A comprehensive Gaia DR3 study of the open cluster NGC 6134: Bayesian distances, present-day mass function, mass segregation, and structural decomposition
Abstract
Open clusters are key laboratories for studying the formation and dynamical evolution of stellar populations. We present a comprehensive characterization of the intermediate-age open cluster NGC 6134 using Gaia DR3 astrometry and photometry. Adopting the 890-member Hierarchical Density-Based Spatial Clustering of Applications with Noise (HDBSCAN) membership catalog, we determine the cluster distance and individual member distances with the Bayesian hierarchical code Kalkayotl under a King spatial prior, derive the fundamental parameters with the automated isochrone-fitting code ASteCA, quantify mass segregation, and decompose the projected spatial distribution into structural components. We obtain a Bayesian cluster distance of 1070.8+21.0−19.0 pc (mode and 68\% credible interval), consistent with the ASteCA value (d = 1064.4 ± 15.2 pc), with member distances peaking at 1071.2 ± 2.5 pc. ASteCA yields [Fe/H] = 0.08 ± 0.06, log(t) = 9.14 ± 0.01, and AV = 1.03 ± 0.05 mag. The present-day mass function (PDMF) follows a broken power law with slopes ΓA = −2.10+0.10−0.10 and ΓB = 1.59+0.14−0.14 and break mass Mc = 0.95+0.02−0.02 M⊙, with a negative low-mass slope and a high-mass slope steeper than the canonical Salpeter value (Γ= 1.35), consistent with the preferential loss of the most massive stars through stellar evolution rather than with dynamical depletion. The observed mass segregation is consistent with an origin in long-term dynamical evolution. The cluster comprises a core, a diffuse halo, and a coherent plane-of-sky elongated feature that is unlikely to arise from noise based on a size-matched isotropic null test, and that lies beyond the radius at which masses are available. The observed main-sequence gap is closely linked to the cluster's binary fraction.
Related
- Characterizing NGC 6383: Study of fundamental properties,pre-main sequence stars, mass segregation, and age using Gaia DR3 and 2MASS
- Globular cluster Observations for Luminosity-dispersion Distances (GOLD): Project description and velocity catalogue
- Systematic uncertainties on DESI Tully-Fisher distances constrained with Integral Field Spectroscopy
- Metal-Silicate Segregation During Planetary Accretion: Limited Iron Emulsification through intermediate Impacts
- Spatial segregation as the origin of anisotropic satellite quenching in haloes and beyond
BibTeX
@misc{jatmiko2026comprehensive,
title = {{A comprehensive Gaia DR3 study of the open cluster NGC 6134: Bayesian distances, present-day mass function, mass segregation, and structural decomposition}},
author = {Agus T. P. Jatmiko and Teduh Perhati and Dhimaz G. Ramadhan and Muhammad Yusuf and Denny Mandey and Mochamad I. Arifyanto and Premana W. Premadi and Sahlan Ramadhan and Ferry Yap and Laksma Satya},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2606.24270},
eprint = {2606.24270},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2606.24270},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - A comprehensive Gaia DR3 study of the open cluster NGC 6134: Bayesian distances, present-day mass function, mass segregation, and structural decomposition
AU - Agus T. P. Jatmiko
AU - Teduh Perhati
AU - Dhimaz G. Ramadhan
AU - Muhammad Yusuf
AU - Denny Mandey
AU - Mochamad I. Arifyanto
AU - Premana W. Premadi
AU - Sahlan Ramadhan
AU - Ferry Yap
AU - Laksma Satya
PY - 2026
DA - 2026/10/19
PB - arXiv
DO - 10.48550/arxiv.2606.24270
UR - https://arxiv.org/abs/2606.24270
AB - Open clusters are key laboratories for studying the formation and dynamical evolution of stellar populations. We present a comprehensive characterization of the intermediate-age open cluster NGC 6134 using Gaia DR3 astrometry and photometry. Adopting the 890-member Hierarchical Density-Based Spatial Clustering of Applications with Noise (HDBSCAN) membership catalog, we determine the cluster distance and individual member distances with the Bayesian hierarchical code Kalkayotl under a King spatial prior, derive the fundamental parameters with the automated isochrone-fitting code ASteCA, quantify mass segregation, and decompose the projected spatial distribution into structural components. We obtain a Bayesian cluster distance of 1070.8^+21.0_−19.0 pc (mode and 68\% credible interval), consistent with the ASteCA value (d = 1064.4 ± 15.2 pc), with member distances peaking at 1071.2 ± 2.5 pc. ASteCA yields [Fe/H] = 0.08 ± 0.06, log(t) = 9.14 ± 0.01, and A_V = 1.03 ± 0.05 mag. The present-day mass function (PDMF) follows a broken power law with slopes Γ_A = −2.10^+0.10_−0.10 and Γ_B = 1.59^+0.14_−0.14 and break mass M_c = 0.95^+0.02_−0.02 M_⊙, with a negative low-mass slope and a high-mass slope steeper than the canonical Salpeter value (Γ= 1.35), consistent with the preferential loss of the most massive stars through stellar evolution rather than with dynamical depletion. The observed mass segregation is consistent with an origin in long-term dynamical evolution. The cluster comprises a core, a diffuse halo, and a coherent plane-of-sky elongated feature that is unlikely to arise from noise based on a size-matched isotropic null test, and that lies beyond the radius at which masses are available. The observed main-sequence gap is closely linked to the cluster's binary fraction.
ER -