The VLTI -- A Status Report

Glindemann, Andreas; Algomedo, J.; Amestica, Rodrigo; Ballester, P.; Bauvir, Bertrand; Bugueño, E.; Correia, Serge; Delgado, Francisco; Delplancke, F.; Dérie, F.; Duhoux, Philippe; Folco, E. Di; Gennai, A.; Gilli, Bruno; Giordano, P.; Gitton, Philippe B.; Guisard, Stéphane; Housen, Nico; Huxley, Alexis; Kervella, P.; Kiekebusch, M.; Koehler, Bertrand; Lévêque, S.; Longinotti, Antonio; Morel, S.; Paresce, Francesco; Duc, Than Phan; Richichi, A.; Schoeller, Markus; Tarenghi, M.; Wallander, Anders; Wittkowski, M.; Wilhelm, Rainer; Ménardi, Serge

doi:10.1117/12.458117

Cited by 42 publications

(28 citation statements)

References 2 publications

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“…Recently, the Very Large Telescope Interferometer (VLTI, Glindemann et al 2003) of ESO's Paranal Observatory has been equipped with MIDI, the MID-infrared Interferometric instrument (Leinert et al 2003). MIDI combines the light of two telescopes and provides spectrally resolved visibilities in the 10 µm atmospheric window.…”

Section: Introductionmentioning

confidence: 99%

Mid-infrared sizes of circumstellar disks around Herbig Ae/Be stars measured with MIDI on the VLTI

Leinert¹,

Boekel²,

Waters

et al. 2004

A&A

177

179

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Abstract. We present the first long baseline mid-infrared interferometric observations of the circumstellar disks surrounding Herbig Ae/Be stars. The observations were obtained using the mid-infrared interferometric instrument MIDI at the European Southern Observatory (ESO) Very Large Telescope Interferometer VLTI on Cerro Paranal. The 102 m baseline given by the telescopes UT1 and UT3 was employed, which provides a maximum full spatial resolution of 20 milli-arcsec (mas) at a wavelength of 10 µm. The interferometric signal was spectrally dispersed at a resolution of 30, giving spectrally resolved visibility information from 8 µm to 13.5 µm. We observed seven nearby Herbig Ae/Be stars and resolved all objects. The warm dust disk of HD 100546 could even be resolved in single-telescope imaging. Characteristic dimensions of the emitting regions at 10 µm are found to be from 1 AU to 10 AU. The 10 µm sizes of our sample stars correlate with the slope of the 10-25 µm infrared spectrum in the sense that the reddest objects are the largest ones. Such a correlation would be consistent with a different geometry in terms of flaring or flat (self-shadowed) disks for sources with strong or moderate mid-infrared excess, respectively. We compare the observed spectrally resolved visibilities with predictions based on existing models of passive centrally irradiated hydrostatic disks made to fit the SEDs of the observed stars. We find broad qualitative agreement of the spectral shape of visibilities corresponding to these models with our observations. Quantitatively, there are discrepancies that show the need for a next step in modelling of circumstellar disks, satisfying both the spatial constraints such as are now available from the MIDI observations and the flux constraints from the SEDs in a consistent way.Key words. stars: circumstellar matter -techniques: interferometric -stars: formation -stars: pre-main-sequenceinfrared: stars Based on observations made with the Very Large Telescope Interferometer at Paranal Observatory.

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Section: Introductionmentioning

confidence: 99%

Mid-infrared sizes of circumstellar disks around Herbig Ae/Be stars measured with MIDI on the VLTI

Leinert¹,

Boekel²,

Waters

et al. 2004

A&A

177

179

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“…ESO and the European Space Agency ESA are currently studying the possibility to build GENIE, a ground demonstrator of the DARWIN nulling interferometer that will operate later in space (Fridlund et al 2003). Finally, a number of concepts for a second generation of VLTI instruments are also being considered (Glindemann et al 2003). For the immediate purpose of this paper, we will not discuss the implications of such developments, that would require a new set of calibrators.…”

Section: Vlti Overviewmentioning

confidence: 99%

“…In the last few years, the CHARA, Keck and VLTI interferometers (ten Brummelaar et al 2003;Colavita & Wizinowich 2003;Glindemann et al 2003) have started operation, while other facilities such as OHANA (Perrin et al 2004) and MRO (Creech-Eakman et al 2003) are being readied. These new large interferometers couple for the first time hectometric baselines with large telescopes, offering a wavelength coverage from the visual to the thermal infrared and aiming also at nulling interferometry.…”

Section: Introductionmentioning

confidence: 99%

First results from the ESO VLTI calibrators program

Richichi¹,

Percheron²

2005

A&A

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Abstract. The ESO Very Large Telescope Interferometer (VLTI) is one of the leading interferometric facilities. It is equipped with several 8.2 and 1.8 m telescopes, a large number of baselines up to 200 m, and with several subsystems designed to enable high quality measurements and to improve significantly the limits of sensitivities currently available to long-baseline interferometry. The full scientific potential of the VLTI can be exploited only if a consistent set of good quality calibrators is available. For this, a large number of observations of potential calibrators have been obtained during the commissioning phase of the VLTI. These data are publicly available. We briefly describe the interferometer, the VINCI instrument used for the observations, the data flow from acquisition to processed results, and we present and comment on the volume of observations gathered and scrutinized. The result is a list of 191 calibrator candidates, for which a total of 12 066 observations can be deemed of satisfactory quality. We present a general statistical analysis of this sample, using as a starting point the angular diameters previously available in the literature. We derive the general characteristics of the VLTI transfer function, and its trend with time in the period 2001 through mid-2004. A second paper will be devoted to a detailed investigation of a selected sample, aimed at establishing a VLTI-based homogeneous system of calibrators.

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“…To a great extent, the current knowledge about the inner part of protoplanetary disks has been obtained with interferometric instruments that are presently in operation: AMBER 7 (Petrov and The AMBER Consortium, 2003) and MIDI 8 (Leinert et al, 2003) on the VLTI (Glindemann et al, 2003), MIRC 9 , CLIMB 10 and VEGA 11 (Mourard 7 Astronomical Multi-beam Combiner: the near-infrared/red focal instrument of the VLTI 8 Mid-infrared interferometric instrument 9 Michigan Infrared Combiner 10 Classic Infrared Multiple Beamcombiner 11 Visible spectrograph and polarimeter (Perrin et al, 2006a). Furthermore, the PTI 14 and IOTA 15 have been used for circumstellar disk studies until recently.…”

Section: Selected Near-future Interferometric Instrumentsmentioning

confidence: 99%

Circumstellar disks and planets

Wolf

Malbet

Alexander

et al. 2012

Astron Astrophys Rev

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We present a review of the interplay between the evolution of circumstellar disks and the formation of planets, both from the perspective of theoretical models and dedicated observations. Based on this, we identify and discuss fundamental questions concerning the formation and evolution of circumstellar disks and planets which can be addressed in the near future with optical and infrared long-baseline interferometers. Furthermore, the importance of complementary observations with long-baseline (sub)millimeter interferometers and high-sensitivity infrared observatories is outlined.

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The VLTI -- A Status Report

Cited by 42 publications

References 2 publications

Mid-infrared sizes of circumstellar disks around Herbig Ae/Be stars measured with MIDI on the VLTI

Mid-infrared sizes of circumstellar disks around Herbig Ae/Be stars measured with MIDI on the VLTI

First results from the ESO VLTI calibrators program

Circumstellar disks and planets

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