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Table 2

Measured shell radii (R) and shell widths (ΔR – FWHM of Gaussian distribution) for R Scl and V644 Sco.

R Scl V644 Sco
R[′′] ΔR[′′] R[′′] ΔR[′′]

this paper 19.7 3.2 9.4 2.0
GD2001a 20.7
GD2003b 20.0 2.0
S2005 (dust)c 27.0 17.0
S2005 (gas)c 20.1 10.5
O2010d 19.2 1.2
M2012e 18.5 1.3

Notes. Both can be determined to with ±0.̋5. The results from this paper are derived from radiative transfer models constrained by the polarised intensity images from PolCor (see Fig. 5). The results are compared to previous estimates of the detached shells. resonance lines; .


Based on observations stellar light scattered in NaD and K;


based on polarised, dust-scattered stellar light;


based on dust and gas radiative transfer models;


based on observations of dust scattered stellar light;


based on fit to observed CO(3−2) line emission with ALMA

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