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1. Calibrating the surface brightness - color relation for late-type red giants stars in the visible domain using VEGA/CHARA interferometric observations

Author

Nardetto, N., Salsi, A., Mourard, D., Hocde, V., Perraut, K., Gallenne, A., Merand, A., Graczyk, D., Pietrzynski, G., Gieren, W., Kervella, P., Ligi, R., Meilland, A., Morand, F., Stee, P., Tallon-Bosc, I., and ten~Brummelaar, T.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

The surface brightness - color relationship (SBCR) is a poweful tool for determining the angular diameter of stars from photometry. It was for instance used to derive the distance of eclipsing binaries in the Large Magellanic Cloud (LMC), which led to its distance determination with an accuracy of 1%. We calibrate the SBCR for red giant stars in the 2.1 < V-K < 2.5 color range using homogeneous VEGA/CHARA interferometric data secured in the visible domain, and compare it to the relation based on infrared interferometric observations, which were used to derive the distance to the LMC. Observations of eight G-K giants were obtained with the VEGA/CHARA instrument. The derived limb-darkened angular diameters were combined with a homogeneous set of infrared magnitudes in order to constrain the SBCR. The average precision we obtain on the limb-darkened angular diameters of the eight stars in our sample is 2.4%. For the four stars in common observed by both VEGA/CHARA and PIONIER/VLTI, we find a 1 sigma agreement for the angular diameters. The SBCR we obtain in the visible has a dispersion of 0.04 magnitude and is consistent with the one derived in the infrared (0.018 magnitude). The consistency of the infrared and visible angular diameters and SBCR reinforces the result of 1% precision and accuracy recently achieved on the distance of the LMC using the eclipsing-binary technique. It also indicates that it is possible to combine interferometric observations at different wavelengths when the SBCR is calibrated., Comment: 9 pages, in press in A&A revue

Published
2020
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2. Development of a Fiber Connectorized Ultrafast Laser Inscribed 2-Telescope Beam Combiner for the CHARA Telescope Array

Author

Benoît, A., primary, Siliprandi, J., additional, MacLachlan, D. G., additional, Ross, C. A., additional, Sharma, T. K., additional, Labadie, L., additional, Madhav, K., additional, Nayak, A. S., additional, Dinkelaker, A. N., additional, Roth, M. M., additional, Pedretti, E., additional, Ten Brummelaar, T. A., additional, Scott, N. J., additional, Du Foresto, V. Condé, additional, and Thomson, R. R., additional

Published
2023
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3. Multiplicity of northern bright O-type stars with optical long baseline interferometry

Author

Lanthermann, C., primary, Le Bouquin, J.-B., additional, Sana, H., additional, Mérand, A., additional, Monnier, J. D., additional, Perraut, K., additional, Frost, A. J., additional, Mahy, L., additional, Gosset, E., additional, De Becker, M., additional, Kraus, S., additional, Anugu, N., additional, Davies, C. L., additional, Ennis, J., additional, Gardner, T., additional, Labdon, A., additional, Setterholm, B., additional, ten Brummelaar, T., additional, and Schaefer, G. H., additional

Published
2023
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4. Multiplicity of northern bright O-type stars with optical long baseline interferometry

Author

Lanthermann, C., Le Bouquin, J.-B., Sana, H., Mérand, A., Monnier, J. D., Perraut, K., Frost, A. J., Mahy, L., Gosset, E., De Becker, M., Kraus, S., Anugu, N., Davies, C. L., Ennis, J., Gardner, T., Labdon, A., Setterholm, B., ten Brummelaar, T., and Schaefer, G. H.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The study of the multiplicity of massive stars gives hints on their formation processes and their evolutionary paths, which are still not fully understood. Large separation binaries (>50 milliseconds of arc, mas) can be probed by adaptive-optics-assisted direct imaging and sparse aperture masking, while close binaries can be resolved by photometry and spectroscopy. However, optical long baseline interferometry is mandatory to establish the multiplicity of Galactic massive stars at the separation gap between 1 and 50 mas. In this paper, we aim to demonstrate the capability of the new interferometric instrument MIRC-X, located at the CHARA Array, to study the multiplicity of O-type stars and therefore probe the full range of separation for more than 120 massive stars (H, 15 pages, 9 figures, 5 tables, accepted in A&A

Published
2023
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5. A Long-Term Vision for Space-Based Interferometry

Author

Rinehart, S. A, Arenberg, J, Baines, E, Chen, C. H, Cleeves, L. IIsedore, Creech-Eakman, M. J, Dale, D, Danchi, W, Farrah, D, Juanola-Parramon, R, Kraus, S, Knight, J. S, Lipscy, S, Leisawitz, D. T, MacGregor, M. A, Mennesson, B, Monnier, J, Naylor, D. A, O'Connor, R, Roberge, A, Savini, G, Schmitt, H, Sewilo, M, ten Brummelaar, T. A, van Belle, G, and Yorke, H. W

Subjects
Astrophysics
Abstract

The processes leading to the formation of planets; the extreme physics occurring near the event horizon of black holes; detailed studies of exoplanets through spectral-spatial mapping: new and unique insights into the physical processes involved across nearly the whole gamut of astrophysics await discovery at small angular scales. The fine spatial resolution needed to explore these processes, however, lies beyond the capabilities of current astronomical facilities and nearly all proposed future facilities. Interferometers can crack this angular resolution problem, and space-based interferometry missions promise to explore entirely new regions of scientific phase space, providing unique new insights into the physical processes lurking at small angular scales.

