1|AK III-31                   |Mermilliod+ (1997, J/A+A/320/74) found this star to be a 5 day SB1, and presented an orbit. A very faint secondary is seen in our spectra, making it an SB2. Independent estimates of the secondary temperature and rotational velocity were not possible from our observations. A template for that star for the TODCOR measurements was selected based on the primary temperature with the help of properties predicted from a model isochrone for the cluster. Although the center-of-mass velocity agrees with the cluster mean, Gaia EDR3 places the object in the foreground of the Pleiades at half the distance, so it is not a member. This explains its location far above the main sequence.
  5|AK III-79                   |Our mean RV and the Gaia p.m. indicate this is a nonmember, even though the parallax agrees with the cluster mean.
 15|PELS 7                      |Our measurements show the velocities to be clearly variable. A minimum occurred in September of 2017, and a handful of CORAVEL observations include another low point in October of 1995. An SB1 orbital solution with a period of 20yr is presented in Table 6 and shown in Appendix B, but is only tentative due to poor phase coverage. The center-of-mass velocity is inconsistent with cluster membership, and the Gaia catalog indicates the parallax and p.m. are as well.
 21|AK III-419                  |Our observations reveal this to be a 34 day SB2.
 22|AK III-416                  |The Gaia EDR3 parallax and p.m., as well as its velocity, indicate this is a nonmember. Mermilliod+ (1997, J/A+A/320/74) found it to be a single-lined binary, and published an orbit with a 10.9 day period.
 26|AK II-346                   |There is spectroscopic evidence for the presence of a narrow-lined star and a broad-lined star from the shape of the cross-correlation functions (CCFs), which show asymmetries. Queloz+ (1998, J/A+A/335/183) also reported it to be an SB2. While we are not able to reliably detect the broad-lined star due to strong blending, the sharp-lined star (which we assume is the secondary) shows clear signs of long-term variability. However, our observations alone are not sufficient to determine an orbit unambiguously, due to a gap in the data between our Digital Speedometer and TRES measurements. The object was also observed by the CORAVEL group (Rosvick+ 1992A&A...255..130R ; Mermilliod+ 2009, J/A+A/498/949), and fortunately those ten measurements fill the gap and point to a period of about 6100 days. Our orbital fit results in a large coefficient for the minimum mass of the companion of 0.38M_{sun}_, consistent with our presumption that it corresponds to the more massive primary star, which we do not detect directly because of its rapid rotation. On one of their epochs, Mermilliod+ (2009, J/A+A/498/949) claim to have resolved the companion and report for it a velocity measurement of +39.01km/s that seems much too large, if the orbit determined here is approximately correct, because it would imply unreasonable minimum masses for the components of 27 and 4 solar masses. We have chosen to disregard that measurement here, and use only their "primary" velocity at that epoch, which fits our orbit well. We consider our solution in Table 6 to be somewhat preliminary at this time, although we do note that an old Mt. Wilson velocity from 1921 reported by Abt (1970ApJS...19..387A) is consistent with our model, and so is the median RV reported by Gaia (gathered over a time span much shorter than the period of the orbit). The orbital period we determine corresponds to a semimajor axis of about 67 mas at the distance to the Pleiades. We are not aware of any visual companions reported for this object.
 32|TRU S25 A, TRU S25          |The similar SIMBAD names suggest an association, but the stars are nearly 4{deg} apart on the sky. TRU S25 A is a nonmember according to Gaia and our RV measurements. TRU S25 is listed in the WDS as a visual binary, but the accompanying note indicates this is dubious. Its velocities have been reported by Torres (2020, J/ApJ/901/91).
 33|TRU S25 A, TRU S25          |The similar SIMBAD names suggest an association, but the stars are nearly 4{deg} apart on the sky. TRU S25 A is a nonmember according to Gaia and our RV measurements. TRU S25 is listed in the WDS as a visual binary, but the accompanying note indicates this is dubious. Its velocities have been reported by Torres (2020, J/ApJ/901/91).
 35|TRU S26                     |RVs together with a 71 day SB1 orbit for this rapidly rotating A star were reported by Torres (2020, J/ApJ/901/91). A previously published 4.7 day orbit by Pearce & Hill (1975PDAO...14..319P) is incorrect.
