 128 140 75 Ossen.   25 300i
AFGL 5379 2600 700 52 -2.3 1.19d 24b 0.5 46 97 250 97 Dorsch.   03 9-200q
IRC +10420 (ISO) 7000 750 5 -2.2 5e 42b 47 693 1980 4400 99.5 Dorsch.   0.5 700-900m
IRC +10420 (LRS) 7000 750 4 -2.2 5e 42b 39 260 522 1600 90 Dorsch. 08 02 700-900m
$\pi $ Gru 3000 900 0.04 -2.0 0.153c 11g 1.04 0.05 0.01 0.06 50 Ossen. 50   0.2-0.7l
C-rich stars                            
Name $T_{\rm eff}$ $T_{\rm c}$ $\mathbf{\tau}_{\lambda}$ n D $V_{\rm gas}$ L ( ${\times}10^{4}$) $\dot{M}({\times}10^{-6}$) $M_{\rm d}$ ( ${\times}10^{-5}$) M ( $\times 10^{-3}$) Am. C SiC MgS $\dot{M}_{\rm ref}$( ${\times}10^{-6}$)
  [K] [K]     [kpc] [km s-1] $L_{\hbox{$\odot$ }}$ [ $M_{\hbox{$\odot$ }}$] [ $M_{\hbox{$\odot$ }}$] [ $M_{\hbox{$\odot$ }}$] [%] [%] [%] [ $M_{\hbox{$\odot$ }}$/yr]
CW Leo 2650 1050 25 -2.3 0.135j 17f 0.9 7 1.2 6.2 66 12 22 22j
AFGL 3068 2650 1000 135 -2.5 1.05d 16f 1.4 110 3.6 300 78 04 18 20-62p

References. avan Langevelde et al. (1990); bKemper et al. (2003); cHipparcos (Perryman & ESA 1997); dYuasa et al. (1999); eJones et al. (1993); fGroenewegen et al. (1996); gKnapp et al. (1999); hHe et al. (2008); iSahai et al. (1999); jGroenewegen et al. (1998); kLoup et al. (1993); lGroenewegen & de Jong (1998); mDinh-V-Trung et al. (2009); nJura & Kleinmann (1990); oHarwit et al. (2001); pRamstedt et al. (2008); qKastner (1992); rChoi et al. (2008).

Notes.  $T_{\rm eff}$ is the effective temperature, $T_{\rm c}$ the dust condensation temperature, $\mathbf{\tau}_{\lambda}$ is the optical depth at 0.55 $\mu $m, n is the density power index, D the distance to the star, $V_{\rm gas}$ the terminal velocity derived from CO line measurements, L the luminosity, $\dot{M}$ the mass loss rate, $M_{\rm d}$ is the dust mass , M the total dust and gas mass loss, $\dot{M}_{\rm ref}$ the mass loss derived from previous studies.


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