Long-term Spectroscopic Survey of the Pleiades Cluster: The Binary Population

TL;DR

This long-term spectroscopic survey of the Pleiades identified over 30 new binary systems, analyzed their orbital properties, and found that the binary frequency is higher than in the field, providing insights into stellar multiplicity in clusters.

Contribution

The study extends the binary census of the Pleiades to longer periods using 43 years of data, doubling the known binaries and analyzing their orbital and statistical properties.

Findings

Binary frequency up to 10^4 days is 25% after correction.

Orbital period distribution similar to field stars, eccentricity distribution differs.

Tidal circularization period confirmed at 7.2 days.

Abstract

We present the results of a spectroscopic monitoring program of the Pleiades region aimed at completing the census of spectroscopic binaries in the cluster, extending it to longer periods than previously reachable. We gathered 6104 spectra of 377 stars between 1981 and 2021, and merged our radial velocities with 1151 measurements from an independent survey by others started three years earlier. With the combined data spanning more than 43 yr we have determined orbits for some 30 new binary and multiple systems, more than doubling the number previously known in the Pleiades. The longest period is 36.5 yr. A dozen additional objects display long-term trends in their velocities, implying even longer periods. We examine the collection of orbital elements for cluster members, and find that the shape of the incompleteness-corrected distribution of periods (up to $10^4$ days) is similar to that of solar-type binaries in the field, while that of the eccentricities is different. The mass-ratio distribution is consistent with being flat. The binary frequency in the Pleiades for periods up to $10^4$ days is $25 \pm 3$%, after corrections for undetected binaries, which is nearly double that of the field up to the same period. The total binary frequency including known astrometric binaries is at least 57%. We estimate the internal radial velocity dispersion in the cluster to be $0.48 \pm 0.04$ km s$^{-1}$. We revisit the determination of the tidal circularization period, and confirm its value to be $7.2 \pm 1.0$ days, with an improved precision compared to an earlier estimate.