 43|PELS 25                     |The mean RV is lower than the cluster mean, but the entry in the Gaia EDR3 catalog shows the parallax and p.m. to be consistent with membership.
 44|AK III-664                  |Our observations show this to be a 14 day SB1.
 56|HCG 65                      |A 1.3" astrometric companion is listed in the Gaia EDR3 catalog.
 69|HII 102                     |This was observed with the CORAVEL by Mermilliod+ (1992A&A...265..513M), but variability was not noticed. Our own velocities also show little change, but are 2-3km/s higher. A time history of all the observations (Appendix C) indicates this is a very long-period binary. Additional velocities by Soderblom+ (1993, J/ApJS/85/315) and White+ (2007, J/AJ/133/2524) fit the trend, as does the median value listed in the Gaia EDR3 catalog. A faint visual companion at 3.6" is listed in the WDS and has an entry in the Gaia catalog, but seems too wide to be the spectroscopic secondary. The system may therefore be a hierarchical triple.
 72|TRU S45                     |A close 0.1" astrometric companion discovered by lunar occultations has been reported only once in 1930, and is unconfirmed. A wider, 1.7" companion to the south is confirmed by Gaia to be physically associated. Our spectroscopic observations do not resolve it, but signs that this is a close binary are seen from the broad wings of the CCF and the impression that the spectral lines are diluted compared to those of other stars of similar spectral type. This suggests the presence of a very rapidly rotating star, in addition to the one we are able to measure velocities for. We presume the star we measure is the fainter secondary of the 1.7" pair, based on the fact that its spectroscopically determined temperature is consistent with the GBP-GRP color from Gaia, whereas the Gaia color of the primary star is much bluer.
 74|HII 120                     |RV variability was first noticed by Raboud & Mermilliod (1998, J/A+A/329/101) based on five measurements. An 8yr orbit is reported for the first time in the present paper. Bouvier+ (1997, J/A+A/323/139) detected a close astrometric companion, but considered the target to be a nonmember; Gaia confirms membership. No parallax or p.m. are listed in Gaia EDR3 for the 3.4" astrometric companion listed in the WDS (Table 14). If the visual companion is physically associated, it would make the system a triple.
 80|MT 41                       |The parallax and p.m. components are somewhat different than the cluster mean, but the very high value of RUWE=10.146 indicates the astrometry may be biased. The rotation period from Rebull+ (2016, J/AJ/152/114 and J/AJ/152/113) is consistent with membership. We retain it as a possible member.
 81|HII 164                     |The secondary is very faint, and is only seen in our TRES spectra. The best parameters for the corresponding template could not be determined independently, and are merely educated guesses. As different choices change the secondary velocities to some degree, we consider the orbit for that component (specifically, K2) to be preliminary.
 86|HII 173                     |This SB2 was found by Mermilliod+ (1992A&A...265..513M), who published the first orbit with a period of 1.3yr. We have combined all CORAVEL observations (including others by Mermilliod+ 2009, J/A+A/498/949) with ours to update the orbital solution.
 89|HII 177                     |Queloz+ (1998, J/A+A/335/183) reported this as an SB2, but no orbit was presented. A single CORAVEL observation by Mermilliod+ (2009, J/A+A/498/949) that resolves the components agrees with the 2280 day orbit we report here. This is a nonmember, based on the center-of-mass velocity as well as information from the Gaia mission.
 93|HII 233                     |Mermilliod+ (1992A&A...265..513M) reported a drift in their CORAVEL velocities suggesting a long orbital period. Our observations reveal it to be an SB1 with a period of 3.5yr.
 98|HII 250                     |We find this to be a 970 day SB1.
100|HII 263                     |RV variability was first noticed by Raboud & Mermilliod (1998, J/A+A/329/101). Merging the CORAVEL velocities with ours indeed shows this to be a binary with a period longer than the duration of our survey. No visual companions have been reported. Prosser & Stauffer (1993IBVS.3826....1P) reported an anomalous dip in brightness in late 1992, and speculated it might be an eclipse. However, the velocities now show that event to have occurred near the bottom of the RV curve, so an eclipse by this companion is ruled out. Spottedness on the primary seems like a natural explanation.
