Table 1: Miras observed.
Star Calibrator UD $_{2.2~\mu \rm m}$ UD $_{3.6~\mu \rm m}$ Dust $_{11~\mu \rm m}^1$ Vel A2 Vel B3 Period Sessions4
    (mas) (mas) (mas) (km s-1) (km s-1)    
R Andromadae J0136+4751       -14.8 -14.8 409.33 AB
omicron Ceti J0217+0144 24.40 (0.11) 35.2 (2.0) 120 48.0 45.0 331.96 ABCD
U Orionis J0555+3948 15.59 (0.06) 28.8 (0.1) 160 -34.0 -40.0 368.30 ABCD
R Leonis J0854+2006 29.435 (0.05) 36.0 (0.5) 140 2.0 -1.0 309.95 ABCD
W Hydrae J1337-1257       41.7 41.7 361.00 C
S Coronae Boralis J1613+3412 11.356 (0.26)     4.0 3.0 360.26 ABCD
U Herculis J1613+3412 10.98 (0.01) 14.3 (0.5)   -14.0 -16.0 406.10 ABCD
R Aquarii J2334+0736 16.88 (0.56) 34.3 (1.0) 140 -23.0 -23.0 386.96 AB
R Cassopeiae J2322+5057 24.78 (0.09) 31.1 (3.0)   25.4 25.4 430.46 CD
1 Fitted inner dust shell diameter from Danchi et al. (1994).
2 $\nu = 2$, J=1-0 transition of SiO at 42.8 GHz.
3 $\nu = 1$, J=1-0 transition of SiO at 43.1 GHz.
4 A = 25 Jan. 2001, B = 29 Apr. 2001, C = 4 Aug. 2001, D = 10 Nov. 2001.
5 From Perrin et al. (1999).
6 From van Belle et al. (2002).

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