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The formation and evolution of binary systems. III. Low-mass binaries in the Praesepe cluster
With the aim of investigating the binary population of the 700 Myr oldPraesepe cluster, we have observed 149 G and K-type cluster membersusing adaptive optics. We detected 26 binary systems with an angularseparation ranging from less than 0.08 to 3.3 arcsec (15-600 AU). Aftercorrecting for detection biases, we derive a binary frequency (BF) inthe log P (days) range from 4.4 to 6.9 of 25.3 +/- 5.4%, which issimilar to that of field G-type dwarfs (23.8%, Duquennoy & Mayor\cite{r20}). This result, complemented by similar ones obtained for the2 Myr old star forming cluster IC 348 (Paper II) and the 120 Myr oldPleiades open cluster (Paper I), indicates that the fraction oflong-period binaries does not significantly evolve over the lifetime ofgalactic open clusters. We compare the distribution of cluster binariesto the binary populations of star forming regions, most notably Orionand Taurus, to critically review current ideas regarding the binaryformation process. We conclude that it is still unclear whether thelower binary fraction observed in young clusters compared to Tassociations is purely the result of the early dynamical disruption ofprimordial binaries in dense clusters or whether it reflectsintrinsically different modes of star formation in clusters andassociations. We also note that if Taurus binaries result from thedynamical decay of small-N protostellar aggregates, one would predictthe existence of a yet to be found dispersed population of mostly singlesubstellar objects in the Taurus cloud. Based on observations obtainedat the Canada-France-Hawaii Telescope.
| Open clusters with Hipparcos. I. Mean astrometric parameters
New memberships, mean parallaxes and proper motions of all 9 openclusters closer than 300 pc (except the Hyades) and 9rich clusters between 300 and 500 pc have been computed using Hipparcosdata. Precisions, ranging from 0.2 to 0.5 mas for parallaxes and 0.1 to0.5 mas/yr for proper motions, are of great interest for calibratingphotometric parallaxes as well as for kinematical studies. Carefulinvestigations of possible biases have been performed and no evidence ofsignificant systematic errors on the mean cluster parallaxes has beenfound. The distances and proper motions of 32 more distant clusters,which may be used statistically, are also indicated. Based onobservations made with the ESA Hipparcos astrometry satellite
| Stellar Activity in Coeval Open Clusters: Praesepe and the Hyades
Randich & Schmitt found that the coronal activity of solar-type andlow-mass stars in Praesepe is significantly lower than that of stars inthe Hyades cluster. This result is quite surprising, since the Hyadesand Praesepe have approximately the same age and metallicity and areoften thought to have originated in the same giant molecular cloudcomplex. We have carried out several tests in order to find a possibleexplanation for this result. We have measured radial velocities of twogroups of Praesepe stars (a dF-dK sample and a dM sample) and havemeasured Hα as a chromospheric activity index for the dM sample.Based on analyses of these data, we conclude that the Praesepe catalogused in the X-ray analysis does not contain a significant number ofnonmembers and, thus, that membership problems do not seem to be thecause of the Randich & Schmitt result. The comparison of theHα equivalent widths for the M dwarfs in Praesepe with those inthe Hyades indicates that, at least for stars in this mass range, thePraesepe stars are as active or more active than their Hyadescounterparts. The similarity of chromospheric emission allows us toreject differences in the rotational velocity distribution as the originof the dissimilar L_x luminosity functions. We have also analyzed a fewROSAT PSPC pointings of Praesepe in order to obtain a new andindependent estimate of the X-ray luminosities and upper limits for asmall sample of Praesepe members. This analysis suggests that theprevious ROSAT PSPC analysis produced slightly optimistic X-ray upperlimits; however, the differences between the old and new upper limitsare not large enough to explain the dichotomy in the X-ray properties ofPraesepe and the Hyades. Therefore, our examination of the availabledata does not provide a clear reason to explain why the X-ray luminosityfunctions of the two clusters are different. Part of the explanationcould be found in the binaries. Speculatively, these clusters could havedifferent orbital period distributions, with more short-period binariesamong the Hyades, which would show larger coronal activity.
| A ROSAT X-ray study of the Praesepe cluster.
We present the results of ROSAT PSPC observations of the Praesepecluster. 68 Praesepe candidates have been detected, above a threshold of=~2x10^28^erg/s, in the ~4x4deg area of the cluster covered by theobservations. 56 out of the 68 detected objects are cataloged as highprobability Praesepe members. Praesepe members of all spectral typeshave been detected with X-ray luminosities ranging from the sensitivitylimit to approximately 10^30^erg/s in the ROSAT broad band. The highestX-ray luminosity has been measured for a very short period W UMa typeSB2 binary. 2 out of the 4 Praesepe late-type giants have also beendetected. X-ray luminosity distribution functions have been derived forlate-type stars in the sample, taking into account both detections andupper limits. The main and most surprising finding are the low detectionrates derived for Praesepe low mass dwarfs. We detected about 30% of theF and G stars, and the detection rate among K and M dwarfs is evenlower. Correspondingly, the luminosity distribution functions for starsin selected color intervals are dominated by the contribution of upperlimits, with the medians below the sensitivity threshold. The comparisonwith the Hyades all-sky survey results shows an evident discrepancybetween the average X-ray properties of late-type dwarfs in the twoapparently coeval clusters; such a discrepancy must be an intrinsic one,since the observations are characterized by similar sensitivities.
| The luminosity function of Praesepe. I - A proper motion and photometric search for candidate members
Proper motions have been measured for a color selected sample of starsin a square 4 x 4 deg region centered on the Praesepe open cluster. Themagnitude limit of the photometry is about 19 and of the proper motionsabout 18. A list is presented of 765 probable and possible members from9 to 18 based on the proper motions, magnitudes, and colors. The resultsare compared with other proper motion surveys, and a preliminaryluminosity function of M(v) = 11 is calculated.
| Investigation of the Praesepe cluster. I - Identification of halo members
Coravel radial velocities and UBVRI (Kron) photometry of 117 starsselected by their proper motion in the region surrounding Praesepe (NGC2632, C 0837 + 201) have permitted identification of 48 members of thecluster halo, up to a distance of 4 deg from the cluster center. The 43(F5-K0) new members represent 51 percent of the number of nucleusmembers known in this spectral interval. Ten spectroscopic binaries havebeen discovered among the F5-F0 members, resulting in a frequency of 23percent, which rises to 33 percent four probable binaries are taken intoaccount. Six orbits have been obtained, with periods ranging from 1.2 to143 d. Four additional binaries have been detected among the non-memberstars.
| A Proper Motion Membership Study of Praesepe
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1983AJ.....88..215J&db_key=AST
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Observation and Astrometry data
| Constellation: | かに座 |
| Right ascension: | 08h39m10.97s |
| Declination: | +18°10'33.6" |
| Apparent magnitude: | 10.282 |
| Proper motion RA: | -37.9 |
| Proper motion Dec: | -14.6 |
| B-T magnitude: | 10.993 |
| V-T magnitude: | 10.341 |
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