First Results from the CHARA Array. II. A Description of the Instrument

By T. T. ten Brummelaar, H. Mcalister, S. Ridgway, W. Bagnuolo, N. Turner, L. Sturmann, J. Sturmann, D. Berger, C. Ogden, R. Cadman and 3 more. 2005

487 citations recorded by the source corpus.

The CHARA Array is a six 1 m telescope optical/IR interferometric array located on Mount Wilson, California, designed and built by the Center for High Angular Resolution Astronomy of Georgia State University. In this paper we describe the main elements of the Array hardware and software control systems, as well as the data reduction methods currently being used. Our plans for upgrades in the near future are also described.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/18dc5beaef6015bc7d55e77a215a24cceea43954

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In Astronomy and Astrophysics

1. D. Huber
2. D. Stello
3. W. Chaplin
4. T. Bedding
5. E. Gaidos
6. D. Charbonneau
7. A. Tokovinin
8. A. Miglio

In Atomic and Molecular Physics, and Optics

1. B. Mason
2. W. Hartkopf
3. Michael J. Ireland
4. A. Miglio
5. D. Stello
6. H. Kjeldsen
7. T. Bedding
8. T. White

In Instrumentation

1. D. Huber
2. D. Stello
3. W. Chaplin
4. T. Bedding
5. A. Tokovinin
6. S. Hekker
7. A. Miglio
8. Luca Casagrande

Citations in the corpus

• STELLAR DIAMETERS AND TEMPERATURES. II. MAIN-SEQUENCE K- AND M-STARS (2012, methodology): “We acquired interferometric observations at the CHARA Array with the Classic beam combiner in single-baseline mode in the near-infrared K ′ and H bands (ten Brummelaar et al. 2005) for 21 K- and M-type dwarfs (Table 1).”
• STELLAR DIAMETERS AND TEMPERATURES. III. MAIN-SEQUENCE A, F, G, AND K STARS: ADDITIONAL HIGH-PRECISION MEASUREMENTS AND EMPIRICAL RELATIONS (2013, methodology): “Observations with the CHARA Array Akin to the observing outlined in DT1 and DT2, observations for this project were made with the CHARA Array, a long-baseline optical/infrared interferometer located on Mount Wilson Observatory in southern California (see ten Brummelaar et al. 2005 for details).”
• FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY (2012, methodology): “At the same time, the development of highly sensitive instruments such as the PAVO beam combiner (Ireland et al. 2008) at the CHARA Array (ten Brummelaar et al. 2005) have pushed the sensitivity limits of long-baseline interferometry, bringing into reach the brightest objects for which high-quality…”
• PREDICTING THE α COMAE BERENICES TIME OF ECLIPSE: HOW 3 AMBIGUOUS MEASUREMENTS OUT OF 609 CAUSED A 26 YEAR BINARY’S ECLIPSE TO BE MISSED (2015, unknown): “Finally, a measurement of the binary separation by the CHARA Array ( Center for High Angular Resolution Astron-omy, ten Brummelaar et al. 2005 ) was made on 2015 January 16 as a separated fringe packet binary using the CLIMB beam combiner.”
• Circumstellar material in the Vega inner system revealed by CHARA/FLUOR (2006, methodology): “In order to better constrain the near-infrared brightness of Vega’s disk, we have used the same method at the CHARA Array (ten Brummelaar et al. 2005) with an optimised set of baselines.”
• First Resolved Images of the Eclipsing and Interacting Binary β Lyrae (2008, background): “The CHARA array, located on Mt. Wilson and consisting of six 1-meter telescopes, is the longest optical/IR interferometer array in the world (ten Brummelaar et al. 2005).”
• A SURVEY OF STELLAR FAMILIES: MULTIPLICITY OF SOLAR-TYPE STARS (2009, methodology): “…wide for radial-velocity campaigns and too close for traditional visual techniques such as speckle interferometry was conducted through a systematic survey for separated fringe packet (SFP) binaries using the Center for High Angular Resolution Astronomy (CHARA) Array (ten Brummelaar et al. 2005).”
• Multiplicity of Galactic Cepheids from long-baseline interferometry – III. Sub-percent limits on the relative brightness of a close companion of δ Cephei (2016, methodology): “The observations were performed in July and October 2015 using the Michigan InfraRed Combiner (MIRC) installed at the CHARA array (ten Brummelaar et al. 2005), located on Mount Wilson, California.”
• STELLAR DIAMETERS AND TEMPERATURES. I. MAIN-SEQUENCE A, F, AND G STARS (2011, background): “Instrument The CHARA Array is an optical/infrared interferometric array located at Mount Wil- son Observatory in the San Gabriel mountains of southern California (a detailed description of the instrument can be found in ten Brummelaar et al. 2005).”
• First Results from the CHARA Array. VII. Long-Baseline Interferometric Measurements of Vega Consistent with a Pole-On, Rapidly Rotating Star (2006, methodology): “We have employed the long baselines of the CHARA Array (ten Brummelaar et al. 2005) on Mount Wilson, together with the capabilties of the spatially-filtered Fiber Linked Unit for Optical Recombination (FLUOR, Coudé du Foresto et al. 2003), as a means to probe the second lobe of Vega’s visibility…”
• An investigation of the close environment of β Cephei with the VEGA/CHARA interferometer (2010, background): “…Center for High Angular Resolution Astronomy (CHARA) of Georgia State University operates an optical interferometric array located at Mount Wilson 1 http://ad.usno.navy.mil/wds/ 2 http://ad.usno.navy.mil/wds/int4.html 3 http://ad.usno.navy.mil/wds/orb6.html Observatory (ten Brummelaar et al. 2005).”
• A CHARA ARRAY SURVEY OF CIRCUMSTELLAR DISKS AROUND NEARBY Be-TYPE STARS (2013, methodology): “The observations were conducted between 2007 October and 2010 November using the CHARA Classic beam combiner operating in theK-band (effective wavelength = 2.1329 µm; ten Brummelaar et al. 2005).”
• VEGA: Visible spEctroGraph and polArimeter for the CHARA array: principle and performance (2009, methodology): “The distribution of length and orientation of these baselines, as given in Table 1 of ten Brummelaar et al. (2005), allows a good coverage of the spatial frequency plane and permits the instrument to reach very high angular resolution.”
• Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, methodology): “…the subgiant HD 140283, and the giant HD 220009 were measured in the near-infrared with the CHARA Array at Mount Wilson Observatory (California, ten Brummelaar et al. 2005) and either the PAVO or the VEGA instruments by Bazot et al. (2011, PAVO), Bigot et al. (2011, VEGA), Creevey et al. (2015,…”
• A Guide to Realistic Uncertainties on the Fundamental Properties of Solar-type Exoplanet Host Stars (2020, methodology): “Panel (a): Ratio of interferometric angular diameters from the CHARA Array for stars with multiple published measurements as a function of diameter.”
• SEPARATED FRINGE PACKET OBSERVATIONS WITH THE CHARA ARRAY. II. ω ANDROMEDA, HD 178911, AND ξ CEPHEI (2014, methodology): “Before 2009, observations for the SFP program were taken as described in Paper I with the CHARA Classic two-beam combiner as described by (ten Brummelaar et al. 2005).”