Published
2019

6. Limb Darkening: Getting Warmer

Author

Aufdenberg, J. P., Ludwig, H.-G., Kervella, P., Mérand, A., Ridgway, S. T., Coudé du Foresto, V., ten Brummelaar, T. A., Berger, D. H., Sturmann, J., Turner, N. H., Leibundgut, Bruno, editor, Richichi, A., editor, Delplancke, F., editor, Paresce, F., editor, and Chelli, A., editor

Published
2008
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7. No Sun-like dynamo on the active star Andromedae from starspot asymmetry

Author

Roettenbacher, R. M., Monnier, J. D., Korhonen, H., Aarnio, A. N., Baron, F., Che, X., Harmon, R. O., Kvri, Zs., Kraus, S., Schaefer, G. H., Torres, G., Zhao, M., ten Brummelaar, T. A., Sturmann, J., and Sturmann, L.

Subjects
Andromeda (Constellation) -- Observations, Symmetry (Physics) -- Observations, Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract

Author(s): R. M. Roettenbacher (corresponding author) [1]; J. D. Monnier [1]; H. Korhonen [2, 3]; A. N. Aarnio [1]; F. Baron [1, 4]; X. Che [1]; R. O. Harmon [5]; [...]

Published
2016
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8. A detailed analysis of the Gl 486 planetary system

Author

Caballero, J. A., primary, González-Álvarez, E., additional, Brady, M., additional, Trifonov, T., additional, Ellis, T. G., additional, Dorn, C., additional, Cifuentes, C., additional, Molaverdikhani, K., additional, Bean, J. L., additional, Boyajian, T., additional, Rodríguez, E., additional, Sanz-Forcada, J., additional, Zapatero Osorio, M. R., additional, Abia, C., additional, Amado, P. J., additional, Anugu, N., additional, Béjar, V. J. S., additional, Davies, C. L., additional, Dreizler, S., additional, Dubois, F., additional, Ennis, J., additional, Espinoza, N., additional, Farrington, C. D., additional, López, A. García, additional, Gardner, T., additional, Hatzes, A. P., additional, Henning, Th., additional, Herrero, E., additional, Herrero-Cisneros, E., additional, Kaminski, A., additional, Kasper, D., additional, Klement, R., additional, Kraus, S., additional, Labdon, A., additional, Lanthermann, C., additional, Le Bouquin, J.-B., additional, González, M. J. López, additional, Luque, R., additional, Mann, A. W., additional, Marfil, E., additional, Monnier, J. D., additional, Montes, D., additional, Morales, J. C., additional, Pallé, E., additional, Pedraz, S., additional, Quirrenbach, A., additional, Reffert, S., additional, Reiners, A., additional, Ribas, I., additional, Rodríguez-López, C., additional, Schaefer, G., additional, Schweitzer, A., additional, Seifahrt, A., additional, Setterholm, B. R., additional, Shan, Y., additional, Shulyak, D., additional, Solano, E., additional, Sreenivas, K. R., additional, Stefánsson, G., additional, Stürmer, J., additional, Tabernero, H. M., additional, Tal-Or, L., additional, ten Brummelaar, T., additional, Vanaverbeke, S., additional, von Braun, K., additional, Youngblood, A., additional, and Zechmeister, M., additional

Published
2022
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14. The expanding fireball of Nova Delphini 2013

Author

Schaefer, G. H., ten Brummelaar, T., Gies, D. R., Farrington, C. D., Kloppenborg, B., Chesneau, O., Monnier, J. D., Ridgway, S. T., Scott, N., Tallon-Bosc, I., McAlister, H. A., Boyajian, T., Maestro, V., Mourard, D., Meilland, A., Nardetto, N., Stee, P., Sturmann, J., Vargas, N., Baron, F., Ireland, M., Baines, E. K., Che, X., Jones, J., Richardson, N. D., Roettenbacher, R. M., Sturmann, L., Turner, N. H., Tuthill, P., van Belle, G., von Braun, K., Zavala, R. T., Banerjee, D. P. K., Ashok, N. M., Joshi, V., Becker, J., and Muirhead, P. S.

Published
2014
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15. Interferometric Imaging of λ Andromedae: Evidence of Starspots and Rotation

Author

Parks, J. R., primary, White, R. J., additional, Baron, F., additional, Monnier, J. D., additional, Kloppenborg, B., additional, Henry, G. W., additional, Schaefer, G., additional, Che, X., additional, Pedretti, E., additional, Thureau, N., additional, Zhao, M., additional, ten Brummelaar, T., additional, McAlister, H., additional, Ridgway, S. T., additional, Turner, N., additional, Sturmann, J., additional, and Sturmann, L., additional

Published
2021
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16. Imaging the surface of Altair

Author

Monnier, John D., Zhao, M., Pedretti, E., Thureau, N., Ireland, M., Muirhead, P., Berger, J.-P., Millan-Gabet, R., Van Belle, G., ten Brummelaar, T., McAlister, H., Ridgway, S., Turner, N., Sturmann, L., Sturmann, J, and Berger, D.