103|HII 298, HII 299            |This is a 5.7" pair with membership confirmed by Gaia EDR3. The brighter star is HII 299, which is slightly hotter than the companion, as expected. The velocities are similar.
104|HII 298, HII 299            |This is a 5.7" pair with membership confirmed by Gaia EDR3. The brighter star is HII 299, which is slightly hotter than the companion, as expected. The velocities are similar.
106|HII 303, HII 302            |This is a 16" pair showing similar RVs. The northern (brighter) component, HII 303, is in turn a close 1.8" visual binary that we have observed separately only once. We refer to it in this paper as HII 303 B. The CCFs for all other observations of HII 303 show variable widths, which may be caused by variable, seeing-dependent contamination from the close companion.
107|HII 303, HII 302            |This is a 16" pair showing similar RVs. The northern (brighter) component, HII 303, is in turn a close 1.8" visual binary that we have observed separately only once. We refer to it in this paper as HII 303 B. The CCFs for all other observations of HII 303 show variable widths, which may be caused by variable, seeing-dependent contamination from the close companion.
112|HII 320                     |This is an SB2. Mermilliod+ (1992A&A...265..513M) reported it as single-lined, and presented the first orbit with a period of 2yr, but noted their suspicion that the companion is a rapidly rotating star, which they could not measure. We confirm this, and are able to measure the secondary RVs in our TRES spectra. Application of TODCOR to our Digital Speedometer spectra shows hints of the secondary, but the velocities for that star are too poor to be useful. Nevertheless, the use of TODCOR has the benefit of avoiding "peak-pulling" for the primary velocities. 10 We find those primary velocities to be consistent with those from TRES, so they have been incorporated into our final solution. We have chosen not to use the CORAVEL velocities in our updated orbital solution, because the semiamplitude of the primary from those velocities is significantly smaller than ours, compared to the errors, suggesting the CORAVEL measurements may be affected by peak-pulling. A vsini measurement for the primary star from CORAVEL (10.8+/-0.5km/s; Queloz+ 1998, J/A+A/335/183) agrees with our estimate of 10+/-2km/s. For the secondary, we measure vsini=35+/-4km/s and a cooler temperature than the primary.
113|HII 338                     |Our RVs show long-term variability, possibly associated with a 3.8" visual companion listed in the WDS.
119|PELS 38                     |Rosvick et al. (1992A&A...255..130R) reported it as a spectroscopic binary, on the basis of three observations. We find it to be a 17 day SB2 with a faint secondary, and present the first orbit. The TODCOR template for the secondary is an educated guess.
123|AK I-2-199                  |A 0.49" visual companion was reported by Konishi+ (2016, J/PASJ/68/92), and is substellar.
127|HII 468                     |This is Electra (17 Tau). The two astrometric companions discovered by lunar occultations may be one and the same (see Richichi et al. 1996). A 100 day spectroscopic orbit reported by Abt+ (1965ApJ...142.1604A) is spurious (see Torres 2020ApJ...898....2T). RV measurements were reported separately in the latter work.
129|HII 476                     |Raboud & Mermilliod (1998, J/A+A/329/101) claimed their RVs indicated a drift. We do not see that in our measurements, and our e/i metric classifies the object as non-variable.
133|HII 522                     |An SB1 orbit with a 23.8 day period was presented by Mermilliod+ (1992A&A...265..513M), which is consistent with ours. Those CORAVEL observations have been included with our own in an updated solution.
134|HII 514                     |A 0.78" astrometric companion was reported by Makarov & Robichon (2001A&A...368..873M) from a special reduction of the Tycho-2 observations.
138|HII 541                     |An astrometric companion has been discovered by lunar occultations. See also Torres (2020, J/ApJ/901/91).
140|HII 563                     |This is Taygeta (19 Tau). RVs and a tentative 8.7yr spectroscopic orbit for this object were reported by Torres (2020, J/ApJ/901/91), who presented new velocities that are inconsistent with an earlier orbit (Abt+ 1965ApJ...142.1604A). An astrometric companion is known from lunar occultations. The spectroscopic and astrometric companions may be the same.
144|HII 571                     |A 15.9 day SB1 orbit was published by Mermilliod+ (1992A&A...265..513M) that is consistent with ours. We have combined the observations to update the solution. A 3.8" visual companion is listed in the WDS, and has a separate entry in Gaia. This would make it a triple system.
