Table A.1
Cepheids in globular clusters.
| Gaia DR3 source id | ra [deg] | dec [deg] | Cluster | likelihood | prior | posterior | Final | Classification | Candidate | Period [d] | SOS |
|---|---|---|---|---|---|---|---|---|---|---|---|
| 899283619691731328 | 114.530019 | 38.912819 | NGC 2419 | 0.963 | 1 | 0.963 | True | ACEP F | False | 1.579 | False |
| 1328057184175359488 | 250.443656 | 36.457716 | NGC 6205 | 0.973 | 1 | 0.973 | True | T2CEP | False | 1.459 | True |
| 1328057867076964864 | 250.399567 | 36.463465 | NGC 6205 | 0.999 | 1 | 0.999 | True | T2CEP | False | 5.111 | True |
| … | … | … | … | … | … | … | … | … | … | … | … |
Notes. The complete version of this table is available at the CDS. If the likelihood for a given source is empty, it indicates that parallax and proper motion data are missing from the Gaia DR3 catalog, these stars were identified as cluster members by C17. The "Final" column specifies whether the star is part of the sample presented at the end of Sect. 4, while the "Classification" column lists the classification assigned to each star in this paper. The "Candidate" column identifies Cepheids for which membership could not be confirmed due to the absence of a measured pulsation period or time-series photometry. The column ’Period’ represents the pulsation period used for classification, while the column ’SOS’ shows whether SOS photometry is available in the Gaia archive.
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