Subjects
Gravity anomalies -- Observations, Stars -- Observations, Stellar evolution -- Observations, Very long baseline interferometry -- Usage
Published
2007

17. Optical interferometry and Gaia measurement uncertainties reveal the physics of asymptotic giant branch stars

Author

Chiavassa, A., Kravchenko, K., Millour, F., Schaefer, G., Schultheis, M., Freytag, Bernd, Creevey, O., Hocde, V., Morand, F., Ligi, R., Kraus, S., Monnier, J. D., Mourard, D., Nardetto, N., Anugu, N., Le Bouquin, J. -B, Davies, C. L., Ennis, J., Gardner, T., Labdon, A., Lanthermann, C., Setterholm, B. R., ten Brummelaar, T., Chiavassa, A., Kravchenko, K., Millour, F., Schaefer, G., Schultheis, M., Freytag, Bernd, Creevey, O., Hocde, V., Morand, F., Ligi, R., Kraus, S., Monnier, J. D., Mourard, D., Nardetto, N., Anugu, N., Le Bouquin, J. -B, Davies, C. L., Ennis, J., Gardner, T., Labdon, A., Lanthermann, C., Setterholm, B. R., and ten Brummelaar, T.

Abstract

Context. Asymptotic giant branch (AGB) stars are cool luminous evolved stars that are well observable across the Galaxy and populating Gaia data. They have complex stellar surface dynamics, which amplifies the uncertainties on stellar parameters and distances.Aims. On the AGB star CL Lac, it has been shown that the convection-related variability accounts for a substantial part of the Gaia DR2 parallax error. We observed this star with the MIRC-X beam combiner installed at the CHARA interferometer to detect the presence of stellar surface inhomogeneities.Methods. We performed the reconstruction of aperture synthesis images from the interferometric observations at different wavelengths. Then, we used 3D radiative hydrodynamics (RHD) simulations of stellar convection with CO5BOLD and the post-processing radiative transfer code OPTIM3D to compute intensity maps in the spectral channels of MIRC-X observations. Then, we determined the stellar radius using the average 3D intensity profile and, finally, compared the 3D synthetic maps to the reconstructed ones focusing on matching the intensity contrast, the morphology of stellar surface structures, and the photocentre position at two different spectral channels, 1.52 and 1.70 mu m, simultaneously.Results. We measured the apparent diameter of CL Lac at two wavelengths (3.299 0.005 mas and 3.053 +/- 0.006 mas at 1.52 and 1.70 mu m, respectively) and recovered the radius (R = 307 +/- 41 and R = 284 +/- 38 R-circle dot) using a Gaia parallax. In addition to this, the reconstructed images are characterised by the presence of a brighter area that largely affects the position of the photocentre. The comparison with 3D simulation shows good agreement with the observations both in terms of contrast and surface structure morphology, meaning that our model is adequate for explaining the observed inhomogenities.Conclusions. This work confirms the presence of convection-related surface structures on an AGB star of Gaia DR2. Our result w

Published
2020
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18. HD 181068: A Red Giant in a Triply Eclipsing Compact Hierarchical Triple System

Author

Derekas, A., Kiss, L. L., Borkovits, T., Huber, D., Lehmann, H., Southworth, J., Bedding, T. R., Balam, D., Hartmann, M., Hrudkova, M., Ireland, M. J., Kovács, J., Mezö, Gy., Moór, A., Niemczura, E., Sarty, G. E., Szabó, Gy. M., Szabó, R., Telting, J. H., Tkachenko, A., Uytterhoeven, K., Benkö, J. M., Bryson, S. T., Maestro, V., Simon, A. E., Stello, D., Schaefer, G., Aerts, C., ten Brummelaar, T. A., De Cat, P., McAlister, H. A., Maceroni, C., Mérand, A., Still, M., Sturmann, J., Sturmann, L., Turner, N., Tuthill, P. G., Christensen-Dalsgaard, J., Gilliland, R. L, Kjeldsen, H., Quintana, E. V., Tenenbaum, P., and Twicken, J. D.

Published
2011
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20. Optical interferometry and Gaia measurement uncertainties reveal the physics of asymptotic giant branch stars

Author

Chiavassa, A., primary, Kravchenko, K., additional, Millour, F., additional, Schaefer, G., additional, Schultheis, M., additional, Freytag, B., additional, Creevey, O., additional, Hocdé, V., additional, Morand, F., additional, Ligi, R., additional, Kraus, S., additional, Monnier, J. D., additional, Mourard, D., additional, Nardetto, N., additional, Anugu, N., additional, Le Bouquin, J.-B., additional, Davies, C. L., additional, Ennis, J., additional, Gardner, T., additional, Labdon, A., additional, Lanthermann, C., additional, Setterholm, B. R., additional, and ten Brummelaar, T., additional

Published
2020
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21. Calibrating the surface brightness – color relation for late-type red giants stars in the visible domain using VEGA/CHARA interferometric observations

Author

Nardetto, N., primary, Salsi, A., additional, Mourard, D., additional, Hocdé, V., additional, Perraut, K., additional, Gallenne, A., additional, Mérand, A., additional, Graczyk, D., additional, Pietrzynski, G., additional, Gieren, W., additional, Kervella, P., additional, Ligi, R., additional, Meilland, A., additional, Morand, F., additional, Stee, P., additional, Tallon-Bosc, I., additional, and ten Brummelaar, T., additional