145|HII 605                     |Mermilliod+ (1992A&A...265..513M) reported not being able to measure this object with CORAVEL because of its rapid rotation. Our observations show instead that it is double-lined, with components of relatively sharp features. The secondary is too faint to determine its rotational velocity independently. We adopt for it vsini=0km/s. Our SB2 orbital solution with a period of 21 days is presented in Tables 7-8 and shown in Appendix B.
156|HII 717                     |A close visual companion is known at a separation of 0.2", corresponding to a period of roughly a century. The RVs show a slow downward drift consistent with this (see Appendix C). RVs by Liu+ (1991ApJ...377..141L) and Soderblom+ (1993, J/ApJS/85/315) agree with the trend. A wider, very faint, and physically associated 5.3" companion is listed in the Gaia EDR3 catalog, which would make the system a triple.
158|HII 727                     |This is a long-period binary with incomplete phase coverage from our own observations, showing a single periastron passage in late 2019. By adding six CORAVEL observations from Mermilliod+ (2009, J/A+A/498/949), two from Liu+ (1991ApJ...377..141L), and one from Soderblom+ (1993, J/ApJS/85/315), we are able to find a satisfactory orbital solution with a period of about 20yr, and a high eccentricity of e=0.83. The minimum secondary mass is fairly large, but we do not detect the companion in our spectra.
160|HII 745                     |We find this to be a 4.2yr SB1. Although the minimum secondary mass is quite large, we are not able to detect the secondary with confidence. Two measurements of the primary star by Liu+ (1991ApJ...377..141L) fit our orbit well. The Gaia catalog lists a very wide astrometric companion at 15.8" that shares the parallax and p.m. of the primary. The system may thus be triple.
162|HII 739                     |An astrometric companion was discovered by lunar occultations.
165|HII 761                     |A 3.3 day SB1 orbit was reported by Mermilliod+ (1992A&A...265..513M). We have found it to be double-lined, and measured the secondary's velocities. However, the secondary is too faint to determine its temperature independently, so for that we have relied on an estimate from a model isochrone for the cluster.
169|HII 785                     |This is Maia (20 Tau). An astrometric companion was discovered by lunar occultations.
172|HII 817                     |This is Asterope (20 Tau). An astrometric companion is reported in the Gaia EDR3 catalog.
175|HII 879, HII 883            |The WDS lists this as a wide 17.5" visual pair, the brighter primary being HII 879. Gaia EDR3 gives nearly identical parallaxes and p.m.
176|HII 879, HII 883            |The WDS lists this as a wide 17.5" visual pair, the brighter primary being HII 879. Gaia EDR3 gives nearly identical parallaxes and p.m.
177|HII 890                     |A visual companion discovered by Bouvier+ (1997, J/A+A/323/139), currently at 1.2", is also listed in the Gaia EDR3 catalog, but the entry has no parallax or p.m.
178|HII 885                     |A 0.9" visual companion discovered by Bouvier+ (1997, J/A+A/323/139) is also listed in the Gaia EDR3 catalog, but the entry has no parallax or p.m.
180|AK I-2-288                  |Mermilliod+ (1997, J/A+A/320/74) first reported this object as an SB2, but lacked sufficient observations to solve for the orbit. Their seven measurements are combined with ours for the new SB2 orbital solution presented in Tables 7-8.
182|HII 916                     |RV variability was first noticed by Raboud & Mermilliod (1998, J/A+A/329/101). The combination of the CORAVEL measurements with our own does seem to support a long-term trend (see Appendix C).
185|HII 956                     |Visual binary with a preliminary orbit by Popovic & Pavlovic (1995BABel.151...45P) giving an angular semimajor axis of a"=1.9" and a period of 1400yr. Another determination by Malkov+ (2012, J/A+A/546/A69) reports a"=1.2" and P=900yr. The star whose velocities we are able to measure has a line broadening corresponding to vsini=55km/s, but the lines appear shallower than expected for its temperature, suggesting dilution by another star. Estimates in the literature of the rotational velocity of HII 956 are much higher than we measure: Smith & Struve (1944ApJ...100..360S) reported vsini=150km/s, Morse et al. (1991AJ....101.1495M) gave 200km/s, and Kounkel+ (2019, J/AJ/157/196) estimated 174km/s. We speculate that these determinations correspond to the primary star of the pair, which would explain the dilution we see. The velocities we measure would therefore be for the secondary.
