The very large telescope Interferometer: 2010 edition

Haguenauer, Pierre; Alonso, Jaime; Bourget, P.; Brillant, S.; Gitton, Philippe B.; Guisard, Stéphane; Poupar, Sébastien; Schuhler, Nicolas; Abuter, R.; Andolfato, Luigi; Blanchard, Guillaume; Berger, J.‐P.; Cortes, Angela; Dérie, F.; Delplancke, F.; Lieto, Nicola Di; Dupuy, Christophe; Gilli, Bruno; Glindemann, Andreas; Guniat, Serge; Huedepohl, Gerhard; Kaufer, A.; Bouquin, Jean-Baptiste Le; Lévêque, S.; Ménardi, Serge; Mérand, A.; Morel, S.; Percheron, Isabelle; Duc, Than Phan; Pino, Andrés del; Ramírez, Andrés; Sridharan, R.; Richichi, A.; Rivinius, Thomas; Schoeller, Markus; Schmid, Christian; Štefl, S.; Valdes, G.; Belle, Gerard van; Wehner, Stefan; Wittkowski, M.

doi:10.1117/12.857070

Cited by 11 publications

(4 citation statements)

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“…VLTI (Haguenauer et al 2010) PIONIER (Bouquin et al 2011) observations were undertaken in service mode during ESO periods 99, 101, and102 (2017-2019), using the four 1.8 m Auxiliary Telescopes on the two largest configurations: A0-G1-J2-J3 and A0-G1-J2-K0 (58-132 m and 49-129 m baselines respectively). The service mode observations had the constraint of clear skies and better than 1.2 arcsec seeing.…”

Section: Interferometric Observationsmentioning

confidence: 99%

Precision angular diameters for 16 southern stars with VLTI/PIONIER

Rains

Ireland

White

et al. 2020

Monthly Notices of the Royal Astronomical Society

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In the current era of Gaia and large, high signal to noise stellar spectroscopic surveys, there is an unmet need for a reliable library of fundamentally calibrated stellar effective temperatures based on accurate stellar diameters. Here we present a set of precision diameters and temperatures for a sample of 6 dwarf, 5 sub-giant, and 5 giant stars observed with the PIONIER beam combiner at the VLTI. Science targets were observed in at least two sequences with five unique calibration stars each for accurate visibility calibration and to reduce the impact of bad calibrators. We use the standard PIONIER data reduction pipeline, but bootstrap over interferograms, in addition to employing a Monte-Carlo approach to account for correlated errors by sampling stellar parameters, limb darkening coefficients, and fluxes, as well as predicted calibrator angular diameters. The resulting diameters were then combined with bolometric fluxes derived from broadband Hipparcos-Tycho photometry and MARCS model bolometric corrections, plus parallaxes from Gaia to produce effective temperatures, physical radii, and luminosities for each star observed. Our stars have mean angular diameter and temperatures uncertainties of 0.8% and 0.9% respectively, with our sample including diameters for 10 stars with no pre-existing interferometric measurements. The remaining stars are consistent with previous measurements, with the exception of a single star which we observe here with PIONIER at both higher resolution and greater sensitivity than was achieved in earlier work.

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Section: Interferometric Observationsmentioning

confidence: 99%

Precision angular diameters for 16 southern stars with VLTI/PIONIER

Rains

Ireland

White

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…We list observational characteristics of sgB[e] with an emphasis on the results obtained in the last 8 years, since the meeting dedicated to the B[e] phenomenon [37]. A particular emphasis is given to results with optical interferometers like the VLTI [38] and CHARA [39]. Our aim is to remain strictly with supergiants and avoid other evolutionary phases that show the B[e] phenomenon.…”

Section: Recent Advances In Observed Properties Of Sgb[e] Starsmentioning

confidence: 99%

Dusty Blue Supergiants: News from High-Angular Resolution Observations

Wit

Oudmaijer

2014

Advances in Astronomy

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An overview is presented of the recent advances in understanding the B[e] phenomenon among blue supergiant stars in light of high-angular resolution observations and with an emphasis on the results obtained by means of long baseline optical stellar interferometry. The focus of the review is on the circumstellar material and evolutionary phase of B[e] supergiants, but recent results on dust production in regular blue supergiants are also highlighted.

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“…For beam monitoring, plastic fibres are appropriate only for low currents due to their very low resistance to heat. In hadrontherapy, an array of plastic scintillating fibres read out by a CCD has been recently developed for the Italian National Centre for Hadrontherapy CNAO [11]. For high currents, Ce 3+ doped quartz surfaces have been used [12] [13] and resistance up to temperatures of 1300°C has been reported.…”

Section: Rationale For a Beam Monitor Detector Based On Doped Silica mentioning

confidence: 99%

A beam monitor detector based on doped silica and optical fibres

Braccini¹,

Ereditato²,

Giacoppo³

et al. 2012

J. Inst.

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A beam monitor detector prototype based on doped silica fibres coupled to optical fibres has been designed, constructed and tested, mainly for accelerators used in medical applications. Scintillation light produced by Ce and Sb doped silica fibres moving across the beam has been measured, giving information on beam position, shape and intensity. Mostly based on commercial components, the detector is easy to install, to operate and no electronic components are located near the beam. Tests have been performed with a 2 MeV proton pulsed beam at an average current of 0.8 µA. The response characteristics of Sb doped silica fibres have been studied for the first time.

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The very large telescope Interferometer: 2010 edition

Cited by 11 publications

References 0 publications

Precision angular diameters for 16 southern stars with VLTI/PIONIER

Precision angular diameters for 16 southern stars with VLTI/PIONIER

Dusty Blue Supergiants: News from High-Angular Resolution Observations

A beam monitor detector based on doped silica and optical fibres

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