Published
2020
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22. Visible and near-infrared spectro-interferometric analysis of the edge-on Be star o Aquarii

Author

de Almeida, E. S. G., primary, Meilland, A., additional, Domiciano de Souza, A., additional, Stee, P., additional, Mourard, D., additional, Nardetto, N., additional, Ligi, R., additional, Tallon-Bosc, I., additional, Faes, D. M., additional, Carciofi, A. C., additional, Bednarski, D., additional, Mota, B. C., additional, Turner, N., additional, and ten Brummelaar, T. A., additional

Published
2020
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23. The CHARA Michelson Array Pathfinder

Author

Mérand, Antoine, Sallum, Stephanie, Sanchez-Bermudez, Joel, Ligon, R., Anderson, M., Anugu, N., ten Brummelaar, T., Farrington, C., Gies, D., Golden, S., Koehler, R., Reynaud, F., Ridgway, S., Schaefer, G., Scott, N., Sturmann, L., Turner, N., and Woods, C.

Published
2022
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24. The Future of Exoplanet Direct Detection

Author

Monnier, J., Rau, G., Baines, E., Sanchez-Bermudez, J., Elvis, M., Ragland, S., Akeson, R., van Belle, G., Norris, R., Gordon, K., Defrère, D., Ridgway, S., Le Bouquin, J., Anugu, N., Scott, N., Kane, S., Richardson, N., Regaly, Z., Zhu, Z., Chiavassa, A., Vasisht, G., Stassun, K., Dong, C., Absil, O., Lacour, S., Weigelt, G., Gies, D., Adams, F., Calvet, N., Quanz, S., Espaillat, C., Gardner, T., Greenbaum, A., Millan-Gabet, R., Packham, C., Gai, M., Kral, Q., Berger, J., Linz, H., Klarmann, L., Bae, J., Lopez Garcia, R., Alexandre, G., Baron, F., Hartmann, L., Kishimoto, M., McClure, M., Olofsson, J., Haniff, C., Line, M., Petrov, R., Smith, M., Hummel, C., ten Brummelaar, T., De Furio, M., Rinehart, S., Leisawitz, D., Danchi, W., Huber, D., Wishnow, E., Mourard, D., Pope, B., Ireland, M., Kraus, S., Setterholm, B., White, R., ITA, USA, GBR, FRA, DEU, ESP, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Computer Science::Digital Libraries, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract

International audience; Diffraction fundamentally limits our ability to image and characterize exoplanets. Interferometry offers some advantages in exoplanet detection and characterization and we explore in this white paper some of the potential scientific breakthroughs possible.

Published
2019

25. Imaging the Key Stages of Planet Formation

Author

Monnier, J., Rau, G., Bermudez, J., Ragland, S., Akeson, R., Duchene, G., van Belle, G., Norris, R., Gordon, K., Defrère, D., Kluska, J., Ridgway, S., Le Bouquin, J., Anugu, N., Scott, N., Kane, S., Richardson, N., Regaly, Z., Zhu, Z., Vasisht, G., Stassun, K., Andrews, S., Lacour, S., Weigelt, G., Turner, N., Adams, F., Gies, D., Calvet, N., Espaillat, C., Millan-Gabet, R., Gardner, T., Packham, C., Gai, M., Kral, Q., Berger, J., Linz, H., Klarmann, L., Bate, M., Bae, J., Lopez, R., Garufi, A., Baron, F., Kama, M., Wilner, D., Hartmann, L., Kishimoto, M., Olofsson, J., McClure, M., Haniff, C., Hoenig, S., Line, M., Petrov, R., Smith, M., ten Brummelaar, T., De Furio, M., Koutoulaki, M., Rinehart, S., Leisawitz, D., Danchi, W., Huber, D., Zhang, K., Pope, B., Ireland, M., Kraus, S., Isella, A., Setterholm, B., White, R., University of Michigan [Ann Arbor], University of Michigan System, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract

International audience; In this white paper, we explore how higher angular resolution beyond ALMA and 8m-class telescopes can extend our understanding of the key stages of planet formation, to resolve accreting circumplanetary disks themselves, and to watch planets forming in situ for the nearest star-forming regions.

Published
2019

27. Fibered visible interferometry and adaptive optics: FRIEND at CHARA

Author

Martinod, M A, Mourard, D, Bério, P, Perraut, K, Meilland, A, Bailet, C, Bresson, Y, ten Brummelaar, T, Clausse, J M, Dejonghe, J, Ireland, Michael, Martinod, M A, Mourard, D, Bério, P, Perraut, K, Meilland, A, Bailet, C, Bresson, Y, ten Brummelaar, T, Clausse, J M, Dejonghe, J, and Ireland, Michael

