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Peer-reviewedCC BY 4.0Astronomy & Astrophysics

UX Men: Detached eclipsing binary as a benchmark candidate

  • G. N. Pawar1
  • K. G. Hełminiak1
  • N. J. Miller2
  • F. Marcadon3
  • A. Moharana4
  • T. B. Pawar5
  • A. Kalsi1
  • M. Konacki1
5 affiliations
  1. 1Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences
  2. 2Department of Physics and Astronomy, Uppsala University
  3. 3Private Researcher
  4. 4Astrophysics Group, Keele University
  5. 5Villanova University, Dept. of Astrophysics and Planetary Sciences
Open at sourceDOICite

Abstract

Context. Detached eclipsing binaries (DEBs) provide model-independent measurements of stellar masses and radii, which are essential for testing stellar-evolution models and calibrating space-based photometric missions.

Aims. We aim to deliver ultra-precise fundamental parameters for the DEB UX Men and to assess its suitability as a benchmark for upcoming missions such as PLATO . We evaluate the temporal stability of the photometric solutions and the way intrinsic stellar variability and instrumental systematics affect the derived parameters.

Methods. We analysed 31 TESS sectors (∼882 d) with the LIGHTKURVE package, and detrended spot-induced variability. Light-curve modelling was performed independently with JKTEBOP and ALLESFITTER . Radial velocities from HARPS (HAM/EGGS), FEROS, CORALIE, and UCLES were extracted via TODCOR and fitted with a Keplerian orbit. Spectral disentangling (5350–5800 Å) yielded individual component spectra, which were processed with ISPEC to determine T eff , [M/H], and micro- and macroturbulence. Eclipse-timing variations were examined through O-C diagrams. We also used multi-band photometry to determine the fluxes, flux ratios, and ultimately, to measure the photometric T eff .

Results. We obtained masses of M A = 1.2300 ± 0.0012 M ⊙ , M B = 1.1946 ± 0.0012 M ⊙ and radii of R A = 1.3605 ± 0.0031 R ⊙ , R B = 1.2801 ± 0.0069 R ⊙ , with a sub-percent precision. Uncertainties were found to be dominated by systematic effects coming from (weak) stellar activity. The metallicity estimates are [ M / H ] A = 0.02 ± 0.13 dex and [ M / H ] B = 0.07 ± 0.10 dex. An isochrone fitting yielded a consistent age of τ = 2.75 ± 0.13 Gyr. The system exhibits a ∼673-day periodicity in eclipse-timing variations, likely due to stellar activity, with no evidence of a third body.

Conclusions. UX Men is a high-precision benchmark binary, providing stringent tests of stellar models and a robust calibration source for PLATO ’s determination of stellar and exoplanet properties. We found no dependence between the results and the specific code that was employed. However, without a proper treatment of systematics caused by activity, the uncertainties would end up underestimated. Expanding the sample of similarly well-characterised DEBs will further strengthen the empirical foundation for stellar physics and improve the calibration of future photometric missions.

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Cite

BibTeXRIS
BibTeX
@article{pawar2026detached,
  title = {{UX Men: Detached eclipsing binary as a benchmark candidate}},
  author = {G. N. Pawar and K. G. Hełminiak and N. J. Miller and F. Marcadon and A. Moharana and T. B. Pawar and A. Kalsi and M. Konacki},
  journal = {Astronomy \& Astrophysics},
  year = {2026},
  month = oct,
  doi = {10.1051/0004-6361/202659300},
  url = {https://www.aanda.org/10.1051/0004-6361/202659300},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - UX Men: Detached eclipsing binary as a benchmark candidate
AU  - G. N. Pawar
AU  - K. G. Hełminiak
AU  - N. J. Miller
AU  - F. Marcadon
AU  - A. Moharana
AU  - T. B. Pawar
AU  - A. Kalsi
AU  - M. Konacki
PY  - 2026
DA  - 2026/10/29
JO  - Astronomy & Astrophysics
DO  - 10.1051/0004-6361/202659300
UR  - https://www.aanda.org/10.1051/0004-6361/202659300
AB  - Context. Detached eclipsing binaries (DEBs) provide model-independent measurements of stellar masses and radii, which are essential for testing stellar-evolution models and calibrating space-based photometric missions.  Aims. We aim to deliver ultra-precise fundamental parameters for the DEB UX Men and to assess its suitability as a benchmark for upcoming missions such as PLATO . We evaluate the temporal stability of the photometric solutions and the way intrinsic stellar variability and instrumental systematics affect the derived parameters.  Methods. We analysed 31 TESS sectors (∼882 d) with the LIGHTKURVE package, and detrended spot-induced variability. Light-curve modelling was performed independently with JKTEBOP and ALLESFITTER . Radial velocities from HARPS (HAM/EGGS), FEROS, CORALIE, and UCLES were extracted via TODCOR and fitted with a Keplerian orbit. Spectral disentangling (5350–5800 Å) yielded individual component spectra, which were processed with ISPEC to determine T eff , [M/H], and micro- and macroturbulence. Eclipse-timing variations were examined through O-C diagrams. We also used multi-band photometry to determine the fluxes, flux ratios, and ultimately, to measure the photometric T eff .  Results. We obtained masses of M A = 1.2300 ± 0.0012 M ⊙ , M B = 1.1946 ± 0.0012 M ⊙ and radii of R A = 1.3605 ± 0.0031 R ⊙ , R B = 1.2801 ± 0.0069 R ⊙ , with a sub-percent precision. Uncertainties were found to be dominated by systematic effects coming from (weak) stellar activity. The metallicity estimates are [ M / H ] A = 0.02 ± 0.13 dex and [ M / H ] B = 0.07 ± 0.10 dex. An isochrone fitting yielded a consistent age of τ = 2.75 ± 0.13 Gyr. The system exhibits a ∼673-day periodicity in eclipse-timing variations, likely due to stellar activity, with no evidence of a third body.  Conclusions. UX Men is a high-precision benchmark binary, providing stringent tests of stellar models and a robust calibration source for PLATO ’s determination of stellar and exoplanet properties. We found no dependence between the results and the specific code that was employed. However, without a proper treatment of systematics caused by activity, the uncertainties would end up underestimated. Expanding the sample of similarly well-characterised DEBs will further strengthen the empirical foundation for stellar physics and improve the calibration of future photometric missions.
SN  - 0004-6361
SN  - 1432-0746
ER  -