2: 5A = BD +45 172. Four SOPHIE measurements were taken into account for 2: 5A each component. A correction of 3m/s was added to our original 2: 5A estimation of the RV calculated by fitting two Gaussian curves to the 2: 5A SOPHIE CCF. Seventeen blended measurements were taken into account in 2: 5A the calculation of the spectroscopic elements, resulting in the blend 2: 5A coefficient C_0_=0.679+/-0.033. 1: 18A = HD 8624. Revision of the orbit of Tokovinin (1999, 1: 18A Cat. J/A+AS/136/373). The Tokovinin's measurements were taken into 1: 18A account with a correction of +310m/s, corresponding to the best fit. 1: 18A Three blended measurements were taken into account in the calculation of 1: 18A the spectroscopic elements, resulting in the blend coefficient 1: 18A C_0_=0.564+/-0.035 1: 19B = HD 8956. Sixteen blended measurements were taken into account in the 1: 19B calculation of the spectroscopic elements, resulting in the blend 1: 19B coefficient C_0_=0.618+/-0.018. 2: 13A = BD +10 303. Preliminary orbit; our observations cover only 79.5% of 2: 13A the period. 2: 16A = HD 14446. The SB1 orbit was computed discarding all the measurements 2: 16A between 0 and -10km/s, which seem to refer to a third component with 2: 16A fixed velocity. The measurements of the secondary component are not 2: 16A symmetric to those of the primary, and it is impossible to derive a SB2 2: 16A orbit. Finally, a part of a long period orbit is visible in the large 2: 16A residuals of the SB1 orbit. Therefore, the system could be quadruple, 2: 16A although the CCF of a sole SOPHIE spectrum exhibits one dip only. 2: 20B = BD +17 493p. Orbit calculated discarding the 4 blended measurements. 2: 20B When they are taken into account, the blend coefficient is 2: 20B C_0_=0.624+/-0.042, but the orbital elements are not improved. 2: 33A = HD 27635. The 8 measurements of the secondary seem fixed around 2: 33A -28km/s, and we prefer to discard them. Otherwise, a SB2 orbit is 2: 33A obtained with K_2_=8.3km/s. 2: 38B = HD 285970. A first orbit was published by Griffin and Gunn 2: 38B (1981AJ.....86..588G). 2: 40A = HD 33185. A bright SB2 (6.67 mag) with a semi-major axis expected 2: 40A around 58mas, which should be easily separated. Fifteen blended 2: 40A measurements were taken into account in the calculation of the 2: 40A spectroscopic elements, resulting in the blend coefficient 2: 40A C_0_=0.762+/-0.061. 2: 48B = HD 59450. The star belongs to a triple CPM system and is also 2:49A. 1: 93A = HD 71149. Five blended measurements were taken into account in the 1: 93A calculation of the spectroscopic elements, resulting in the blend 1: 93A coefficient C_0_=0.683+/-0.032. 2: 54B = HD 80101 = ADS 7288AB. A visual binary system with separation 2: 54B 0.3arcsec. The A component is the SB1. The dip of the B component is 2: 54B visible on the CORAVEL CCF, with the fixed velocity 2: 54B V_B_=(52.08+/-0.33)km/s. Twenty-nine 29 blended RV refer to components 2: 54B A and B, with the blend coefficient C_0_=0.717+/-0.023. 1:112A = HD 81997. Revision of the orbit of Duquennoy and Mayor 1:112A (1991A&A...248..485D). 2: 58B = HD 89745. A correction of 0.489km/s was added to the 7 RV measurements 2: 58B derived from SOPHIE for each component, in order to get the best fit. 2: 58B Twenty-four blended measurements were taken into account in the 2: 58B calculation of the spectroscopic elements, resulting in the blend 2: 58B coefficient C_0_=0.788+/-0.037. 1:130B = HD 92855. Revision of the orbit of Tokovinin (1994PAZh...20..826T), 1:130B which was based on 17 recent measurements, but also on 9 measurements 1:130B performed between 1916 and 1932. We applied a correction of +0.381km/s 1:130B for the former, and +1.45km/s for the latter. 2: 64B = BD +12 2343. A first orbit was published by Jeffries, Bertram and 2: 64B Spurgeon (1995MNRAS.276..397J). 1:156A = HD 102509. Orbit of Griffin & Griffin (2004MNRAS.350..685G), partly 1:156A based on our RV measurements. The periastron epoch was converted in JD, 1:156A and the systemic velocity was translated in the CORAVEL system. 2: 68B = BD +28 2103. Revision of the orbit of Latham et al. 2: 68B (2002, Cat. J/AJ/124/1144); we found a correction of -0.120km/s to apply 2: 68B to their measurements. 