Abstract

Aims. In the context of the future developments of long baseline interferometry at visible wavelengths, we have built a prototype instrument called Fibered spectrally Resolved Interferometer - New Design (FRIEND) based on single mode fibers and a new generation detector called Electron Multiplying Charge-Coupled Device (EMCCD). Installed on the Center for High Angular Resolution Astronomy (CHARA) array, it aims to estimate the performance of a fibered instrument in the visible when coupled with telescopes equipped with adaptive optics (AO) in partial correction. Methods. We observed different sequences of targets and reference stars to study the compensation of the birefringence of the fibers, the coupling efficiency in various conditions of correction, and to calibrate our numerical model of signal-to-noise ratio (S/N). We also used a known binary star to demonstrate the reliability and the precision of our squared visibility and closure phase measurements. Results. We firstly present a reliable and stable solution for compensating the birefringence of the fibers with an improvement of a factor of 1.5 of the instrumental visibility. We then demonstrate an improvement by a factor of between 2.5 and 3 of the coupling efficiency when using the LABAO systems in closed loop. The third results of our paper is the demonstration of the correct calibration of the parameters of our S/N estimator provided the correct excess noise factor of EMCCD is correctly taken into account. Finally with the measurements of the angular separation, difference of magnitude and individual diameters of the two components of zeta Ori A, we demonstrate the reliability and precision of our interferometric estimators, and in particular a median residual on the closure phase of 1.2 degrees

Published
2018

28. Interferometric Constraints on Gravity Darkening with Application to the Modeling of Spica A & B

Author

Aufdenberg, J.P., Ireland, M. J., Mérand, A., du Foresto, V. Coudé, Absil, O., Folco, E. Di, Kervella, P., Bagnuolo, W. G., Gies, D. R., Ridgway, S. T., Berger, D. H., ten Brummelaar, T. A., McAlister, H. A., Sturmann, J., Sturmann, L., Turner, N. H., and Jacob, A. P.

Subjects
Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract

In 2005 we obtained very precise interferometric measurements of the pole-on rapid rotator Vega (A0 V) with the longest baselines of the Center for High Angular Angular Resolution (CHARA) Array and the Fiber Linked Unit for Optical Recombination (FLUOR). For the analysis of these data, we developed a code for mapping sophisticated PHOENIX model atmospheres on to the surface of rotationally distorted stars described by a Roche-von Zeipel formalism. Given a set of input parameters for a star or binary pair, this code predicts the interferometric visibility, spectral energy distribution and high-resolution line spectrum expected for the system. For the gravity-darkened Vega, our model provides a very good match to the K-band interferometric data, a good match to the spectral energy distribution - except below 160 nm - and a rather poor match to weak lines in the high dispersion spectrum where the model appears overly gravity darkened. In 2006, we used the CHARA Array and FLUOR to obtain high precision measurements of the massive, non-eclipsing, double-line spectroscopic binary Spica, a 4-day period system where both components are gravity darkened rapid rotators. These data supplement recent data obtained with the Sydney University Stellar Interferometer (SUSI). Our study follows the classic 1971 study by Herbison-Evans et al. who resolved Spica as a binary with the Narrabri Stellar Intensity Interferometer (NSII). We will report on our progress modeling the new interferometric and archival spectroscopic data, with the goal towards better constraining the apsidal constant

Published
2017

29. Fibered visible interferometry and adaptive optics: FRIEND at CHARA

Author

Martinod, M. A., primary, Mourard, D., additional, Bério, P., additional, Perraut, K., additional, Meilland, A., additional, Bailet, C., additional, Bresson, Y., additional, ten Brummelaar, T., additional, Clausse, J. M., additional, Dejonghe, J., additional, Ireland, M., additional, Millour, F., additional, Monnier, J. D., additional, Sturmann, J., additional, Sturmann, L., additional, and Tallon, M., additional

Published
2018
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31. Orbital Elements and Stellar Parameters of the Active Binary UX Arietis

Author

Hummel, C. A., Monnier, J. D., Roettenbacher, Rachael M., Torres, G., Henry, G. W., Korhonen, H., Beasley, A., Schaefer, G. H., Turner, N. H., Ten Brummelaar, T., Farrington, C. D., Sturmann, J., Sturmann, L., Baron, F., Kraus, S., Hummel, C. A., Monnier, J. D., Roettenbacher, Rachael M., Torres, G., Henry, G. W., Korhonen, H., Beasley, A., Schaefer, G. H., Turner, N. H., Ten Brummelaar, T., Farrington, C. D., Sturmann, J., Sturmann, L., Baron, F., and Kraus, S.

Abstract

Stellar activity observed as large surface spots, radio flares, or emission lines is often found in binary systems. UX Arietis exhibits these signs of activity, originating on the K0 subgiant primary component. Our aim is to resolve the binary, measure the orbital motion, and provide accurate stellar parameters such as masses and luminosities to aid in the interpretation of the observed phenomena. Using the CHARA six-telescope optical long-baseline array on Mount Wilson, California, we obtained amplitudes and phases of the interferometric visibility on baselines up to 330 m in length, resolving the two components of the binary. We reanalyzed archival Center for Astrophysics spectra to disentangle the binary component spectra and the spectrum of the third component, which was resolved by speckle interferometry. We also obtained new spectra with the Nordic Optical Telescope, and we present new photometric data that we use to model stellar surface spot locations. Both interferometric visibilities and spectroscopic radial velocities are modeled with a spotted primary stellar surface using the Wilson-Devinney code. We fit the orbital elements to the apparent orbit and radial velocity data to derive the distance (52.1 +/- 0.8 pc) and stellar masses (M-P = 1.30 +/- 0.06 M-circle dot, M-S = 1.14 +/- 0.06 M-circle dot). The radius of the primary can be determined to be R-P = 5.6 +/- 0.1 R-circle dot and that of the secondary to be R-S = 1.6 +/- 0.2 R-circle dot. The equivalent spot coverage of the primary component was found to be 62% with an effective temperature 20% below that of the unspotted surface.