199|HII 1084                    |An astrometric companion was discovered by lunar occultations.
201|TRU S93                     |Our observations show this to be a single-lined binary with a period of 2.9yr.
203|HII 1100                    |The Gaia EDR3 catalog reports that the 0.8" visual companion listed in the WDS has a slightly different p.m. than the target, although the Gaia quality flags indicate the astrometric solutions were problematic (large RUWE values for both components).
204|HII 1117                    |An SB2 orbit with a period of 26 days was published by Mermilliod+ (1992A&A...265..513M). Additional velocities were reported by Mermilliod+ (2009, J/A+A/498/949), though some of them have the primary and secondary interchanged. All of these CORAVEL observations have been incorporated into our updated orbital solution.
206|HII 1132                    |A 2.6" astrometric companion reported by Geissler+ (2012ApJ...746...44G) and Yamamoto+ (2013PASJ...65...90Y) is substellar.
218|HII 1284                    |RVs have been reported by Torres (2020, J/ApJ/901/91). Our new effective temperature estimate is 7740+/-200K.
219|HII 1298                    |The closer of two astrometric companions reported in the WDS (0.6") was discovered by lunar occultations. It may be the same as the 1.2" companion.
221|HII 1306                    |An astrometric companion was discovered by lunar occultations.
227|HII 1338                    |See Section 5.2.
228|HII 1348                    |Queloz+ (1998, J/A+A/335/183) reported this to be an SB2 based on three spectra from the ELODIE instrument, although no velocities were published. Our velocities yield the 95 day SB2 orbit presented in Tables 7-8. A visual companion at 1.1" is known, which is substellar (see Geissler+ 2012ApJ...746...44G and Yamamoto+ 2013PASJ...65...90Y). This would therefore be an interesting triple system with a circumbinary brown dwarf.
232|HII 1375                    |The astrometric companion listed in the WDS was discovered by lunar occultations.
233|HII 1407                    |Our observations show this to be a single-lined binary with a period of 2.6yr.
234|HII 1392, HII 1397          |This pair is separated by 5.7". The brighter star, HII 1397, is a metallic-line star and an SB1 with a 7 day orbit that was first reported by Conti (1968AJ.....73..348C). Our independent solution is consistent with theirs. The elements reported in Table 6 combine all observations together. We find HII 1392 to be an SB2 with a 2yr period and a large eccentricity (e=0.82), which would make this a quadruple system. Raboud & Mermilliod (1998, J/A+A/329/101) reported four measurements of HII 1392 with CORAVEL, but they are all near times of conjunction so the double nature of the source was not detected. Queloz+ (1998, J/A+A/335/183) measured a projected rotational velocity of 15.7+/-1.6km/s that is larger than our values for the two components (10-12km/s); this is likely the result of line blending.
235|HII 1392, HII 1397          |This pair is separated by 5.7". The brighter star, HII 1397, is a metallic-line star and an SB1 with a 7 day orbit that was first reported by Conti (1968AJ.....73..348C). Our independent solution is consistent with theirs. The elements reported in Table 6 combine all observations together. We find HII 1392 to be an SB2 with a 2yr period and a large eccentricity (e=0.82), which would make this a quadruple system. Raboud & Mermilliod (1998, J/A+A/329/101) reported four measurements of HII 1392 with CORAVEL, but they are all near times of conjunction so the double nature of the source was not detected. Queloz+ (1998, J/A+A/335/183) measured a projected rotational velocity of 15.7+/-1.6km/s that is larger than our values for the two components (10-12km/s); this is likely the result of line blending.
237|HII 1431                    |This is a 2.5 day eclipsing binary (HD 23642) discovered independently by Miles (1999JBAA..109..106M) and Torres (2003IBVS.5402....1T) using Hipparcos photometry. It has been used to address the controversy over the distance to the Pleiades, following the Hipparcos determination of a value smaller than the canonical one (see Munari+ 2004A&A...418L..31M ; Southworth+ 2005A&A...429..645S and Groenewegen+ 2007, J/A+A/463/579). The secondary of this SB2 is a metallic-line A star. Consequently, we used a synthetic template with a metallicity of [Fe/H]=+0.5 for that star, which provided better results. Nevertheless, a statistically significant primary/secondary velocity offset remains in our orbital solution, which we attribute to template mismatch stemming from the anomalous chemical composition of the secondary.
