The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age

Morales, Leslie M.; Sandquist, Eric L.; Schaefer, Gail H.; Farrington, C.; Klement, Róbert; Bedin, L. R.; Libralato, Mattia; Malavolta, L.; Nardiello, D.; Orosz, Jerome A.; Monnier, John D.; Kraus, Stefan; Bouquin, J.-B. Le; Anugu, Narsireddy; Brummelaar, T. ten; Davies, Claire L.; Ennis, Jacob; Gardner, Tyler; Lanthermann, Cyprien

doi:10.3847/1538-3881/ac7329

Cited by 6 publications

(4 citation statements)

References 120 publications

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“…An exhaustive investigation of convective-core overshooting remains outside the scope of the present paper simply because we do not have neither the required observations nor models to settle the issue. A detailed revisit of the investigation by Knudstrup et al (2020) and other binary stars along with a simultaneous study of asteroseismic and binary measurements in NGC 6866, Hyades (Brogaard et al 2021a), M 44 (Morales et al 2022), NGC 6811 (Arentoft et al 2017), NGC 6819 (Handberg et al 2017), NGC 1817 (Sandquist et al 2020), and additional young open clusters could provide more constraints and insights in the future.…”

Section: Models Without Rotationmentioning

confidence: 99%

Asteroseismic age estimate of the open cluster NGC 6866 using Kepler and Gaia

Brogaard,

Arentoft,

Miglio

et al. 2023

A&A

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Context. Asteroseismic investigations of solar-like oscillations in giant stars allow for the derivation of their masses and radii. For members of open clusters, this allows us to obtain an age estimate of the cluster that is expected to be identical to the age estimate given by the colour-magnitude diagram, but independent of the uncertainties that are present for that type of analysis. Thus, a more precise and accurate age estimate can be obtained. Aims. We aim to identify and measure the asteroseismic properties of oscillating giant members of the open cluster NGC 6866 and utilise them for a cluster age estimate. Model comparisons also allow constraints to be placed on the stellar physics. Here, we investigate the efficiency of convective-core overshoot during the main sequence evolution, which has a significant influence on the age estimations for these relatively massive giants. The effects of rotation and core overshoot are similar, but not identical, and so, we also investigated the potential of our measurements to distinguish between these effects. Methods. We identified six giant members of NGC 6866 via photometry, proper motions, and parallaxes from Gaia, and spectroscopic literature measurements. These were combined with asteroseismic measurements, which we derived using photometric data from the Kepler mission for five of the stars. Comparisons to stellar-model isochrones constrained the convective-core overshoot and enable a more precise and accurate age estimate than previously possible. Results. A significant amount of differential reddening is found for NGC 6866. Asteroseismology establishes the helium-core burning evolutionary phase for the giants, which have a mean mass of 2.8 M⊙. Their radii are significantly smaller than predicted by current 1D stellar models unless the amount of convective-core overshoot on the main sequence is reduced to αov ≤ 0.1 ⋅ Hp in the step-overshoot description. Our measurements also suggest that rotation has affected the evolution of the stars in NGC 6866 in a way that is consistent with 3D simulations, but not with current 1D stellar models. The age of NGC 6866 is estimated to be 0.43 ± 0.05 Gyr, which is significantly younger and more precise than most previous estimates. Conclusions. We derive a precise cluster age while constraining convective-core overshooting and the effects of rotation in the stellar models. A comparison to age estimates from machine learning methods of the same and similar giant stars uncovers potential biases for automated asteroseismic and non-asteroseismic age estimates of helium-core burning stars.

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Section: Models Without Rotationmentioning

confidence: 99%

Asteroseismic age estimate of the open cluster NGC 6866 using Kepler and Gaia

Brogaard,

Arentoft,

Miglio

et al. 2023

A&A

Self Cite

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“…At the low-mass end of the main sequence, predictions from evolutionary models tend to overestimate the temperatures of stars by 3% and underestimate the radii of stars by 5%. 30 Comparing radii and temperatures with evolutionary models provides a way to measure the ages of nearby moving groups [31][32][33][34] and exoplanet host stars. 35 Moreover, these fundamental parameters are used to refine the location of the habitable zone around exoplanet host stars [36][37][38] and infer the radius of transiting exoplanets based on the stellar diameter and eclipse timing.…”

Section: Angular Diameter Of Starsmentioning

confidence: 99%

Design of the new CHARA instrument SILMARIL: pushing for the sensitivity of a 3-beam combiner in the H- and K-band.