Published
2017
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32. Asymmetries on red giant branch surfaces from CHARA/MIRC optical interferometry

Author

Chiavassa, A., Norris, R. P., Montargés, M., Ligi, R., Fossati, L., Bigot, L., Baron, F., Kervella, P., Monnier, J. D., Mourard, D., Nardetto, N., Perrin, G., Schaefer, G. H., ten Brummelaar, T. A., Magic, Zazralt, Collet, R., Asplund, M., Chiavassa, A., Norris, R. P., Montargés, M., Ligi, R., Fossati, L., Bigot, L., Baron, F., Kervella, P., Monnier, J. D., Mourard, D., Nardetto, N., Perrin, G., Schaefer, G. H., ten Brummelaar, T. A., Magic, Zazralt, Collet, R., and Asplund, M.

Published
2017

33. VEGA/CHARA interferometric observations of Cepheids

Author

Nardetto, N., Mérand, A., Mourard, D., Storm, J., Gieren, W., Fouqué, P., Gallenne, A., Graczyk, D., Kervella, P., Neilson, H., Pietrzynski, G., Pilecki, B., Breitfelder, J., Berio, P., Challouf, M., Clausse, J.-M., Ligi, R., Mathias, P., Meilland, A., Perraut, K., Poretti, E., Rainer, M., Spang, A., Stee, P., Tallon-Bosc, I., ten Brummelaar, T., Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Osservatorio Astronomico di Brera, Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL)

Subjects
[PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2016
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34. The fundamental parameters of the roAp star HD 24712

Author

Perraut, K., Brandão, I., Cunha, M., Shulyak, D., Mourard, D., Nardetto, N., Ten Brummelaar, T., Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2016
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35. A near-infrared interferometric survey of debris-disc stars

Author

Nuñez, P. D., primary, Scott, N. J., additional, Mennesson, B., additional, Absil, O., additional, Augereau, J.-C., additional, Bryden, G., additional, ten Brummelaar, T., additional, Ertel, S., additional, Coudé du Foresto, V., additional, Ridgway, S. T., additional, Sturmann, J., additional, Sturmann, L., additional, Turner, N. J., additional, and Turner, N. H., additional

Published
2017
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36. Asymmetries on red giant branch surfaces from CHARA/MIRC optical interferometry

Author

Chiavassa, A., primary, Norris, R., additional, Montargès, M., additional, Ligi, R., additional, Fossati, L., additional, Bigot, L., additional, Baron, F., additional, Kervella, P., additional, Monnier, J. D., additional, Mourard, D., additional, Nardetto, N., additional, Perrin, G., additional, Schaefer, G. H., additional, ten Brummelaar, T. A., additional, Magic, Z., additional, Collet, R., additional, and Asplund, M., additional

Published
2017
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37. First Images of Cool Starspots on a Star Other than the Sun: Interferometric Imaging of $\lambda$ Andromedae

Author

Parks, J. R., White, R. J., Baron, F., John D Monnier, Kloppenborg, B., Henry, G., Scheafer, G., Che, X., Pedretti, E., Thureau, N., Zhao, M., Ten Brummelaar, T., Mcalister, H., Ridgway, S. T., Turner, N., Sturmann, J., and Sturmann, L.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Presented are the first interferometric images of cool starspots on the chromospherically active giant $\lambda$ Andromedae. These images represent the first model-independent images of cool starspots on a star other than the Sun to date. The interferometric observations, taken with the Michigan Infra-Red Combiner coupled to the Center for High Angular Resolution Astronomy Array, span 26 days from Aug 17$^{th}$, 2008 to Sep 24$^{th}$, 2011. The photometric time series acquired at Fairborn Observatory spanning Sep 20$^{th}$, 2008 to Jan 20$^{th}$, 2011 is also presented. The angular diameter and power law limb-darkening coefficient of this star are 2.759 $\pm$ 0.050 mas and 0.229 $\pm$ 0.111, respectively. Starspot properties are obtained from both modeled and SQUEEZE reconstructed images. The images from 2010 through 2011 show anywhere from one to four starspots. The measured properties of identical starspots identified in both the model and reconstructed images are within two $\sigma$ error bars in 51$\%$ of cases. The cadence in the data for the 2010 and 2011 data sets are sufficient to measure a stellar rotation period based on apparent starspot motion. This leads to estimates of the rotation period (P$_{2010}$ = 60 $\pm$ 13 days, P$_{2011}$ = 54.0 $\pm$ 7.6 days) that are consistent with the photometrically determined period of 54.8 days. In addition, the inclination and position angle of the rotation axis is computed for both the 2010 and 2011 data sets; values ($\bar{\Psi}$ = 21.5$\degree$, $\bar{\emph{i}}$ = 78.0$\degree$) for each are nearly identical between the two years. \end{abstract}

Published
2015

38. The fundamental parameters of the Ap star 78 Virginis

Author

Perraut, K., Cunha, M., Brandão, I., Loridat, J., Mourard, D., Meilland, A., Nardetto, N., Mcalister, H., Ten Brummelaar, T., Sturmann, J., Sturmann, L., Turner, N., Farrington, C., Vargas, N., Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2015
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39. Robust high-contrast companion detection from interferometric observations