245|TRU S115                    |Our RVs for this rapid rotator show a hint of a downward trend (about 2km/s over 6000 days), which may or may not be significant. The e/i value is smaller than our threshold for variability.
249|HII 1645                    |This is a nonmember, and appears to have variable RV.
251|HII 1653                    |Our RVs show this to be a single-lined binary with a period of 1.5yr.
254|HII 1762                    |The 10.7yr spectroscopic orbit reported here has a very large minimum secondary mass. The RVs measured are believed to be for the secondary component. This is based on the broad wings seen in the CCF, as well as the unexpectedly shallow spectral lines for a star of near-solar temperature as determined from our spectra, corresponding to a spectral type of G1. This suggests dilution of the lines from the presence of a much more rapidly rotating star. This interpretation is supported by the large vsini of 180km/s reported for HII 1762 by Uesugi & Fukuda (1970crvs.book.....U), and the combined color index from Gaia EDR3, which, after correction for reddening, corresponds to an early F star (consistent with the A9V classification given in SIMBAD). The pair was resolved once by speckle interferometry, and found unresolved on two other occasions. The companion may be the same one detected spectroscopically. Liu+ (1991ApJ...377..141L) reported double lines in one of their two observations, but the velocity difference they measured is far too large to be consistent with the 10.7yr period.
261|HII 1823                    |The astrometric companion listed in the WDS was discovered by lunar occultations.
264|HII 1876                    |The astrometric companion listed in the WDS was discovered by lunar occultations. A new effective temperature estimate from this paper gives 9580+/-200K. RVs have been published by Torres (2020, J/ApJ/901/91).
266|HII 1912                    |This target has no parallax or p.m. from Gaia EDR3, and is listed as having a highly significant excess astrometric noise. A poorly determined p.m. from the Gaia DR2 catalog does appear consistent with membership, while the (also poor) parallax is smaller than expected. It has been considered a cluster member by some authors (e.g., Schilbach+ 1995, J/A+A/299/696 ; Belikov+ 1998, J/A+A/332/575 and Sampedro+ 2017, J/MNRAS/470/3937), and more doubtful by others (Olivares+ 2018, J/A+A/617/A15). A rotation period of 3.17 days by Oelkers+ (2018, J/AJ/155/39) seems to agree with the rotational sequence for the Pleiades, arguing for membership. A close (0.2") visual companion is listed in the WDS, and a wider one at 0.85" was reported by Makarov & Robichon (2001A&A...368..873M) from a special reduction of Tycho-2 observations. The latter measurement is uncertain, and it is unclear whether it corresponds to a different companion. In any case, one or both of these companions probably explain the difficulty with Gaia's astrometric solution. Our spectra suggest a blend of broad and narrow lines. We report velocities for the narrow-lined star only, which are constant and agree with the cluster mean.
267|TRU S127                    |Our velocities indicate this very rapid rotator (vsini=175km/s) is a long-period binary (see Appendix C), but the orbit is as yet undetermined. As the center of mass is not yet known, we have retained it as a possible Pleiades member even though the Gaia parallax is formally different from the cluster mean (but the p.m. is consistent with membership). The Gaia EDR3 quality flags indicate the astrometric solution was problematic, which may have affected the parallax.
269|HII 2027                    |See Section 5.2.
274|HII 2147                    |Single-lined binary with an 18yr orbit and absolute mass determinations from Torres+ (2020ApJ...898....2T), from a combination of astrometric and spectroscopic observations. The star seen spectroscopically is the secondary.
277|HII 2172                    |A 30.2 day SB1 orbit was presented by Mermilliod+ (1992A&A...265..513M). We have combined their observations with ours to update the solution. We see no sign of the secondary in our spectra.
278|HII 2195                    |The astrometric companion listed in the WDS was discovered by lunar occultations.
282|HII 2284                    |Raboud & Mermilliod (1998, J/A+A/329/101) reported this object as a spectroscopic binary based on eight CORAVEL measurements, but did not have enough velocities for an orbit. We confirm it to be a single-lined binary with a period of 807 days.
