Notes. Meaning of the different columns is as follows: (1) Gaia DR3 source id; (2) Literature Name; (3) Pulsation mode (RRab=Fundamental; RRc= First Overtone); (4) Pulsation period (P), as re-evaluated in the present analysis; (5) Intensity-averaged G-band mean magnitude, as derived from the SOS Cep&RRL pipeline; (6) number of valid RVS RV measurements; (7) Peak-to-peak amplitude of the combined RVS and literature RV data. The RVS measurements of TV Boo and M4-V32 were shifted by +5km s⁻¹, those of TW Her and UU Vir by −4 km/s, and those of AV Peg by −3 km/s to better match the corresponding literature data; (8) Centre of mass RV (γ) of the curve obtained by combining RVS and literature RV data, with in parentheses the rms scatter of the modelled RV curve; (9) Literature values for γ; (10) Iron abundance; (11) Mean effective temperature; (12) Mean gravity; (13) References for the literature RV; (14) References for the stellar parameters; (15) Notes: Binary (Bin) and/or Blazhko (Blaz.).; (16) Instrument type: a=CORAVEL; b=spectra; c=image-tube spectrograph; d=photoelectric RV meter. The meaning of the numbers in columns (13) and (14) is as follows: 1=Liu & Janes (1989); 2=Cacciari et al. (1987); 3=Clementini et al. (1990); 4=Skillen et al. (1993); 5=Barnes et al. (1988); 6=Meylan et al. (1986); 7=Jones et al. (1987); 8=Jones et al. (1988); 9=Liu & Janes (1990); 10=Cacciari et al. (1989a); 11=Cacciari et al. (1989b); 12=Skillen et al. (1989); 13=Cacciari et al. (1992); The binarity information is taken from Kervella et al. (2019). ^aGravity value at ϕ=0.0. ^b Cacciari et al. (1992) derived a mean gravity of 2.83±0.11 dex by averaging the gravity values inferred from the radii and masses published by Jones et al. (1992), which were derived from the B-W analysis of 18 RRab and 2 RRc stars. This mean gravity value can be used in place of ^(a), ^(c) and ^(d) or when a ⟨logg⟩ value is missing. ^cConstant gravity value adopted in Cacciari et al. (1992) B-W analysis of UU Cet, RV Phe and W Tuc, and in Skillen et al. (1993) analysis of W Crt. ^d2.7±0.2 is the ‘static’ gravity, that is the gravity of an RR Lyrae star were it not pulsating (Fernley et al. 1989). ^e ⟨T_eff⟩=6460 K estimated from the V − K colour by (Jones et al. 1988). ^fThe period derived by the SOS pipeline for this star (P_SOS=0.428933547 d) is incorrect, we provide in the table the correct period (P=0.4774854 d). The ⟨G⟩, Amp(RV) and γ_RVS values of V440 Sgr listed in the table were computed using the correct period. ^g Two RV measurements from Gaia RVS around the curve maximum are outliers with large errors. They were discarded when computing the Amp(RV) and γ values in columns (7) and (8).