The multiplicity fraction in 202 open clusters from <i>Gaia</i>

Donada, Joan Tort i; Anders, F.; Jordi, C.; Masana, E.; Gieles, M.; Perren, G. I.; Balaguer-Núñez, L.; Castro-Ginard, A.; Cantat-Gaudin, T.; Casamiquela, L.

doi:10.1051/0004-6361/202245219

Cited by 9 publications

(9 citation statements)

References 88 publications

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“…Our estimated BF for NGC 6819 is 25.72% ± 4.34%, slightly higher than the results (22% ± 3%) obtained by Milliman et al (2014) based on 93 spectroscopic binaries. The subplot in Figure 9 shows the relationship between BF and age, and the trend is consistent with that of Donada et al (2023) (red dashed line).…”

Section: Binary Fractionsupporting

confidence: 59%

Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation

Long,

Bi,

Zhang

et al. 2023

ApJS

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Using data from Gaia Data Release 3 and Kepler/K2, we present a catalog of 16 open clusters with ages ranging from 4–4000 Myr that provides detailed information on membership, binary systems, and rotation. We assess the memberships in 5D phase space, and estimate the basic parameters of each cluster. Among the 20,160 members, there are 4381 stars identified as binary candidates and 49 stars identified as blue straggler stars. The fraction of binaries varies in each cluster, and the range is between 9% and 44%. We obtain the rotation periods of 5467 members, of which 4304 are determined in this work. To establish a benchmark for the rotation–age–color relation, we construct color–period diagrams. We find that the rotational features of binaries are similar to that of single stars, while the features for binaries are more scattered in the rotation period. Moreover, the morphology of the color–period relationship is already established for Upper Scorpius at the age of 19 Myr, and some stars of varying spectral types (i.e., FG, K, and M type) show different spin-down rates after the age of ∼110 Myr. By incorporating the effects of stalled spin-down into our analysis, we develop an empirical rotation–age–color relation, which is valid with ages between 700–4000 Myr and colors corresponding to a range of 0.5 < ( G BP − G RP ) 0 < 2.5 mag.

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Section: Binary Fractionsupporting

confidence: 59%

Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation

Long,

Bi,

Zhang

et al. 2023

ApJS

View full text Add to dashboard Cite

show abstract

“…In general, our results for the binary fraction (after completeness correction) are in agreement with their results, except for three clusters: Alessi 9, NGC 1901, and NGC 3228. For these clusters, we find higher binary fractions than Donada et al (2023). This difference might be attributed to the different lower limit for the mass ratio (q > 0.6 in Donada et al 2023) adopted when calculating the binary fraction.…”

Section: Crossmatch With Previous Workmentioning

confidence: 52%

“…30 clusters in our sample are also described in the study of Donada et al (2023). The latter study also carried out distancedependent completeness corrections for the binary fraction.…”

Section: Crossmatch With Previous Workmentioning

confidence: 99%

Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters

Pang,

Wang,

Tang

et al. 2023

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Using membership of 85 open clusters from previous studies based on Gaia Data Release 3 data, we identify binary candidates in the color–magnitude diagram for systems with mass ratio q > 0.4. The binary fraction is corrected for incompleteness at different distances due to the Gaia angular resolution limit. We find a decreasing binary fraction with increasing cluster age, with substantial scatter. For clusters with a total mass >200 M ⊙, the binary fraction is independent of cluster mass. The binary fraction depends strongly on stellar density. Among the four types of cluster environments, the lowest-density filamentary and fractal stellar groups have the highest mean binary fraction: 23.6% and 23.2%, respectively. The mean binary fraction in tidal tail clusters is 20.8% and is lowest in the densest halo-type clusters: 14.8%. We find clear evidence of early disruptions of binary stars in the cluster sample. The radial binary fraction depends strongly on the clustercentric distance across all four types of environments, with the smallest binary fraction within the half-mass radius r h and increasing toward a few r h. Only hints of mass segregation are found in the target clusters. The observed amounts of mass segregation are not significant enough to generate a global effect inside the target clusters. We evaluate the bias of unresolved binary systems (assuming a primary mass of 1 M ⊙) in 1D tangential velocity, which is 0.1–1 km s−1. Further studies are required to characterize the internal star cluster kinematics using Gaia proper motions.

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“…However, we do not find any trend of binary fraction with the number of relaxation times. Some previous studies of photometric binaries in OCs have also observed such a trend between binary fraction and cluster age (Donada et al 2023), while others have not (Pang et al 2023; see also Section 5.4). However, many of these previous studies employ less reliable techniques to identify photometric binaries (i.e., "chi by eye").…”

Section: Impacts Of Stellar Dynamics and Relaxationmentioning

confidence: 84%

Goodbye to Chi by Eye: A Bayesian Analysis of Photometric Binaries in Six Open Clusters

Childs,

Geller,

von Hippel

et al. 2024

ApJ

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We present a robust methodology for identifying photometric binaries in star clusters. Using Gaia DR3, Pan-STARRS, and Two Micron All Sky Survey data, we self-consistently define the cluster parameters and binary demographics for the open clusters (OCs) NGC 2168 (M35), NGC 7789, NGC 6819, NGC 2682 (M67), NGC 188, and NGC 6791. These clusters span in age from ∼200 Myr (NGC 2168) to more than ∼8 Gyr (NGC 6791) and have all been extensively studied in the literature. We use the Bayesian Analysis of Stellar Evolution software suite to derive the age, distance, reddening, metallicity, binary fraction, and binary mass-ratio posterior distributions for each cluster. We perform a careful analysis of our completeness and also compare our results to previous spectroscopic surveys. For our sample of main-sequence stars with masses between 0.6 and 1 M ⊙, we find that these OCs have similar binary fractions that are also broadly consistent with the field multiplicity fraction. Within the clusters, the binary fraction increases dramatically toward the cluster centers, likely a result of mass segregation. Furthermore nearly all clusters show evidence of mass segregation within the single and binary populations. The OC binary fraction increases significantly with cluster age in our sample, possibly due to a combination of mass-segregation and cluster-dissolution processes. We also find a hint of an anticorrelation between binary fraction and cluster central density as well as total cluster mass, possibly due to an increasing frequency of higher-energy close stellar encounters that inhibit long-period binary survival and/or formation.

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The multiplicity fraction in 202 open clusters from Gaia

Cited by 9 publications

References 88 publications

Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation

Investigating 16 Open Clusters in the Kepler/K2–Gaia DR3 Field. I. Membership, Binary Systems, and Rotation

Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters

Goodbye to Chi by Eye: A Bayesian Analysis of Photometric Binaries in Six Open Clusters

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