283|HII 2278                    |A 0.4" visual companion discovered by Bouvier+ (1997, J/A+A/323/139) is also listed in the Gaia EDR3 catalog, but has no parallax or p.m.
290|HII 2406                    |A 33 day single-lined orbit was reported by Mermilliod+ (1992A&A...265..513M). We have detected the secondary in our TRES spectra, and updated the solution using all measurements.
291|HII 2407                    |Mermilliod+ (1992A&A...265..513M) reported the first orbit for this SB1 with a 7 day period. It was recently discovered by David+ (2015ApJ...814...62D) to be an eclipsing binary based on observations from NASA's K2 mission. We combine the original CORAVEL velocities (as transformed to the IAU system by Mermilliod+ 2009, J/A+A/498/949) with our own, more numerous measurements, to provide an improved solution. The secondary is very faint and is not seen in our spectra.
297|HII 2500, HII 2503, HII 2507|These three objects may well form a multiple system. The brighter star, HII 2507, is an SB2 (P=16.7 days) first announced as an SB1 by Abt+ (1965ApJ...142.1604A) and later by Pearce & Hill (1975PDAO...14..319P). The secondary has been detected here for the first time. The two astrometric companions to HII 2507 reported in the WDS correspond to HII 2503 (3.3") and HII 2500 (10.1"). The latter is itself a close visual binary (0.3"), and also an SB1 with a period of about 6.5yr, although these two companions cannot be the same, making the object at least a triple. The variability of HII 2500 was first noticed by Raboud & Mermilliod (1998, J/A+A/329/101), who did not have enough observations for an orbit. There is no indication of a change in the width of the CCF for HII 2500, as might be expected from the 0.3" companion. If all of these stars are physically bound, this would be a sextuple system.
298|HII 2500, HII 2503, HII 2507|These three objects may well form a multiple system. The brighter star, HII 2507, is an SB2 (P=16.7 days) first announced as an SB1 by Abt+ (1965ApJ...142.1604A) and later by Pearce & Hill (1975PDAO...14..319P). The secondary has been detected here for the first time. The two astrometric companions to HII 2507 reported in the WDS correspond to HII 2503 (3.3") and HII 2500 (10.1"). The latter is itself a close visual binary (0.3"), and also an SB1 with a period of about 6.5yr, although these two companions cannot be the same, making the object at least a triple. The variability of HII 2500 was first noticed by Raboud & Mermilliod (1998, J/A+A/329/101), who did not have enough observations for an orbit. There is no indication of a change in the width of the CCF for HII 2500, as might be expected from the 0.3" companion. If all of these stars are physically bound, this would be a sextuple system.
299|HII 2500, HII 2503, HII 2507|These three objects may well form a multiple system. The brighter star, HII 2507, is an SB2 (P=16.7 days) first announced as an SB1 by Abt+ (1965ApJ...142.1604A) and later by Pearce & Hill (1975PDAO...14..319P). The secondary has been detected here for the first time. The two astrometric companions to HII 2507 reported in the WDS correspond to HII 2503 (3.3") and HII 2500 (10.1"). The latter is itself a close visual binary (0.3"), and also an SB1 with a period of about 6.5yr, although these two companions cannot be the same, making the object at least a triple. The variability of HII 2500 was first noticed by Raboud & Mermilliod (1998, J/A+A/329/101), who did not have enough observations for an orbit. There is no indication of a change in the width of the CCF for HII 2500, as might be expected from the 0.3" companion. If all of these stars are physically bound, this would be a sextuple system.
300|HCG 384                     |This is a 542 day SB2 with a faint secondary, for which we report an orbit here. A wide 13.9" companion listed in Gaia EDR3 may not be physical: its parallax and p.m. are somewhat different from those of the target.
303|HII 2601                    |A 1.9" companion is listed in the Gaia EDR3 catalog.
316|HII 2881                    |Queloz+ (1998, J/A+A/335/183) reported this as a suspected long-period double-lined binary. Our velocities show no significant change, and the e/i diagnostic incorporating the CORAVEL measurements is below our threshold for variability.