Author

Gallenne, A., Mérand, A., Kervella, P., Monnier, J., Schaefer, G., Baron, F., Breitfelder, J., Le Bouquin, J., Roettenbacher, R., Gieren, W., Pietrzyński, G., Mcalister, H., Ten Brummelaar, T., Sturmann, J., Sturmann, L., Turner, N., Ridgway, S., Kraus, S., European Southern Observatory (ESO), Laboratoire Franco-Chilien d'Astronomie (LFCA), Universidad de Chile = University of Chile [Santiago] (UCHILE)-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Concepción - University of Concepcion [Chile], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Georgia State University, University System of Georgia (USG), Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Center for High Angular Resolution Astronomy (CHARA), University System of Georgia (USG)-University System of Georgia (USG), National Optical Astronomy Observatory (NOAO), Max-Planck-Institut für Radioastronomie (MPIFR), Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Chile, Université Nice Sophia Antipolis (... - 2019) (UNS), and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2015
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40. VizieR Online Data Catalog: Pulsation model data for delta Cep and eta Aql (Merand+, 2015)

Author

Merand, A., Kervella, P., Breitfelder, J., Gallenne, A., Coude Du Foresto, V., ten Brummelaar, T. A., Mcalister, H. A., Ridgway, S., Sturmann, L., Sturmann, J., Turner, N. H., and bibliotheque, la.

Subjects
Models, Stars: distances, Stars: variable, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph]
Abstract

FITS files containing the stars' (delta Cep and eta Aql) data and model presented in the paper. Each fits file has 3 HDU: 1- primary HDU: contains no data apart from the header. The header has the parameters of the model (keywords 'HIERARCH PARAM') as well as some other quantities derived from the modeling (keywords 'HIERARCH MODEL'). These quantities are aimed at people who would like to reproduce or compare their results with us. 2- 'DATA' HDU: this contains the data used for the fit. Each line is a scalar measurement described as follow: col1='MJD' (E) modified Julian date of the observations col2='OBS' (A50) description of the data point: the string before ";" defines the type, after ";" is the source. after | are anciliary data: for diam, UDdiam: [wavelengthum, interfbaseline_m] for mag: photometric band for color: photometric band1 - photometric band2 col3='MEAS' (E) the actual measurements. units are km/s for Vpuls or Vrad (which includes the p-factor correction), and mas (milli-arcseconds) for diameters (diam of UDdiam). col4='ERR' (E) the uncertainty on the measurement. col5='MODEL' (E) corresponding value predicted by the model col6='PHASE' (E) pulsation phase computed from the model ranges from 0 to 1. col7='PERIOD' (E) pulsation period computed from the model in days 3- 'MODEL' HDU: a tabulation of the pulsation model, as a function of pulsation phase. col1='PHASE' (E) phase from 0 to 1. col2='Vpuls' (E) pulsation velocity, in km/s. col3='Vrad' (E) radial velocity, in km/s. It is Vpuls/p-factor + Vgamma. col4='diam' (E) Rosseland angular diameter, in milliarcseconds (mas). col5='Teff' (E) effective temperature, in Kelvin. col6='Lum' (E) Luminosity in solar luminosities. col7='logg' (E) surface gravity, in log_10(cm/s2). col8,9,10='diamK xxxm' (E) biased angular diameters measured by an interferometer at baselines xxx (in m), for xxx=[100, 200, 300]. In milliarcseconds col>=11= 'MAG ...' or 'COLOR ...' (E) reddenned magnitudes or colors in various bands, depending on the data entry. '...' is the name of band for magnitudes, and pair of bands for colors. (6 data files).

Published
2015

41. Progress of the CHARA/SPICA project

Author

Tuthill, Peter G., Mérand, Antoine, Sallum, Stephanie, Pannetier, C., Mourard, D., Berio, P., Cassaing, F., Allouche, F., Anugu, N., Bailet, C., ten Brummelaar, T., Dejonghe, J., Gies, D., Jocou, L., Kraus, S., Lacour, S., Lagarde, S., Le Bouquin, J. B., Lecron, D., Monnier, J., Nardetto, N., Patru, F., Perraut, K., Petrov, R., Rousseau, S., Stee, P., Sturmann, J., and Sturmann, L.

Published
2020
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42. An update on the CHARA array

Author

ten Brummelaar, T, Gies, D G, McAlister, H, Ridgway, S T, Sturmann, J, Sturmann, Laszlo, Schaefer, G H, Turner, N H, Farrington, C, Scott, N J, Ireland, Michael, ten Brummelaar, T, Gies, D G, McAlister, H, Ridgway, S T, Sturmann, J, Sturmann, Laszlo, Schaefer, G H, Turner, N H, Farrington, C, Scott, N J, and Ireland, Michael

Abstract

The CHARA Array, operated by Georgia State University, is located at Mount Wilson Observatory just north of Los Angeles in California. The CHARA consortium includes many groups, including LIESA in Paris, Observatoire de la Cote d’Azur, the University of Michigan, Sydney University, the Australian National University, the NASA Exoplanet Science Institute, and most recently the University of Exeter. The CHARA Array is a six-element optical/NIR interferometer, and for the time being at least, has the largest operational baselines in the world. In this paper we will give a brief introduction to the array infrastructure with a focus on our Adaptive Optics program, and then discuss current funding as well as opportunities of funding in the near future.

