The Araucaria Project: accurate stellar parameters and distance to evolved eclipsing binary ASAS J180057-2333.8 in Sagittarius Arm

Suchomska, K.; Graczyk, D.; Smolec, R.; Pietrzyński, G.; Gieren, W.; Stępień, K.; Konorski, P.; Pilecki, B.; Villanova, S.; Thompson, I. B.; Górski, Marek; Karczmarek, P.; Wielgórski, Piotr; Anderson, Richard I.

doi:10.1093/mnras/stv951

Cited by 24 publications

(24 citation statements)

References 55 publications

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“…Reddenings to each object were taken from the literature, if available, and also derived independently using the extinction maps by Schlegel et al (1998) following the prescription given in Suchomska et al (2015). Dereddened magnitudes and colors were calculated using the mean Galactic interstellar extinction curve from Fitzpatrick & Masana (2007) assuming R V = 3.1.…”

Section: Temperature and Reddeningmentioning

confidence: 99%

The Surface Brightness-color Relations Based on Eclipsing Binary Stars: Toward Precision Better than 1% in Angular Diameter Predictions

Graczyk

Konorski

Pietrzyński

et al. 2017

ApJ

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In this study we investigate the calibration of surface brightness-color (SBC) relations based solely on eclipsing binary stars. We selected a sample of 35 detached eclipsing binaries with trigonometric parallaxes from Gaia DR1 or Hipparcos, whose absolute dimensions are known with an accuracy better than 3% and that lie within 0.3 kpc from the Sun. For the purpose of this study, we used mostly homogeneous optical and near-infrared photometry based on the Tycho-2 and 2MASS catalogs. We derived geometric angular diameters for all stars in our sample with a precision better than 10%, and for 11 of them with a precision better than 2%. The precision of individual angular diameters of the eclipsing binary components is currently limited by the precision of the geometric distances (∼5% on average). However, by using a subsample of systems with the best agreement between their geometric and photometric distances, we derived the precise SBC relations based only on eclipsing binary stars. These relations have precisions that are comparable to the best available SBC relations based on interferometric angular diameters, and they are fully consistent with them. With very precise Gaia parallaxes becoming available in the near future, angular diameters with a precision better than 1% will be abundant. At that point, the main uncertainty in the total error budget of the SBC relations will come from transformations between different photometric systems, disentangling of component magnitudes, and for hot OB stars, the main uncertainty will come from the interstellar extinction determination. We argue that all these issues can be overcome with modern high-quality data and conclude that a precision better than 1% is entirely feasible.

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Section: Temperature and Reddeningmentioning

confidence: 99%

The Surface Brightness-color Relations Based on Eclipsing Binary Stars: Toward Precision Better than 1% in Angular Diameter Predictions

Graczyk

Konorski

Pietrzyński

et al. 2017

ApJ

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“…On the other hand, rotationrelated effects have been shown to be highly successful in explaining apparent age spreads in such clusters as a combination of different MS lifetimes for stars of different initial rotation rate but identical mass and metallicity (Bastian & de Mink 2009;D'Antona et al 2015), and inclination effects such as gravity darkening (Espinosa Lara & Rieutord 2011;Brandt & Huang 2015;Niederhofer et al 2015). As another example, different initial rotation velocities may provide a straightforward explanation for some cases of binary stars that do not both fit on a single isochrone (e.g., Suchomska et al 2015).…”

Section: Introductionmentioning

confidence: 99%

On the effect of rotation on populations of classical Cepheids

Anderson

Saio

Ekström

et al. 2016

A&A

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172

257

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Classical Cepheid variable stars (from hereon: Cepheids) are high-sensitivity probes of stellar evolution and fundamental tracers of cosmic distances. While rotational mixing significantly affects the evolution of Cepheid progenitors (intermediate-mass stars), the impact of the resulting changes in stellar structure and composition on Cepheids and their pulsational properties is hitherto unknown. Here we present the first detailed pulsational instability analysis of stellar evolution models that include the effects of rotation, for both fundamental mode and first overtone pulsation. We employ Geneva evolution models spanning a three-dimensional grid in mass (1.7-15 M ), metallicity (Z = 0.014, 0.006, 0.002), and rotation (non-rotating, average & fast rotation). We determine (1) hot and cool instability strip (IS) boundaries taking into account the coupling between convection and pulsation; (2) pulsation periods; and (3) rates of period change. We investigate relations between period and (a) luminosity; (b) age; (c) radius; (d) temperature; (e) rate of period change; (f) mass; (g) the flux-weighted gravity-luminosity relation (FWGLR). We confront all predictions aside from those for age with observations, finding generally excellent agreement. We tabulate period-luminosity relations (PLRs) for several photometric passbands and investigate how the finite IS width, different IS crossings, metallicity, and rotation affect PLRs. We show that a Wesenheit index based on H, V, and I photometry is expected to have the smallest intrinsic PLR dispersion. We confirm that rotation resolves the Cepheid mass discrepancy. Period-age relations depend significantly on rotation, with rotation leading to older Cepheids, offering a straightforward explanation for evolved stars in binary systems that cannot be matched by conventional isochrones assuming a single age. We further show that Cepheids obey a tight FWGLR. Rotation is a fundamental property of stars that has important implications for the study of intermediate-mass stars, intermediate-age clusters, and classical Cepheid variable stars.

