Principles of Stellar Interferometry

Glindemann, Andreas

doi:10.1007/978-3-642-15028-9

Cited by 53 publications

(48 citation statements)

References 181 publications

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“…It was first derived by Shao & Colavita (1992) and again in a more intuitive way by Glindemann (2011). Glindemann (2011, pg.…”

Section: Differential Fringe Motionmentioning

confidence: 95%

“…(2.7) and the Taylor hypothesis of frozen turbulence, the power spectrum of temporal differential fringe motion for fringes formed with a pair of pinhole sized apertures is given by Glindemann (2011) as, Φ dOPD,t pf q " 0.628λ wherev is the effective wind speed, r 0 is the Fried parameter, ∆s is the separation of two stars whose differential fringe motion are to be measured,h is the effective height of the atmospheric turbulent layer and B is the baseline of an interferometer used to observe the stellar fringes. The power spectrum has a unit of m 2 /Hz if the variables in the equation are in S.I.…”

Section: Appendix a Differential Fringe Motionmentioning

confidence: 99%

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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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“…It was first derived by Shao & Colavita (1992) and again in a more intuitive way by Glindemann (2011). Glindemann (2011, pg.…”

Section: Differential Fringe Motionmentioning

confidence: 95%

Section: Appendix a Differential Fringe Motionmentioning

confidence: 99%

Phase-Referenced Interferometry and Narrow-Angle Astrometry With Susi

Kok

Ireland

Tuthill

et al. 2013

J. Astron. Instrum.

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“…We note that this is not intended to be a thorough derivation of the fundamentals of interferometry, but should provide a sound basis for the understanding of observations presented in further sections, and act as a first step for the discovery of more in depth reviews and textbooks (e.g. Glindemann 2011;Taylor et al 1999;Thompson et al 2008). We also note that we do not discuss aspects of short wavelength (i.e.…”

Section: Basics Of Interferometrymentioning

confidence: 99%

Interferometry and the study of protoplanetary disks

Ilee

Greaves

2015

EPJ Web of Conferences

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Abstract. Interferometry offers access to scales that are unresolvable using single dish telescopes, which is especially important when investigating objects with small angular sizes, such as protoplanetary disks. This Chapter introduces the concept of interferometry, and describes the basic aspects of interferometric observations when considering long (i.e. sub-millimetre to radio) wavelength observations. Examples of recent work using both continuum and spectral line observations are investigated, and their diagnostic power is examined. Finally, a selection of currently available facilities are=ussed, and the prospects of future instruments are explored.

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“…The analytical expression for the diffraction of the star light at the lunar limb is given by Fresnel diffraction when the Moon is regarded as an infinite straight edge the light wave on the surface of the Earth can be written as (Glindemann 2011)…”

Section: Occultation Light Curves and Limb Irregularitiesmentioning

confidence: 99%

Advances in the interpretation and analysis of lunar occultation light curves

Richichi

Glindemann

2012

A&A

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Context. The introduction of fast 2D detectors and the use of very large telescopes have significantly advanced the sensitivity and accuracy of the lunar occultation technique. Recent routine observations at the ESO Very Large Telescope have yielded hundreds of events with results, especially in the area of binary stars, which are often beyond the capabilities of any other techniques. Aims. With the increase in the quality and in the number of the events, subtle features in the light curve patterns have occasionally been detected which challenge the standard analytical definition of the lunar occultation phenomenon as diffraction from an infinite straight edge. We investigate the possible causes for the observed peculiarities. Methods. We have evaluated the available statistics of distortions in occultation light curves observed at the ESO VLT, and compared it to data from other facilities. We have developed an alternative approach to model and interpret lunar occultation light curves, based on 2D diffraction integrals describing the light curves in the presence of an arbitrary lunar limb profile. We distinguish between large limb irregularities requiring the Fresnel diffraction formalism, and small irregularities described by Fraunhofer diffraction. We have used this to generate light curves representative of several limb geometries, and attempted to relate them to some of the peculiar data observed. Results. We conclude that the majority of the observed peculiarities is due to limb irregularities, which can give origin both to anomalies in the amplitude of the diffraction fringes and to varying limb slopes. We investigate also other possible effects, such as detector response and atmospheric perturbations, finding them negligible. We have developed methods and procedures that for the first time allow us to analyze data affected by limb irregularities, with large ones bending the fringe pattern along the shape of the irregularity, and small ones creating fringe amplitude perturbations in comparison to the ideal fringe pattern. Conclusions. The effects of a variable limb slope can be satisfactorily corrected. More complex limb irregularities could be fitted in principle with a grid search based on the standard analytical model, however this method is time consuming and does not lead to unique solutions. The incidence of the limb perturbations is relatively small, but its significance is increased with the use of very large telescopes due both to the footprint at the lunar limb and to the increased sensitivity. In general, we recommend to observe occultations using sub-pupils. This will be a necessary requirement with the next generation of extremely large telescopes.

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Principles of Stellar Interferometry

Cited by 53 publications

References 181 publications

Phase-Referenced Interferometry and Narrow-Angle Astrometry With Susi

Phase-Referenced Interferometry and Narrow-Angle Astrometry With Susi

Interferometry and the study of protoplanetary disks

Advances in the interpretation and analysis of lunar occultation light curves

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