The Sydney University Stellar Interferometer -- I. The instrument

Davis, John; Tango, W. J.; Booth, A. J.; Brummelaar, Theo A. ten; Minard, R. A.; Owens, S. M.

doi:10.1046/j.1365-8711.1999.02269.x

Cited by 70 publications

(69 citation statements)

References 1 publication

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“…Interferometer (SUSI, New South Wales, Australia, Davis et al 1999) by North et al (2007North et al ( , 2009 The most recent diameter of Arcturus was obtained by Lacour et al (2008) in the H-band (1.5 to 1.8 µm) with the IOTA (Infrared-Optical Telescope Array) interferometer (Arizona, Traub et al 2003). The diameters of the remaining stars were measured in the K-band (2.2 µm) with either the VLT Interferometer (VLTI, VINCI instrument, Kervella et al 2003a) or the CHARA Array using the Classic or FLUOR instrument, and in two cases, data from the Palomar Testbed Interferometer (PTI, California, Colavita et al 1999) were used (for HD 122563 by Creevey et al 2012 and for η Boo by van Belle et al 2007).…”

Section: Angular Diametersmentioning

confidence: 99%

GaiaFGK benchmark stars: Effective temperatures and surface gravities

Heiter

Jofré

Gustafsson

et al. 2015

A&A

287

414

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Context. In the era of large Galactic stellar surveys, carefully calibrating and validating the data sets has become an important and integral part of the data analysis. Moreover, new generations of stellar atmosphere models and spectral line formation computations need to be subjected to benchmark tests to assess any progress in predicting stellar properties. Aims. We focus on cool stars and aim at establishing a sample of 34 Gaia FGK benchmark stars with a range of different metallicities. The goal was to determine the effective temperature and the surface gravity independently of spectroscopy and atmospheric models as far as possible. Most of the selected stars have been subjected to frequent spectroscopic investigations in the past, and almost all of them have previously been used as reference, calibration, or test objects. Methods. Fundamental determinations of T eff and log g were obtained in a systematic way from a compilation of angular diameter measurements and bolometric fluxes and from a homogeneous mass determination based on stellar evolution models. The derived parameters were compared to recent spectroscopic and photometric determinations and to gravity estimates based on seismic data. Results. Most of the adopted diameter measurements have formal uncertainties around 1%, which translate into uncertainties in effective temperature of 0.5%. The measurements of bolometric flux seem to be accurate to 5% or better, which contributes about 1% or less to the uncertainties in effective temperature. The comparisons of parameter determinations with the literature in general show good agreements with a few exceptions, most notably for the coolest stars and for metal-poor stars. Conclusions. The sample consists of 29 FGK-type stars and 5 M giants. Among the FGK stars, 21 have reliable parameters suitable for testing, validation, or calibration purposes. For four stars, future adjustments of the fundamental T eff are required, and for five stars the log g determination needs to be improved. Future extensions of the sample of Gaia FGK benchmark stars are required to fill gaps in parameter space, and we include a list of suggested candidates.

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Section: Angular Diametersmentioning

confidence: 99%

GaiaFGK benchmark stars: Effective temperatures and surface gravities

Heiter

Jofré

Gustafsson

et al. 2015

A&A

287

414

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“…However, problems have been experienced at blue wavelengths (∼440 nm) with the Sydney University Stellar Interferometer (SUSI) (Davis et al 1999a) when the program object and calibrator are separated by more than ≈ 5…”

Section: Introductionmentioning

confidence: 99%

Calibration observations of Fomalhaut with the VLTI

et al. 2005

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Abstract. An investigation of the stability of the transfer function of the European Southern Observatory's Very Large Telescope Interferometer has been carried out through observations of Fomalhaut, which was observed over a range in hour angle from 21:50-05:24 on 20 October 2002. No significant variation in the transfer function was found for the zenith angle range 5• -70• . The projected baseline varied between 139.7 m and 49.8 m during the observations and, as an integral part of the determination of the transfer function, a new accurate limb-darkened angular diameter for Fomalhaut of 2.109 ± 0.013 mas has been established. This has led to improved values for the emergent flux = (3.43 ± 0.10)×108 Wm −2 , effective temperature = 8819 ± 67 K and radius = (1.213 ± 0.011)×10 9 m (R/R ⊙ = 1.744 ± 0.016). The luminosity has been found to be (6.34 ± 0.20)×1027 W (L/L ⊙ = 16.5 ± 0.5).

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“…The Sydney University Stellar Interferometer (SUSI) is a university owned optical long baseline interferometer located near Narrabri, Australia (Davis et al, 1999). The furthest distance between two siderostats (mirrors used to collect starlight) in the SUSI array, also known as the baseline, is 160m, although it can be extended to 640m which will then make it the world's longest.…”

Section: The Susi Advantagementioning

confidence: 99%

“…SUSI is a 2-element optical long baseline interferometer (Davis et al, 1999). It has a North-South (N-S) oriented baseline which is made up of a combination of 2 (one from each arm) out of 7 usable siderostats 3 .…”

Section: Susimentioning

confidence: 99%

Phase-Referenced Interferometry and Narrow-Angle Astrometry With Susi

Kok

Ireland

Tuthill

et al. 2013

J. Astron. Instrum.

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This thesis describes the development of an astrometric facility at the Sydney University Stellar Interferometer (SUSI) with an aim to measure at high precision the relative astrometry of bright close binary stars and ultimately to detect the presence of exoplanets within those binary star systems through observations of the systems' perturbed motion. At the core of the facility is a new beam combiner that is phase-referenced to an existing primary beam combiner in the visible wavelength regime. The latter provides post-processed fringe-tracking information to the former for fringe stabilization and coherent integration of pre-recorded stellar fringes using newly developed data reduction software. Interference fringe packets of a binary star are recorded alternately; first the fringe packet of the primary, then the secondary, finally back to the primary again. The measurement of the fringe packet separation is facilitated by an air-filled differential delay line and a network of interferometer-based metrology systems. Characterizations and initial astronomical observations carried out with the dual beam combiner setup demonstrated for the first time the success of the dual-star phase-referencing technique in visible (ă1µm) wavelengths. The current astrometric precision is larger than 100µas while the long term astrometric accuracy is yet to be characterized. In a parallel development, a complementary observing method using only the primary beam combiner is also demonstrated in this thesis. Relative astrometry of binary stars up to "0.8 2 separation with this technique has been demonstrated to have precision of better than 100µas. A simple detection limit analysis based on a list of target binary stars estimates up to two exoplanet detections can be achieved with SUSI if the new astrometric facility attains precision of 10µas while the primary beam combiner operates at its designed peak performance. Finally, one new stellar companion was resolved and a preliminary astrometry for another suspected companion was estimated from the astronomical observation data collected throughout the course of this thesis.

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The Sydney University Stellar Interferometer -- I. The instrument

Cited by 70 publications

References 1 publication

GaiaFGK benchmark stars: Effective temperatures and surface gravities

GaiaFGK benchmark stars: Effective temperatures and surface gravities

Calibration observations of Fomalhaut with the VLTI

Phase-Referenced Interferometry and Narrow-Angle Astrometry With Susi

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