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“…In order to determine the correct vsini we also took into account the macroturbulence velocities and the instrumental profile contributions, as described in Suchomska et al (2015). The macroturbulance velocities were estimated to be v mt1 =1.74 km s −1 and v mt2 =1.70 km s −1 for the primary and secondary components.…”

Section: Blg-123903mentioning

confidence: 99%

“…We also used the extinction maps of Schlegel et al (1998) with the recalibration of Schlafly & Finkbeiner (2011) to estimate the reddening in the direction of BLG-123903. We followed the description given in Suchomska et al (2015). We estimated the value of E(B − V) = 0.329 ± 0.059.…”

Section: Blg-123903mentioning

confidence: 99%

Accurate stellar parameters and distance to two evolved eclipsing binary systems, OGLE-BLG-ECL-123903 and OGLE-BLG-ECL-296596, towards the Galactic bulge

Suchomska

Graczyk

Pietrzyński

et al. 2019

A&A

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Aims. Our aim is to obtain high-accuracy measurements of the physical and orbital parameters of two evolved eclipsing binary systems, and to use these measurements to study their evolutionary status. We also aim to derive the distances to the systems by using a surface brightness-colour relation and compare these distances with the measurements provided by GAIA. Methods. We measured the physical and orbital parameters of both systems based on V-band and I-band photometry from OGLE, near-infrared photometry obtained with the NTT telescope and the instrument SOFI, as well as highresolution spectra obtained at ESO 3.6m/HARPS and Clay 6.5/MIKE spectrographs. The light curves and radialvelocity curves were analysed with the Wilson-Devinney code. Results. We analysed two double-lined eclipsing binary systems OGLE-BLG-ECL-123903 and OGLE-BLG-ECL-296596 from the Optical Gravitational Lensing Experiment (OGLE) catalogue. Both systems have a configuration of two welldetached giants stars. The masses of the components of OGLE-BLG-ECL-123903 are M 1 = 2.045 ± 0.027 and M 2 = 2.074 ± 0.023 M and the radii are R 1 = 9.540 ± 0.049 and R 2 = 9.052 ± 0.060 R . For OGLE-BLG-ECL-296596, the masses are M 1 = 1.093 ± 0.015 and M 2 = 1.125 ± 0.014 M , while the radii are R 1 = 18.06 ± 0.28 and R 2 = 29.80 ± 0.33 R . Evolutionary status was discussed based on the isochrones and evolutionary tracks from parsec and mesa codes. The ages of the systems were established to be around 1.3 Gyr for the OGLE-BLG-ECL-123903 and 7.7 Gyr for the OGLE-BLG-ECL-296596. We also determined the distance to both systems. For OGLE-BLG-ECL-123903 this is equal to d= 2.95 ± 0.06 (stat.) ± 0.07 (syst.) kpc, while for the OGLE-BLG-ECL-296596 it is d= 5.68 ± 0.07 (stat.) ± 0.14 (syst.) kpc. This is the first analysis of its kind for these unique evolved eclipsing binary systems.

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The Araucaria Project: accurate stellar parameters and distance to evolved eclipsing binary ASAS J180057-2333.8 in Sagittarius Arm

Cited by 24 publications

References 55 publications

The Surface Brightness-color Relations Based on Eclipsing Binary Stars: Toward Precision Better than 1% in Angular Diameter Predictions

The Surface Brightness-color Relations Based on Eclipsing Binary Stars: Toward Precision Better than 1% in Angular Diameter Predictions

On the effect of rotation on populations of classical Cepheids

Accurate stellar parameters and distance to two evolved eclipsing binary systems, OGLE-BLG-ECL-123903 and OGLE-BLG-ECL-296596, towards the Galactic bulge

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