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The Araucaria Project: High-Precision Orbital Parallax and Masses of Eclipsing Binaries from Infrared Interferometry? A

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The Araucaria Project: High-Precision Orbital Parallax and Masses of Eclipsing Binaries from Infrared Interferometry? A Astronomy & Astrophysics manuscript no. 2019-Eclipsing-v2r2 c ESO 2019 October 9, 2019 The Araucaria Project: High-precision orbital parallax and masses of eclipsing binaries from infrared interferometry? A. Gallenne1; 2, G. Pietrzynski´ 3; 4, D. Graczyk4; 5; 6, B. Pilecki3, J. Storm7, N.Nardetto1, M. Taormina3, W. Gieren4, A. Tkachenko8, P. Kervella9, A. Mérand10 and M. Weber7 1 European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Santiago, Chile 2 Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte dAzur, Nice, France 3 Nicolaus Copernicus Astronomical Centre, Polish Academy of Sciences, Bartycka 18, 00-716 Warszawa, Poland 4 Universidad de Concepción, Departamento de Astronomía, Casilla 160-C, Concepción, Chile 5 Millenium Institute of Astrophysics, Av. Vicuña Mackenna 4860, Santiago, Chile 6 Centrum Astronomiczne im. Mikołaja Kopernika, PAN, Rabianska´ 8, 87-100 Torun,´ Poland 7 Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany 8 Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium 9 LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, 92195 Meudon, France 10 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany Received May 06, 2019; accepted October 7, 2019 ABSTRACT Context. The precise determinations of stellar mass at . 1 % provide important constraints on stellar evolution models. Accurate parallax measurements can also serve as independent benchmarks for the next Gaia data release. Aims. We aim at measuring the masses and distance of binary systems with a precision level better than 1 % using a fully geometrical and empirical method. Methods. We obtained the first interferometric observations for the eclipsing systems AI Phe, AL Dor, KW Hya, NN Del, Cen and V4090 Sgr with the VLTI/PIONIER combiner, which we combined with radial velocity measurements to derive their three- dimensional orbit, masses, and distance. Results. We determined very precise stellar masses for all systems, ranging from 0.04 % to 3.3 % precision level. We combined these measurements with stellar effective temperature and linear radius to fit stellar isochrones models and determined the age of the systems. We also derived the distance to the systems with a precision level as high as 0.4 %. Conclusions. The comparison of theoretical models with stellar parameters shows that stellar models are still deficient in simultane- ously fitting the stellar parameters (Teff ; R and M) with such level of precision on individual masses. This stresses the importance of precisely measuring the stellar parameters to better calibrate stellar evolution models. The precision of our model-independent orbital parallaxes varies from 24µas as to 70µas and they provide a unique opportunity to check on the future Gaia measurements for possible systematic errors. Key words. techniques: interferometric – techniques: high angular resolution – stars: variables: Cepheids – star: binaries: close 1. Introduction Binary stars are the only tool enabling direct and accurate distance and stellar mass measurements. When they are double- In the course of the Araucaria project, different techniques for lined spectroscopic binaries, the geometric distance can be mea- distance measurement are applied in order to track down the in- sured, providing an independent benchmark to other measure- fluence of the population effects on the most important standard ments, such as for instance, the future Gaia parallax measure- candles like Cepheids, RR Lyrae stars, red clump stars, tip of the ments (Gaia Collaboration et al. 2016). The mass is a fundamen- red-giant branch, etc... (Gieren et al. 2005a,b). Binary systems tal parameter in order to understand the structure and evolution arXiv:1910.03393v1 [astro-ph.SR] 8 Oct 2019 are of particular importance in our project, as demonstrated in of stars, and precise measurements are necessary to check the our works with eclipsing binary systems, which have provided consistency with theoretical models and tighter the constraints. the most accurate distance of the Large and Small Magellanic For now, stellar parameters (e.g. the effective temperature, ra- Clouds (Pietrzynski´ et al. 2019, 2013; Graczyk et al. 2014). dius, ...) predicted from different stellar evolution codes can lead to discrepancies with the empirical values, and therefore provid- ing a large range of possible age for a given system (see e.g. Tor- Send offprint requests to: A. Gallenne res et al. 2010; Gallenne et al. 2016). Models of stellar interior ? Based on observations made with ESO telescopes at Paranal and La Silla observatory under program IDs 087.C-0012(A), 087.C- differ in various ways, as for instance in the input physics, the 0012(B), 089.C-0415(A), 089.C-0415(B), 092.C-0454(A), 093.C- initial chemical compositions, the treatment of convective-core 