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Table 1

Characteristics of the RR Lyrae spectra.

Night JD Tel. Obs. Spectro. Resolving RE λstart − λend S/N φstart φend ψ N Texp
(yyyy-mm-dd) (−2 400 000) power (pixel) (Å) (s)
1994-08-03 49 568 193 OHP ELODIE 44 000 2.1 3 800−6 800 78 0.08 0.09 0.39 1 420
1996-08-02 50 298 193 OHP ELODIE 44 000 2.1 3 800−6 800 60 0.08 0.09 0.08 1 480
1997-06-03 50 603 193 OHP ELODIE 44 000 2.1 3 800−6 800 84 0.08 0.09 0.89 1 300
1997-08-05 50 666 193 OHP ELODIE 44 000 2.1 3 800−6 800 32 0.08 0.09 0.50 1 300
1997-08-09 50 670 193 OHP ELODIE 44 000 2.1 3 800−6 800 17 0.08 0.09 0.60 1 480
1997-08-31 50 692 193 OHP ELODIE 44 000 2.1 3 800−6 800 69 0.08 0.09 0.17 1 300
2013-10-12 56 578 152 OHP AURELIE 22 700 2.8 6 500−6 700 86 0.04 0.04 0.91 1 300
2013-10-16 56 582 35 Chelles ESHEL I 10 500 3.2 4 300−7 100 75 0.08 0.09 0.03 1 300
2014-05-01 56 778 35 Foncaude ESHEL II 10 500 4.3 4 300−7 100 56 0.90 0.94 0.36 1 300
2014-08-13 56 883 35 Foncaude ESHEL II 10 500 4.3 4 300−7 100 43 0.90 0.94 0.04 7 300
2016-07-18 57 588 35 Chelles ESHEL I 10 500 3.2 4 300−7 100 69 0.08 0.09 0.00 1 300
2017-04-07 57 851 35 Chelles ESHEL I 10 500 3.2 4 300−7 100 76 0.04 0.42 0.75 21 900
2017-04-08 57 852 35 Chelles ESHEL I 10 500 3.2 4 300−7 100 78 0.80 0.18 0.77 18 900
2017-04-09 57 853 35 Chelles ESHEL I 10 500 3.2 4 300−7 100 74 0.56 0.85 0.80 16 900
2017-04-10 57 854 35 Chelles ESHEL I 10 500 3.2 4 300−7 100 60 0.37 0.50 0.83 7 900
2017-04-11 57 855 35 Chelles ESHEL I 10 500 3.2 4 300−7 100 80 0.20 0.47 0.85 5 900
2017-04-12 57 856 35 Chelles ESHEL I 10 500 3.2 4 300−7 100 86 0.92 0.22 0.88 6 900
2017-04-17 57 861 35 Chelles ESHEL I 10 500 3.2 4 300−7 100 77 0.65 0.02 0.00 6 900
2017-05-17 57 891 35 Chelles ESHEL I 10 500 3.2 4 300−7 100 72 0.08 0.09 0.75 3 600

Notes. Columns provide the date of the night, the corresponding Julian Date, the telescope (Tel.), the observatory (Obs.), the attached spectrograph (Spectro.), its resolving power, its resolution element (RE) at λ5896.92, the spectral range, the mean S/N per pixel in the λ6630 region, the start and end of the pulsation phase φ and the Blazhko phase ψ for each night, the number N of observed spectra, and finally the exposure time Texp used for the night.

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