328|HII 3104                    |Our RVs show this to be a 3.6yr SB1. The decl. component of the p.m. from Gaia EDR3 is rather different from the mean for the cluster, suggesting the object may not be a member. However, the quality flags indicate the astrometric solution may be severely disturbed by the companion, so membership cannot yet be ruled out. The center-of-mass velocity is not far from the expected value.
330|HII 3097                    |A 2yr SB1 orbit was published by Mermilliod+ (1992A&A...265..513M) with a very high eccentricity of e=0.78. The better phase coverage of our observations improves the solution significantly. Table 6 and Appendix B present the combined fit using both data sets, augmented with additional CORAVEL measures by Mermilliod+ (2009, J/A+A/498/949).
332|HII 3163                    |The shape of the CCF suggests a blend of a broad and narrow peak. Our RVs correspond to the narrow peak. No astrometric companions have been reported.
338|HII 3197                    |This is a close visual binary with a 30.2yr astrometric orbit reported by Schaefer+ (2014AJ....147..157S). The semimajor axis is 0.08". A wider companion at 0.5" has also been found, making this a triple system. Our spectroscopic measurements correspond to the combined light.
342|PELS 69                     |This is a nonmember according to Gaia. We find it to be an SB1 with a period of 3.6 yr. Our solution combines our own measurements with about a dozen older ones from the CORAVEL (Mermilliod+ 2009, J/A+A/498/949).
348|AK IV-287                   |Our observations show that this is an SB1 with a 5yr period.
349|TRU S177                    |The parallax and p.m. information in the Gaia EDR3 catalog casts doubt on the membership of this object. However, there are indications that the astrometric solution may have been disturbed. Our RVs display a slow downward drift of 4km/s indicating binarity, which may be the cause of the excess astrometric noise. We retain it as a possible member.
351|DH 794                      |We find this to be a 5.7 day SB2, with a secondary that is too faint for us to establish its temperature and vsini independently from our spectra. The corresponding template was selected with help from the cluster isochrone.
352|AK IV-314                   |The 1.0" astrometric companion listed in the WDS has an entry in the Gaia EDR3 catalog, but no parallax or p.m. are reported.
356|HCG 489                     |We find this to be a 3 day double-lined binary.
358|HCG 495                     |Our observations show this is an 8.5 day SB2.
359|AK V-151                    |We find this to be an 8.4yr SB2, in which the rapidly rotating primary is only detectable in our TRES spectra. Gaia EDR3 indicates this is a background object; the center-of-mass velocity from our orbital solution is far from the cluster mean.
366|AK V-198                    |Mermilliod+ (1997, J/A+A/320/74) reported this as a double-lined binary, but lacked enough observations for an orbit. We now report an SB2 orbit with a period of 176 days. The parallax and p.m. information in the Gaia EDR3 catalog are somewhat different than the cluster mean, although evidence from a statistically significant excess astrometric noise and a large value of 2.797 for the RUWE parameter indicate the astrometric solution may have been affected. The rotation period measured by Rebull+ (2016, J/AJ/152/113 and J/AJ/152/114) is consistent with membership. We retain it as a possible member.
367|TRU S184x                   |This is a nonmember according to Gaia. It was observed 25 times with the CORAVEL by Rosvick et al. (1992A&A...255..130R), and although the measurements show considerable scatter, the authors were unable to decide whether it is a binary. The effective temperature and projected rotational velocity of the object are near the limit of the instrumental capabilities of northern CORAVEL. Our own observations show less scatter, but have not clarified the picture. Using only our TRES measurements, which have higher precision (except for the first, with an uncertainty twice as large as the others), we are able to obtain a marginally significant orbital solution with a period of about 6yr and a semiamplitude of only 1.5km/s, which we consider too tentative to report. The apparent variability could simply be due to stellar activity.
369|TRU S185                    |The Gaia EDR3 catalog lists a companion at 7.4" with similar parallax and p.m. as the target.
372|TRU S194                    |RVs along with a 10yr SB1 orbit have been reported by Torres (2020, J/ApJ/901/91) for this rapidly rotating B star. Our new effective temperature estimate is 10500+/-300K.
375|PELS 173                    |Information from Gaia EDR3 indicates this is a nonmember. Adding the CORAVEL observations to ours, there is a hint of an upward drift in the velocities. The median RV from Gaia is consistent with this.