Near-infrared IOTA interferometry of the symbiotic star CH Cyg

Hofmann, K.-H.; Beckmann, U.; Berger, J.‐P.; Bloêcker, T.; Brewer, Michael K.; Lacasse, M. G.; Malanushenko, V. P.; Millan-Gabet, R.; Monnier, John D.; Ohnaka, K.; Pedretti, E.; Schertl, D.; Schloerb, F. Peter; Scholz, M.; Traub, Wesley A.; Weigelt, G.; Yudin, B. F.

doi:10.1117/12.458904

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“…Table 2 shows the parameters that were obtained from the fit. The value of 8.6±0.2 mas, for the diameter of the red giant, agrees well within errors with the value obtained with infrared interferometry by Hofmann et al 36 The errors were derived using bootstrap statistics on the data set. A marginally improved χ 2 was obtained by fitting an elliptical dust distribution around the star.…”

Section: The Elusive Symbiotic Star Ch Cygsupporting

confidence: 90%

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Last technology and results from the IOTA interferometer

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Section: The Elusive Symbiotic Star Ch Cygsupporting

confidence: 90%

“…The star V Hya increased its angular diameter from 11. 36 The size of the dust was found to be 17.1±0.2 mas or 2.0±0.1 stellar radii.…”

Section: Discussionmentioning

confidence: 89%

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“…G. Weigelt and collaborators have developed a spectrometer for use on two element interferometers, which allows near-infrared molecular bandheads of CO and H 2 O to be spatially probed (e.g. Weigelt et al, 2000;Hofmann, 2002). More interestingly, the AMBER instrument for the VLTI will boast three different spectral resolutions (up to R ∼10000 across the infrared), making observations of individual lines possible (e.g., Petrov et al, 2000).…”

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confidence: 99%

Optical interferometry in astronomy

2003

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Abstract. Here I review the current state of the field of optical stellar interferometry, concentrating on ground-based work although a brief report of space interferometry missions is included. We pause both to reflect on decades of immense progress in the field as well as to prepare for a new generation of large interferometers just now being commissioned (most notably, the CHARA, Keck and VLT Interferometers). First, this review summarizes the basic principles behind stellar interferometry needed by the lay-physicist and general astronomer to understand the scientific potential as well as technical challenges of interferometry. Next, the basic design principles of practical interferometers are discussed, using the experience of past and existing facilities to illustrate important points. Here there is significant discussion of current trends in the field, including the new facilities under construction and advanced technologies being debuted. This decade has seen the influence of stellar interferometry extend beyond classical regimes of stellar diameters and binary orbits to new areas such as mapping the accretion disks around young stars, novel calibration of the Cepheid Period-Luminosity relation, and imaging of stellar surfaces. The third section is devoted to the major scientific results from interferometry, grouped into natural categories reflecting these current developments. Lastly, I consider the future of interferometry, highlighting the kinds of new science promised by the interferometers coming on-line in the next few years. I also discuss the longer-term future of optical interferometry, including the prospects for space interferometry and the possibilities of large-scale ground-based projects. Critical technological developments are still needed to make these projects attractive and affordable. †

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Detection of non-radial pulsation and faint companion in the symbiotic star CH Cyg

Pedretti¹,

Monnier²,

Lacour³

et al. 2009

Monthly Notices of the Royal Astronomical Society

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International audienceWe have detected asymmetry in the symbiotic star CH Cyg through the measurement of precision closure phase with the Integrated Optics Near-Infrared Camera (IONIC) beam combiner, at the infrared optical telescope array interferometer. The position of the asymmetry changes with time and is correlated with the phase of the 2.1-year period found in the radial velocity measurements for this star. We can model the time-dependent asymmetry either as the orbit of a low-mass companion around the M giant or as an asymmetric, 20 per cent change in brightness across the M giant. We do not detect a change in the size of the star during a 3-year monitoring period neither with respect to time nor with respect to wavelength. We find a spherical dust shell with an emission size of 2.2 +/- 0.1 D* full width at half-maximum around the M giant star. The star to dust flux ratio is estimated to be 11.63 +/- 0.3. While the most likely explanation for the 20 per cent change in brightness is non-radial pulsation, we argue that a low-mass companion in close orbit could be the physical cause of the pulsation. The combined effect of pulsation and low-mass companion could explain the behaviour revealed by the radial velocity curves and the time-dependent asymmetry detected in the closure-phase data. If CH Cyg is a typical long secondary period variable then these variations could be explained by the effect of an orbiting low-mass companion on the primary star

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Near-infrared IOTA interferometry of the symbiotic star CH Cyg

Cited by 3 publications

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Last technology and results from the IOTA interferometer

Last technology and results from the IOTA interferometer

Optical interferometry in astronomy

Detection of non-radial pulsation and faint companion in the symbiotic star CH Cyg

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