Released on February 21st, 2007
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|A&A special feature: First astrophysical results with AMBER/VLTI
Special feature on the first results with AMBER/VLTI
Published in Astronomy & Astrophysics, volume 464-1, March II 2007
This press release is issued as a collaboration with ESO, CNRS, MPG, INAF, and Astronomy & Astrophysics.
See table of contents
The AMBER instrument installed at the Very Large Telescope (VLT) of the European Southern Observatory (ESO) combines the light from three 8.2 meter telescopes, making the VLT the world’s largest optical telescope, with a total mirror surface larger than 150 m2 and a maximum telescope separation greater than 130 m. Two years after installation, the first astrophysical results are blossoming. They are being published this week as a special feature in Astronomy & Astrophysics.
AMBER is one of the two science instruments of the Very Large Telescope Interferometer (VLTI). It is an interferometer beam combiner for the VLT, sensitive in the near-infrared wavelength range (from 1 to 2.5 microns). The consortium team  installed AMBER at ESO’s VLT in Chile in March 2004 and, although the instrument is still in the test and commissioning process, a wealth of original results about the close environment of a variety of stars have been obtained. This week, Astronomy & Astrophysics is publishing 11 articles as a special feature on AMBER/VLTI: three of them describe the instrument; the other 8 papers reveal completely new astrophysical results about the early and late stages of stellar evolution.
The principle of the interferometric technique is to combine the light collected by two or more distant telescopes. The greater the distance between the telescopes, the sharper the observations obtained. For the VLTI, this distance can be up to 130 meters, providing observers with milli-arcsecond spatial resolution. With such high spatial resolution – 16 times higher than the resolution from a single telescope – one should be able to distinguish details on the Moon that are about 2 meters in size. In addition to this high spatial resolution, AMBER also provides astronomers with a spectral resolution up to 10000, corresponding to a velocity of 30 km/s.
The first results presented in this issue cover various fields of stellar and circumstellar physics. Two papers deal with Herbig Ae/Be stars, a class of pre-main sequence stars with masses ranging from 2 to 5 solar masses and with ages younger than 10 Myr. These articles present observations of the stellar system MWC 297 (see Fig. 1) and the lower-mass, less active system HD 104237. They offer new information about the geometry of the surrounding disks and of the associated outflowing winds. These results illustrate that AMBER is a major tool for understanding both the very close environment of young stars and their circumstellar gas and dust disks, where planet formation takes place.
Three articles are devoted to hot, active stars of particular interest: a Arae, which is one of the closest Be stars ; k Canis Majoris, one of the brightest ones; and CPD -57°2874, a hot star with a peculiar emission-line spectrum. They provide new, precise information about their rotating gas envelopes.
Fig. 1 - A new picture of this system from AMBER observations of the young stellar object MWC 297. MWC 297 is surrounded by an equatorial optically-thick disc that is possibly still accreting, and an outflowing wind is located just above it.
The AMBER team also studied the very massive and luminous star h Carinae. By zooming into the very heart of this enigmatic object, h Carinae was shown to be surrounded by a fast and dense stellar wind that totally obscures the central star. The mass loss due to this stellar wind is enhanced along the polar axis (see Fig. 2) which is also the main axis of the Homunculus nebulae  at larger scale. These new observations show the similarities between the present-day wind and the ancient stellar eruptions that have generated the nebulae.
Several papers from this special feature focus on the later stages in a star’s life. Looking at the binary system g2 Velorum, consisting of a Wolf-Rayet star  and an O-type star, the AMBER measurements allowed the spectra of the two stars to be disentangled and might bring new information about their colliding winds. Last but not least, the authors observed the famous recurrent nova RS Ophiuchi after it exploded on Feb. 12th 2006. This event has been expected since its last outburst 21 years ago. AMBER was able to detect the extension of the expanding emission only 5 days after the discovery. These observations show a complex geometry and kinematics, far from the simple interpretation of a spherical fireball in extension (Fig. 3).
Fig. 2. The aspherical and latitude-dependent stellar wind of h Carinae. The artist’s impression visualizes the inner regions of h Carinae probed with AMBER at different wavelengths. The dense stellar wind (blue) totally obscures the central star and the direction of the outflowing wind corresponds to the main axis of the Homunculus nebulae at larger scale.
As illustrated above, AMBER’s capabilities, combined with the current VLTI performance, allow astronomers to obtain a profusion of new results on various hot topics in stellar physics, from the earliest to the latest stages of the stellar evolution. When the VLTI achieves full performance, AMBER should be able to reach its most ambitious objectives: observation of the dust tori in active galactic nuclei and of the hot extrasolar planets close to their parent stars.
Fig. 3. Observation of the explosion of the recurrent nova RS Ophiuchi. Sketch of the extension observed in the near-infrared with AMBER (ellipses) 5.5 days after the explosion compared to the radio structure observed 13.8 days after.
 The AMBER consortium, led by R. Petrov (principal investigator) and F. Malbet (project scientist), includes researchers from the Laboratoire d’Astrophysique de Grenoble (France), Laboratoire Universitaire d'Astrophysique de Nice (France), Max-Planck Institut für Radioastronomie (Bonn, Germany), INAF-Observatorio Astrofisico di Arcetri (Italy), Observatoire de la Côte d’Azur (Nice, France).
 Be stars are hot stars (B-type) with prominent hydrogen emission lines.
 The Homunculus nebula is the emission nebula surrounding h Carinae.
 A Wolf-Rayet star is an evolved massive star that rapidly loses mass through a very strong stellar wind.
The Astronomy & Astrophysics special feature (volume 464 n°1 – March II 2007) on the first AMBER results includes 11 articles. They are freely available on the A&A web site.
Table of contents of the A&A special feature (and free access to the PDF files)
For additional information and access to the associated press releases, see the AMBER web site.
Dr. Fabien Malbet
LAOG/CNRS/UJF, Grenoble, France
Email: Fabien.Malbet (at) obs.ujf-grenoble.fr
Phone: +33 4 76 63 58 33
Dr. Romain Petrov
LUAN/CNRS/UNSA, Nice, France
Email: Romain.Petrov (at) unice.fr
Phone: +33 4 92 07 63 47
MPifR, Bonn, Germany
Email: weigelt (at) mpifr-bonn.mpg.de
Phone: +49 (228) 525 243
Dr. Leonardo Testi
OAA/INAF, Firenze, Italy
Email: lt (at) arcetri.astro.it
Phone: +39 055 2752 234
Dr. Jennifer Martin
Astronomy & Astrophysics
61, avenue de l'Observatoire
75014 Paris, France
Phone: +33 1 43 29 05 41 - Email: aanda.paris (at) obspm.fr
© Astronomy & Astrophysics 2007