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tokens: motion in declination direction. The proper motion of SV Cru, (μ αcos δ, Cep , μ δ, Cep ) = (− 6.43 ± 0.04, 1.31 ± 0.05) mas yr −1 , deviates 10.9σ in declination direction from the proper motion of Ruprecht 97, (μ αcos δ, cl , μ δ, cl ) = (− 6.49 ± 0.07, 0.44 ± 0.07). The mean proper motion is estimated by 23 OC members and the deviation of proper motion may be caused by the strict selection of OC members. Considering the good matching of other constraints, we regard SV Cru as an OC Cepheid. The distance and age of Ruprecht 97 are DM = 12.95 ± 0.53 mag and log ( t yr −1 ) = 8.13 ± 0.21, which are consistent with Cantat-Gaudin et al. ( 2020 ). 3.1.10 UBC 231 and WX Pup WX Pup is located at about 25.9 arcmin from the centre of UBC 231. Its proper motion is 2.2σ from the mean proper motion of UBC 231. The parameters of UBC 231 DM = 12.31 ± 0.17 mag and log ( t yr −1 ) = 7.87 ± 0.30 are in agreement with the reference values DM = 12.31 mag and log ( t yr −1 ) = 8.07, given by Cantat-Gaudin et al. ( 2020 ). 3.1.11 UBC 375 and V438 Cyg V438 Cyg is located at approximately 7.0 arcmin from the centre of UBC 375. V438 Cyg satisfies the constraints of the spatial position and parallax. The proper motion of V438 Cyg is (μ αcos δ, Cep , μ δ, Cep ) = (− 3.28 ± 0.07, −4.27 ± 0.07) mas yr −1 , which is 6.4σ away from the mean proper motion of UBC 375 (μ αcos δ, cl , μ δ, cl ) = (− 3.42 ± 0.07, −5.22 ± 0.11) mas yr −1 . The determined OC’s parameters are DM = 11.08 ± 0.21 mag and log ( t yr −1 ) = 8.03 ± 0.30, which are consistent with Cantat-Gaudin et al. ( 2020 ). Since only 32 OC members are adopted to estimate the mean proper motion, the deviation of proper motion may be attributed to the strict selection of OC members. Considering the good matching of other constraints, we still regard V438 Cyg as an OC Cepheid. 3.1.12 FSR 0158 and GQ Vul GQ Vul is located at approximately 2.4 arcmin from the centre of FSR 0158. GQ Vul agrees well with FSR 0158 in the proper motion (0.6σ) and parallax (0.1σ). This new OC Cepheid is ∼5.3 kpc from us and almost at the detection limit of our method based on proper motions and parallaxes. The far away OC Cepheids in the Milky Way’s disk are helpful to testify the probable bias in Cepheid’s PAR. 3.2 Issue about the known OC Cepheid In this subsection, we discuss known OC Cepheids not included in our catalogue. We compared with Turner ( 2010 ) who established an OC Cepheid catalogue based on optical data and found that 11 of the 24 OC Cepheids in that work are in our list. Nine of the other 13 Cepheids are in small clusters or star associations and they are not included in Cantat-Gaudin’s membership analysis catalogue. Three OC Cepheids have proper-motion differences larger than 10σ. The remaining OC Cepheid is BB Sgr in Collinder 394. 3.2.1 Collinder 394 and BB Sgr BB Sgr was treat as an OC Cepheid for a long time from Turner Pedreros ( 1985 ). However, based on Gaia , the membership is questionable. The proper motion of BB