0417(A), 094.C-0428(A), 094.D-0056(A), 096.C-0417(A), 096.D- overshooting, the rotational mixing or the mixing length param- 0299(A), 097.D-0025(A), 097.C-0571(B), 098.C-0292(A), 0100.D- eter (Marigo et al. 2017; Bressan et al. 2012; Dotter et al. 2008; 0024(A), 0100.D-0339(B). Pietrinferni et al. 2004). With high-precision measurements, evo- Article number, page 1 of 22 A&A proofs: manuscript no. 2019-Eclipsing-v2r2 lutionary models can be tightly constrained and provide a better 2012; Sybilski et al. 2018). Recently, variations in the systemic understanding of the stellar interior physics (Higl et al. 2018; velocity seem to indicate that there is a possible wider compo- Claret & Torres 2018; Valle et al. 2017). nent in the system (M. Konacki, priv, comm.), however, no or- The precision on stellar parameters (Teff; R; M; :::) gradually bital parameters have been derived so far. improved with years thanks to eclipsing binary systems and Kirkby-Kent et al.(2016) provided precise mass measure- ground- and space-based large photometric surveys (e.g. OGLE, ments (∼ 0:3 %) which already enabled to test stellar evolution WASP, KEPLER, LSST, TESS, ...). Combining radial veloci- models, to constrain the mixing length and the helium abun- ties data with photometric observations during the eclipses, mea- dance, and to derive an age of 4:39 ± 0:32 Gyr. The last results surements at a ∼ 1 − 3 % precision level are routinely achieved of Sybilski et al.(2018) gave masses precise to ∼ 0:08 %, but (e.g. Pilecki et al. 2018; Pribulla et al. 2018; Kirkby-Kent et al. there is no additional information about the stellar evolution. A 2016; Graczyk et al. 2015; Pilecki et al. 2015; Gieren et al. 2015; third visual component located at about 1100was thought to be Pilecki et al. 2013), but recent work shows that precision on the also bound to the AI Phe system, however, Kirkby-Kent et al. stellar mass << 1 % is necessary to obtain reliable determina- (2016) concluded that it is not physically associated. tions of the stellar interior model parameters (overshooting, ini- From spectroscopic and photometric observations, Andersen tial helium abundance, ..., Higl et al. 2018; Valle et al. 2017). et al.(1988) derived the parallax to be 6 :17 ± 0:23 mas, consis- Another model-independent approach for measuring stellar tent with the 5:94 ± 0:24 mas from Graczyk et al.(2017) using masses and geometrical distances with binary systems at < 1 % the same method and the 5:98 ± 0:31 mas from Stassun & Tor- accuracy is to combine spectroscopic and astrometric observa- res(2016) from absolute stellar luminosity and bolometric flux tions (see e.g. Pribulla et al. 2018; Gallenne et al. 2016; Torres fitting. The value from Hipparcos (van Leeuwen 2007, assum- et al. 2009; Zwahlen et al. 2004; Morbey 1975; Herbison-Evans ing a single star) is ∼ 2σ away from the more recent estimate et al. 1971). This method does not require any assumptions. This (Graczyk et al. 2017), but the Gaia measurement is within 1σ has been recently applied to a Galactic binary Cepheid and has with 5:8336 ± 0:0262 mas (Gaia Collaboration et al. 2018). provided the most accurate distance and mass for a Milky Way Cepheid (Gallenne et al. 2018a). However, the systems need to be spatially resolved to enable astrometric measurements, which AL Doradus: This eclipsing system has two identical main- is not always the case with single-dish telescope observations sequence stars orbiting each other with a period of 14:9 d where the components are too close. A higher angular resolu- (G0V+F9V Graczyk et al. 2019). It was identified to be eclips- tion is provided from optical long-baseline interferometry (LBI), ing by Kazarovets et al.(1999) and has been poorly moni- where close-in binary systems (< 20 mas) can be detected. LBI tored in the past. The orbital parameters where only recently already proved its efficiency in terms of angular resolution and derived by Graczyk et al.(2019) combining new photometric accuracy for close-in binary stars (see e.g. Pribulla et al. 2018; and spectroscopic observations, but they did not provide esti- Gallenne et al. 2018a, 2016, 2015, 2014, 2013; Le Bouquin et al. mates of the masses and the distance. The parallax from Gaia 2013; Baron et al. 2012). is 15:1292 ± 0:0286 mas, which corresponds to a distance of Recent work using LBI with eclipsing systems provided the 66:97±0:13 pc, while the Hipparcos measurement (van Leeuwen most precise distances and masses for such systems, i.e. < 0:4 % 2007) has a lower accuracy with 16:07 ± 0:43 mas, but roughly and < 0:1 % respectively (Pribulla et al. 2018; Gallenne et al. agrees with each other. 2018b, 2016). Valle et al.(2017) demonstrated that such very precise mass determinations are required to obtain reliable de- KW Hydrae: The primary star is a chemically peculiar post- terminations of stellar parameters such as the convective core main-sequence A-type star (A5m, with metallic lines), and dis- overshooting, the initial helium abundance and the age of the covered to be double-lined spectroscopic binary by Chauville system.
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