Lanthermann

Brummelaar²,

Tuthill³

et al. 2022

Optical and Infrared Interferometry and Imaging VIII

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Optical interferometry is a powerful technique to achieve high angular resolution. However, its main issue is its lack of sensitivity, compared to other observation techniques. Efforts have been made in the previous decade to improve the sensitivity of optical interferometry, with instruments such as PIONIER and GRAVITY at VLTI, or MIRC-X and MYSTIC at CHARA. While those instruments pushed on sensitivity, their design focus was not the sensitivity but relative astrometric accuracy, imaging capability, or spectral resolution. Our goal is to build an instrument specifically designed to optimize for sensitivity. This meant focusing our design efforts on different parts of the instrument and investigating new technologies and techniques. First, we make use of the low noise C-RED One camera using e-APD technology and provided by First Light Imaging, already used in the improvement of sensitivity in recent new instruments. We forego the use of single-mode fibers but still favor an image plane design that offers more sensitivity than a pupil plane layout. We also use a minimum number of optical elements to maximize the throughput of the design, using a long focal length cylindrical mirror. We chose to limit our design to 3 beams, to have the capability to obtain closure phases, but not dilute the incoming flux in more beam combinations. We also use in our design an edge filter to have the capability to observe Hand K-band at the same time. We use a low spectral resolution, allowing for group delay fringe tracking but maximizing the SNR of the fringes for each spectral channel. All these elements will lead to a typical limiting magnitude between 10 and 11 in both H-and K-bands.

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“…We continue our paper series of determining the visual orbits of spectroscopic binary stars with long baseline interferometry -Paper I (Lester et al 2019a), Paper II (Lester et al 2019b), and Paper III (Lester et al 2020)-in order to determine the fundamental stellar parameters of the components. Precise fundamental parameters of binary systems are essential for determining orbital demographics (Raghavan et al 2010;Bordier et al 2022), testing models of stellar structure and evolution (e.g., Claret & Torres 2018;Morales et al 2022), calibrating mass and distance determination methods for single stars (Torres et al 2010;Chaplin & Miglio 2013;Gallenne et al 2018), and studying how binary stars form and evolve (e.g., Richardson et al 2021). In this paper, we present the results for the more massive binaries, HD 61859, HD 89822, HD 109510, and HD 191692.…”

Section: Introductionmentioning

confidence: 99%

Visual Orbits of Spectroscopic Binaries with the CHARA Array. IV. HD 61859, HD 89822, HD 109510, and HD 191692

Lester

Schaefer

Fekel

et al. 2022

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We present the visual orbits of four spectroscopic binary stars, HD 61859, HD 89822, HD 109510, and HD 191692, using long baseline interferometry with the CHARA Array. We also obtained new radial velocities from echelle spectra using the APO 3.5 m, CTIO 1.5 m, and Fairborn Observatory 2.0 m telescopes. By combining the astrometric and spectroscopic observations, we solve for the full, three-dimensional orbits and determine the stellar masses to 1%–12% uncertainty and distances to 0.4%–6% uncertainty. We then estimate the effective temperature and radius of each component star through Doppler tomography and spectral energy distribution analyses. We found masses of 1.4–3.5 M ⊙, radii of 1.5–4.7 R ⊙, and temperatures of 6400–10,300 K. We then compare the observed stellar parameters to the predictions of the stellar evolution models, but found that only one of our systems fits well with the evolutionary models.

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The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age

Cited by 6 publications

References 120 publications

Asteroseismic age estimate of the open cluster NGC 6866 using Kepler and Gaia

Asteroseismic age estimate of the open cluster NGC 6866 using Kepler and Gaia

Design of the new CHARA instrument SILMARIL: pushing for the sensitivity of a 3-beam combiner in the H- and K-band.

Visual Orbits of Spectroscopic Binaries with the CHARA Array. IV. HD 61859, HD 89822, HD 109510, and HD 191692

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