Table 1
Basic parameters of the CoRoT RR Lyrae stars.
CoRoT ID | RA (2000) | Dec (2000) | V [mag] | Run | Type | f0,1 ampl. [mag] | PBl [days] | puls. period [days] | Ref. |
|
|||||||||
0101370131 | 19 28 14.40 | +0 06 02.27 | 15.60 | LRc01 | RRab | 0.257 | − | 0.619332 | (1) |
0101315488 | 19 27 47.40 | +0 58 35.62 | 16.15 | LRc01 | RRab | 0.029a | − | 0.4853033 | this work |
0103800818 | 18 31 23.80 | +9 10 10.45 | 13.70 | LRc04 | RRab | 0.345b | − | 0.4659348 | this work |
0104315804 | 18 34 28.92 | +8 57 00.43 | 15.94 | LRc04 | RRab | 0.130 | − | 0.7218221 | this work |
0100689962 | 19 24 00.10 | +1 41 48.70 | 14.96 | LRc01 | RRab Bl | 0.201 | 26.88 | 0.3559966 | (2) |
0101128793 | 19 26 37.32 | +1 13 34.90 | 15.93 | LRc01 | RRab Bl | 0.235 | 17.86 | 0.4719296 | (3) |
0100881648 | 19 25 05.43 | +1 39 23.83 | 16.16 | LRc01 | RRab Bl | 0.033a | 59.77 | 0.607186 | this work |
0101503544 | 19 29 10.12 | +0 43 47.14 | 14.79 | LRc01 | RRab Bl | 0.009a,b | 25.60 | 0.605087 | this work |
0105288363 | 18 39 30.86 | +7 26 53.95 | 15.32 | LRc02 | RRab Bl | 0.179 | 35.6 | 0.5674412 | (4, 5, 6) |
0103922434 | 18 32 08.55 | +8 32 40.78 | 15.84 | LRc04 | RRab Bl | 0.280 | 54.5 | 0.5413828 | (7) |
0105036241 | 18 38 09.60 | +7 43 56.68 | 15.58 | LRc02 | RRc | 0.196 | − | 0.372921 | this work |
0105735652 | 18 42 10.13 | +6 33 05.15 | 15.01 | LRc02 | RRc | 0.204 | − | 0.2791596 | this work |
0101368812 | 19 28 13.61 | +0 40 42.46 | 15.86 | LRc01 | RRd f0 | 0.053 | − | 0.4880408 | (8) |
RRd f1 | 0.143 | − | 0.3636016 |
Notes. The columns contain the CoRoT ID number, the coordinates, V magnitude, the CoRoT run, RR Lyrae subtype, the amplitude of the dominant mode(s), the Blazhko period in case of modulated stars, the pulsation period, and references. V magnitude values were taken from the ExoDat catalog. No good candidates classified as RR Lyrae stars were found in the third runs.
Reference. (1): Paparó et al. (2009); (2): Chadid et al. (2010); (3): Poretti et al. (2010); (4): Guggenberger et al. (2011); (5): Chadid et al. (2011); (6): Guggenberger et al. (2012), (7): Poretti et al. (in prep)., (8): Chadid (2012).
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