Table 1
Cepheids for which an interferometric BW method has been applied.
| Cepheids | Reference |
|
|
|
| visible | |
| 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) |
| ℓ 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) |
| ℓ Car | Anderson et al. (2016) |
| X Sgr, W Sgr, ζ Gem, β Dor, ℓ 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⋆, ℓ 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, ℓ 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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