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Table 1

Cepheids for which an interferometric BW method has been applied.

Cepheids Reference

δ Cep Mourard et al. (1997)
α UMi, ζ Gem, δ Cep, η Aql Nordgren et al. (2000)
δ Cep, η Aql Armstrong et al. (2001)
Car Davis et al. (2009)

H band
ζ Gem Lane et al. (2000)
ζ Gem, η Aql Lane et al. (2002)
κ Pav Breitfelder et al. (2015)
Car Anderson et al. (2016)
X Sgr, W Sgr, ζ Gem, β Dor, Car Breitfelder et al. (2016)

K band
ζ Gem Kervella et al. (2001)
X Sgr, η Aql, W Sgr, ζ Gem, β Dor, Y Oph, Car Kervella et al. (2004)
δ Cep Mérand et al. (2005)
Y Oph Mérand et al. (2007)
FF Aql, T Vul Gallenne et al. (2012)
δ Cep, η Aql Merand et al. (2015a)

Notes. For some studies corresponding to the first attempts (indicated by asterisks) the pulsation could not be clearly resolved angularly leading to a mean value of the angular diameter of the Cepheid. In the visible domain, the BW method was applied successfully to only one Cepheid, Car, while in the infrared, among the eleven Cepheids the pulsation could be resolved for all stars, even X Sgr, which is known to be atypical likely owing to shockwaves travelling within the atmosphere (Mathias et al. 2006).

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