Published
2016

43. No Sun-like dynamo on the active star zeta Andromedae from starspot asymmetry

Author

Roettenbacher, R. M., Monnier, J. D., Korhonen, H., Aarnio, A. N., Baron, F., Che, X., Harmon, R. O., Kovari, Zs., Kraus, S., Schaefer, G. H., Torres, G., Zhao, M., ten Brummelaar, T. A., Sturmann, J., Sturmann, L., Roettenbacher, R. M., Monnier, J. D., Korhonen, H., Aarnio, A. N., Baron, F., Che, X., Harmon, R. O., Kovari, Zs., Kraus, S., Schaefer, G. H., Torres, G., Zhao, M., ten Brummelaar, T. A., Sturmann, J., and Sturmann, L.

Published
2016

44. A disk wind in AB Aurigae traced with Hαinterferometry

Author

Perraut, K., primary, Dougados, C., additional, Lima, G. H. R. A., additional, Benisty, M., additional, Mourard, D., additional, Ligi, R., additional, Nardetto, N., additional, Tallon-Bosc, I., additional, ten Brummelaar, T., additional, and Farrington, C., additional

Published
2016
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46. An update on the CHARA array

Author

ten Brummelaar, T. A., additional, Gies, D. G., additional, McAlister, H. A., additional, Ridgway, S. T., additional, Sturmann, J., additional, Sturmann, L., additional, Schaefer, G. H., additional, Turner, N. H., additional, Farrington, C. D., additional, Scott, N. J., additional, Monnier, J. D., additional, and Ireland, M. J., additional

Published
2016
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48. Multiplicity of Galactic Cepheids from long-baseline interferometry – III. Sub-percent limits on the relative brightness of a close companion of δ Cephei

Author

Gallenne, A., primary, Mérand, A., additional, Kervella, P., additional, Monnier, J. D., additional, Schaefer, G. H., additional, Roettenbacher, R. M., additional, Gieren, W., additional, Pietrzyński, G., additional, McAlister, H., additional, ten Brummelaar, T., additional, Sturmann, J., additional, Sturmann, L., additional, Turner, N., additional, and Anderson, R. I., additional

Published
2016
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50. Stellar diameters and temperatures - VI. High angular resolution measurements of the transiting exoplanet host stars HD 189733 and HD 209458 and implications for models of cool dwarfs

Author

Boyajian, T., von Braun, K., Feiden, Gregory, Huber, D., Basu, S., Demarque, P., Fischer, D. A., Schaefer, G., Mann, A. W., White, T. R., Maestro, V., Brewer, J., Lamell, C. B., Spada, F., López-Morales, M., Ireland, M., Farrington, C., van Belle, G. T., Kane, S. R., Jones, J., ten Brummelaar, T. A., Ciardi, D. R., McAlister, H. A., Ridgway, S., Goldfinger, P. J., Turner, N. H., Sturmann, L., Boyajian, T., von Braun, K., Feiden, Gregory, Huber, D., Basu, S., Demarque, P., Fischer, D. A., Schaefer, G., Mann, A. W., White, T. R., Maestro, V., Brewer, J., Lamell, C. B., Spada, F., López-Morales, M., Ireland, M., Farrington, C., van Belle, G. T., Kane, S. R., Jones, J., ten Brummelaar, T. A., Ciardi, D. R., McAlister, H. A., Ridgway, S., Goldfinger, P. J., Turner, N. H., and Sturmann, L.

Abstract

We present direct radii measurements of the well-known transiting exoplanet host stars HD 189733 and HD 209458 using the CHARA Array interferometer. We find the limb-darkened angular diameters to be thetaLD = 0.3848 +/- 0.0055 and 0.2254 +/- 0.0072 milliarcsec for HD 189733 and HD 209458, respectively. HD 189733 and HD 209458 are currently the only two transiting exoplanet systems where detection of the respective planetary companion's orbital motion from high resolution spectroscopy has revealed absolute masses for both star and planet. We use our new measurements together with the orbital information from radial velocity and photometric time series data, Hipparcos distances, and newly measured bolometric fluxes to determine the stellar effective temperatures (Teff = 4875 +/- 43, 6093 +/- 103 K), stellar linear radii (R* = 0.805 +/- 0.016, 1.203 +/- 0.061 Rsun), mean stellar densities (rho* = 1.62 +/- 0.11, 0.58 +/- 0.14 rhosun), planetary radii (Rp = 1.216 +/- 0.024, 1.451 +/- 0.074 RJup), and mean planetary densities (rhop = 0.605 +/- 0.029, 0.196 +/- 0.033 rhoJup) for HD 189733 b and HD 209458 b, respectively. The stellar parameters for HD 209458, a F9 dwarf, are consistent with indirect estimates derived from spectroscopic and evolutionary modeling. However, we find that models are unable to reproduce the observational results for the K2 dwarf, HD 189733. We show that, for stellar evolutionary models to match the observed stellar properties of HD 189733, adjustments lowering the solar-calibrated mixing length parameter from 1.83 to 1.34 need to be employed.

Published
2015
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