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Topic: VLTI

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	Very Large Telescope - Wikipedia, the free encyclopedia
		The VLTs are equiped with a large set of instruments permitting observations to be performed from the near-UV to the mid-IR (ie a large fraction of the light wavelengths accessible from the surface of the Earth), with the full range of techniques including high-resolution spectroscopy, multi-object spectroscopy, imaging, and high-resolution imaging.
		The VLTI is intended to achieve an effective angular resolution of 0.001 arcsecond at a wavelength of 1 µm.
		With the installation of the three-telescope AMBER closure-phase instrument in 2005, the first imaging observations from the VLTI are expected soon.
	en.wikipedia.org /wiki/Very_Large_Telescope (1098 words)

	JENAM 2002 - Programme - WS VLTI
		Indeed, in a first phase, the VLTI data will be obtained in the form of visibilities which require special training for their interpretation.
		The aim of this workshop is both to train non-expert astronomers in interferometry and the VLTI, and to allow expert interferometrists to present and discuss astrophysics research done with interferometers.
		The VLTI is an horizontal facility addressing science in all areas of galactic astrophysics (outer solar system, IMF, extra-solar planets, star clusters, stellar surface structure, distance scales, star formation,...) and some areas of extragalactic astrophysics (AGNs and associated jets, dust tori, line regions,...).
	www.sp-astronomia.pt /jenam2002/ws-vlti (496 words)

	10µm interferometry on the VLTI with the MIDI instrument:a preview
		From the left, the afocal beams from two telescopes of the VLTI are approaching the instrument.
		Their nominal diameter is 80 mm, and they are reduced to 18 mm by a beam compressor provided as part of the VLTI infrastructure, represented here for simplicity by two lenses.
		Apart from the spatial resolution given by the geometry of the VLTI array, it strongly depends on the sensitivity of the instrument and on the accuracy of visibility calibration.
	www.mpia-hd.mpg.de /MIDI/midi_overview/MIDIoverview.htm (3733 words)

	VLTI first fringes with two auxiliary telescopes at Paranal
		This will enable the VLTI to operate with enormous flexibility and, in particular, to obtain extremely detailed (sharp) images of celestial objects - ultimately with a resolution that corresponds to detecting an astronaut on the Moon.
		The VLT Interferometer (VLTI) combines starlight captured by two 8.2- VLT Unit Telescopes, dramatically increasing the spatial resolution and showing fine details of a large variety of celestial objects.
		Thus, in order to exploit the VLTI each night and to achieve the full potential of this unique setup, some other (smaller), dedicated telescopes were included into the overall VLT concept.
	www.eurekalert.org /pub_releases/2005-03/eso-vff031005.php (1309 words)

	First results from the ESO VLTI calibrators program
		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.
		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.
		We derive the general characteristics of the VLTI transfer function, and its trend with time in the period 2001 through mid-2004.
	www.edpsciences.org /articles/aa/abs/2005/18/aa2257/aa2257.html (264 words)

	ESA Science & Technology: The power of optical/IR interferometry: recent scientific results and 2nd generation VLTI ...
		A suite of powerful long baseline interferometers has come into operation recently, along with sophisticated instrumentation that is providing new levels of accuracy, spectral resolution and access to various spectral bands from the optical to the thermal infrared.
		Investigations are now enabled on a wealth of astrophysical sources with unprecedented levels of angular resolution and sensitivity, producing a considerable body of new, exciting scientific results.
		In celebrating the completion of the first phase of the VLTI development, this workshop will review and discuss new results of the VLTI and of other stellar interferometers, and will assess their impact on astronomy as a whole.
	sci.esa.int /science-e/www/object/index.cfm?fobjectid=36402 (200 words)

	Sharper and deeper views with MACAO-VLTI
		Soon the astronomers will be thus able to obtain interference fringes with the VLTI (ESO PR 23/01) of a large number of objects hitherto out of reach with this powerful observing technique, e.g.
		The VLTI measures the degree of coherence of the combined beams as expressed by the contrast of the observed interferometric fringe pattern.
		The higher the degree of coherence between the individual beams, the stronger is the measured signal.
	www.eurekalert.org /pub_releases/2003-05/eso-sad051303.php (1850 words)