2: 72A = HD 110025. A secondary dip was observed by Halbwachs et al. (2011, 2: 72A Proceedings SF2A 2011, pg 303), leading to the mass ratio q~0.64. 2: 72B = BD +17 2512. A secondary dip was observed by Halbwachs et al. (2011, 2: 72B Proceedings SF2A 2011, pg 303), leading to the mass ratio q~0.66. 2: 73B = HD 110106. A secondary dip was observed by Halbwachs et al. (2011, 2: 73B Proceedings SF2A 2011, pg 303), leading to the mass ratio q~0.75. 2: 74B = BD +26 2401. Eleven blended measurements were taken into account in the 2: 74B calculation of the spectroscopic elements, resulting in the blend 2: 74B coefficient C_0_=0.879+/-0.026. 1:175A = HD 112033. The star is ADS 8695, a visual binary with P=359yr, 1:175A a=1.18arcsec and {Delta}m=2.2mag (Heintz W.D., 1997ApJS..111..335H); the 1:175A secondary component is not visible on our observations, and the SB1 1:175A orbit refers to the brightest component of the visual binary. 1:175A A correction of -0.263km/s was applied to the 7 original SOPHIE 1:175A measurements. 2: 79B = HD 117433. Eleven blended measurements were taken into account in the 2: 79B calculation of the spectroscopic elements, resulting in the blend 2: 79B coefficient C_0_=0.743+/-0.028. 2: 85B = HIP 69885. Sixteen blended measurements were taken into account in the 2: 85B calculation of the spectroscopic elements, resulting in the blend 2: 85B coefficient C_0_=0.862+/-0.041. 2: 92A = HD 153252. A G5-type star without luminosity class. Due to the short 2: 92A period, it cannot be a giant; assuming the primary component is a dwarf, 2: 92A the secondary component has a minimum mass around 50 Jupiter masses, 2: 92A and it is a brown dwarf candidate. 2: 97B = HD 164025. Orbit of Griffin (2004Obs...124..190G), partly based on our 2: 97B RV measurements. The periastron epoch was converted in JD, and the 2: 97B systemic velocity was translated in the CORAVEL system. 2: 98B = HD 238865. The star is a triple system, consisting in a long period SB1 2: 98B with an additional short period orbit. Preliminary elements of the 2: 98B short period orbit were published by Tokovinin and Smekhov 2: 98B (1995PAZh...21..283T); in order to avoid the drift due to the long 2: 98B period, we rejected 21 of our CORAVEL measurements made before 2: 98B JD 2449000, but we took into account 16 measurements performed with 2: 98B Russian telescopes; the correction to add to the latter is +1.15km/s. 2: 99A = HD 169822. Revision of the orbit of Latham et al. (2002, 2: 99A Cat. J/AJ/124/1144), with a correction of -0.328km/s to their 2: 99A measurements. The spectral type of the star is G7 V, leading to a 2: 99A minimum mass around 30 Jupiter masses for the secondary component. 1:280A = HD 194765. A bright SB2 (6.70mag) with a semi-major axis expected 1:280A around 17mas, which should be easily separated. Five blended 1:280A measurements were taken into account in the calculation of the 1:280A spectroscopic elements, resulting in the blend coefficient 1:280A C_0_=0.683+/-0.024. 1:300B = BD +17 4697p. A bright SB2 (6.70mag) with a semi-major axis expected 1:300B around 17mas, which should be easily separated. Two blended measurements 1:300B were taken into account in the calculation of the spectroscopic 1:300B elements, resulting in the blend coefficient C_0_=0.736+/-0.061. 1:307A = HD 214511 = ADS 16111AB. Triple system already studied by Tokovinin 1:307A (1998, Cat. J/PAZh/24/343). A triple system solution was computed, 1:307A combining a long period SB2 with a SB1 as primary component. The period 1:307A of the SB2 was fixed to the value obtained by Docobo and Costa 1:307A (1986, IAU Double Star Inf. Circ. 99) for a visual orbit, as reported by 1:307A Hartkopf and Mason (Sixth Catalog of Orbits of Visual Binary Stars, 1:307A http://ad.usno.navy.mil/wds/orb6.html). The selection of the blended 1:307A measurements was done as follows: when only one RV was obtained, it was 1:307A assumed to be a blend as soon as the difference |V_1_-V_2_| was found 1:307A to be less than 30km/s. Nineteen blended measurements were taken into 1:307A account in the calculation of the spectroscopic elements, resulting in 1:307A the blend coefficient C_0_=0.928+/-0.022. The solution presented 1:307A hereafter is based on our measurements only, since it is better than the 1:307A one obtained when the measurements of Tokovinin are added.