2006 interferometry imaging beauty contest

Lawson, Peter R.; Cotton, W. D.; Hummel, Christian A.; Baron, Fabien; Young, John S.; Kraus, Stefan; Hofmann, Karl H.; Weigelt, G.; Ireland, Michael; Monnier, John D.; Thiébaut, Éric; Sridharan, R.; Chesneau, O.

doi:10.1117/12.670409

Cited by 27 publications

(21 citation statements)

References 3 publications

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“…Goodman 2005). The proceedings of recent summer schools on optical interferometry are also very instructive in considering these instruments further (in particular, Lawson 2000;Haniff 2007aHaniff , 2007b, as is Bracewell (2000)'s book on the Fourier transform itself. In practice, an optical interferometer takes light from two or more telescopes and recombines in such a way that the light from the apertures combines coherently, or interferes with itself (hence the name).…”

Section: Observational Quantities Predictionsmentioning

confidence: 99%

“…3 of Zhao et al (2009), who use the Maximum Entropy Method of radio synthesis imaging (Narayan and Nityananda 1986) as developed by Ireland et al (2006) into the "Markov-Chain Imager for Optical Interferometry" (MACIM) code. Blind tests of the results from MACIM (Lawson et al 2006) have shown it to be a robust tool for image reconstruction with optical interferometric data. For the application to rapid rotators, Zhao et al (2009) incorporated an ellipse prior, justified by the reasonable expectation that the stellar photosphere has a sharp cutoff at the edge.…”

Section: Image Reconstructionmentioning

confidence: 99%

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Interferometric observations of rapidly rotating stars

Belle

2012

Astron Astrophys Rev

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Optical interferometry provides us with a unique opportunity to improve our understanding of stellar structure and evolution. Through direct observation of rotationally distorted photospheres at sub-milliarcsecond scales, we are now able to characterize latitude dependencies of stellar radius, temperature structure, and even energy transport. These detailed new views of stars are leading to revised thinking in a broad array of associated topics, such as spectroscopy, stellar evolution, and exoplanet detection. As newly advanced techniques and instrumentation mature, this topic in astronomy is poised to greatly expand in depth and influence.

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Section: Observational Quantities Predictionsmentioning

confidence: 99%

Section: Image Reconstructionmentioning

confidence: 99%

Interferometric observations of rapidly rotating stars

Belle

2012

Astron Astrophys Rev

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“…All these algorithms have been compared on simulated data during Interferometric Beauty Contests [16], [60], [61]. The results of the contest were very encouraging.…”

Section: B Image Reconstruction Algorithmsmentioning

confidence: 99%

Image reconstruction in optical interferometry

Thiébaut¹,

Giovannelli

2010

IEEE Signal Process. Mag.

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Abstract-This tutorial paper describes the problem of image reconstruction from interferometric data with a particular focus on the specific problems encountered at optical (visible/IR) wavelengths. The challenging issues in image reconstruction from interferometric data are introduced in the general framework of inverse problem approach. This framework is then used to describe existing image reconstruction algorithms in radio interferometry and the new methods specifically developed for optical interferometry.

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“…For this purpose, we employed the Building Block Mapping (BBM) image reconstruction algorithm 18 . This algorithm has already been employed successfully in various earlier projects to reconstruct interferometric images from simulated 19,20 and long-baseline interferometric data [21][22][23] . The reconstruction was performed on a 256 × 256 grid using a pixel scale of 0.85 mas/pixel and convergence was reached after ∼ 12 000 iteration steps.…”

Section: Aperture Synthesis Imagingmentioning

confidence: 99%

First results from VLTI near-infrared interferometry on high-mass young stellar objects

et al. 2010

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Due to the recent dramatic technological advances, infrared interferometry can now be applied to new classes of objects, resulting in exciting new science prospects, for instance, in the area of high-mass star formation. Although extensively studied at various wavelengths, the process through which massive stars form is still only poorly understood. For instance, it has been proposed that massive stars might form like low-mass stars by mass accretion through a circumstellar disk/envelope, or otherwise by coalescence in a dense stellar cluster. Therefore, clear observational evidence, such as the detection of disks around high-mass young stellar objects (YSOs), is urgently needed in order to unambiguously identify the formation mode of the most massive stars.After discussing the technological challenges which result from the special properties of these objects, we present first near-infrared interferometric observations, which we obtained on the massive YSO IRAS 13481-6124 using VLTI/AMBER infrared long-baseline interferometry and NTT speckle interferometry. From our extensive data set, we reconstruct a model-independent aperture synthesis image which shows an elongated structure with a size of ∼ 13 × 19 AU, consistent with a disk seen under an inclination of ∼ 45• . The measured wavelengthdependent visibilities and closure phases allow us to derive the radial disk temperature gradient and to detect a dust-free region inside of 9.5 AU from the star, revealing qualitative and quantitative similarities with the disks observed in low-mass star formation. In complementary mid-infrared Spitzer and sub-millimeter APEX imaging observations we detect two bow shocks and a molecular outflow, which are oriented perpendicular to the disk plane and indicate the presence of a bipolar outflow emanating from the inner regions of the system.

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2006 interferometry imaging beauty contest

Cited by 27 publications

References 3 publications

Interferometric observations of rapidly rotating stars

Interferometric observations of rapidly rotating stars

Image reconstruction in optical interferometry

First results from VLTI near-infrared interferometry on high-mass young stellar objects

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