	AMBER Project [v.2.1]
		The VLTI is an interferometer made of 4 unit 8-m telescopes and 3 auxiliary 1.8-m telescopes.
		This interferometer will allow European astronomers to achieve the spatial resolution equivalent to the one of a 200-m telescope with a sensitivity of an 8-m telescope.
		The focus of the VLTI will be equipped with three instruments:
	www.obs-nice.fr /amber/vlti.php (99 words)

	[No title]
		We have so far made use of VLTI observations of the near- and mid-infrared stellar sizes and of concurrent VLBA observations of the SiO maser emission.
		We illustrate in general the potential of interferometric measurements to study stellar atmospheres and circumstellar envelopes, and demonstrate in particular the advantages of a coordinated multi-wavelength approach including near/mid-infrared as well as radio interferometry.
		We have used VLTI observations of the near- and mid-infrared stellar sizes and concurrent VLBA observations of the SiO maser emission.
	www.gps.caltech.edu /~mbrown/astroph.html (15393 words)

	NOVA ESO VLTI Expertise Center (NEVEC)
		NEVEC (the NOVA-ESO Expertise Center for VLTI) is a joint venture between NOVA (Netherlands Research School for Astronomy) and ESO (European Southern Observatory).
		Current activities of NEVEC concentrate of developing software for the first scientific VLTI instrument MIDI, the VLTI calibration program, algorithm development and scientific exploitation of VLTI data, and operational analysis for MIDI.
		The field of optical/infrared interferometry is blooming with the commissioning of the VLTI and a number of anticipated space-based interferometric missions (e.g., DARWIN, Terrestrial Planet Finder).
	www.strw.leidenuniv.nl /~nevec/vacancies/ph_d_position_2002.html (266 words)

	Very Large Telescope : VLTI
		It is located at the Paranal Observatory[?] on Cerro Paranal[?], a 2,635-m high mountain in the Atacama desert in northern Chile.
		The VLT consists of a cluster four of large telescopes, and an interferometer (VLTI) which will be used to resolve fine features.
		The telescopes have been named after the names of some astronomical objects in the local Mapuche[?] language: Antu (The Sun), Kueyen (The Moon), Melipal (The Southern Cross), and Yepun (Venus)
	www.freearchive.info /vl/vlti.html (581 words)

	Status of VLTI control system: how to make an optical interferometer a data producing facility (SMEALSearch) - ... (Site not responding. Last check: 2007-10-19)
		Status of VLTI control system: how to make an optical interferometer a data producing facility
		Even though optical interferometry today may be considered more experimental than single telescope astronomy, we have aimed at developing a system with the same requirements on reliability and operability as for a single VLT telescope.
		The VLTI control system is responsible for controlling and coordinating all devices making up VLTI,...
	gunther.smeal.psu.edu /93323.html (277 words)

	Catalogue: J/A+A/434/1201 (Site not responding. Last check: 2007-10-19)
		J/A+A/434/1201 ESO VLTI Calibrators Program (Richichi+, 2005) ================================================================================ First results from the ESO VLTI Calibrators Program.
		It is equiped with several 8.2 and 1.8m telescopes, a large number of baselines up to 200m, and with several subsystems designed to enable high quality measurements and to improve significantly the limits of sensitivities currently available to long-baseline interferometry.
		Note (2): Number of observations (OBs) on the specified VLTI baselines, processed by the pipeline and validated according to the criteria (flags) described in the paper.
	cdsweb.u-strasbg.fr /cgi-bin/Cat?J/A+A/434/1201 (367 words)

	The Very Large Telescope Interferometer
		The Very Large Telescope Interferometer (VLTI) consists in the coherent combination of the four VLT Unit Telescopes and of the four moveable 1.8m Auxiliary Telescopes.
		Once fully operational, the VLTI will provide both a high sensitivity as well as milli-arcsec angular resolution provided by baselines of up to 200m length.
		ESO Press Release 01/04: First Auxiliary Telescope for the VLT Interferometer Installed at Paranal.
	www.eso.org /projects/vlti (269 words)

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