A. Richichi

Arcetri Astrophysical Observatory

Author Statistics

Papers

Citation

H-Index

i-10 index

Research Trends

Author Order

Document Type

Co-Authors

M. Wittkowski

European Southern Observatory

Andreas Glindemann

European Southern Observatory

Francesco Paresce

Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna

S. Morel

VIB-KU Leuven Center for Microbiology

P. Kervella

Qualissima (France)

F. Delplancke

European Southern Observatory

M. Schöller

BOKU University

F. Malbet

Institut de Planétologie et d'Astrophysique de Grenoble

M. Tarenghi

Atacama Large Millimeter Submillimeter Array

Rainer Wilhelm

Collecte Localisation Satellites (France)

Cooperative Institutions

Centre National de la Recherche Scientifique

280

European Southern Observatory

233

Max Planck Society

175

Observatoire de la Côte d’Azur

137

Max Planck Institute for Astronomy

123

Observatoire de Paris

European Southern Observatory

Université Côte d'Azur

Max Planck Institute for Radio Astronomy

Université Paris Cité

Author Statistics

Papers

Citation

H-Index

i-10 index

Research Field

The VLTI and its Subsystems

EAS Publications Series (2003)

Andreas Glindemann J. Algomedo Rodrigo Amestica P. Ballester B. Bauvir

The Very Large Telescope (VLT) Observatory on Cerro Paranal (2635 m) in Northern Chile is approaching completion. After the four 8-m Unit Telescopes (UT) individually saw first light in the last years, two of them were combined for the first time on October 30, 2001 to form a stellar interferometer, the VLT Interferometer. The remaining two UTs will be integrated into the interferometric array later this year, so that any two UTs can be used for interferometry. In this article, we will describe the subsystems of the VLTI and the planning for the following years.

Very Large Telescope

10.1051/eas:2003008

Cite

Citations (1)

First Fringes with ANTU and MELIPAL

Msngr (2001)

Andreas Glindemann P. Ballester B. Bauvir Erich Bugueno Michael Cantzler

A. GLINDEMANN, P. BALLESTER, B. BAUVIR, E. BUGUENO, M. CANTZLER, S. CORREIA, F. DELPLANCKE, F. DERIE, P. DUHOUX, E. DI FOLCO, A. GENNAI, B. GILLI, P. GIORDANO, P. GITTON, S. GUISARD, N. HOUSEN, A. HUXLEY, P. KERVELLA, M. KIEKEBUSCH, B. KOEHLER, S. LEVEQUE, A. LONGINOTTI, A. LOPEZ, S. MENARDI, S. MOREL, F. PARESCE, T. PHAN DUC, A. RAMIREZ, A. RICHICHI, M. SCHOLLER, J. SPYROMILIO, M. TARENGHI, A. WALLANDER, R. WILHELM, M. WITTKOWSKI

Source

Cite

Citations (1)

Astrophysics and Space Science (2003)

Andreas Glindemann J. Algomedo Rodrigo Amestica P. Ballester B. Bauvir

Very Large Telescope

10.1023/a:1026145709077

Cite

Citations (16)

Infrared high angular resolution measurements of stellar sources

Astronomy and Astrophysics (2001)

A. Richichi G. Calamai

In the framework of an ongoing series of high angular resolution observations by lunar occultations in the near infrared, we present accurate angular measurements for ten late-type giant stars, seven of which were measured for the first time. The sample includes one K and seven M stars. It also includes two S stars, representing to our knowledge the first direct determination of the angular diameter for this class of stars. The measured angular diameters range from 2.50 to 4.82 milliarcsec, with an average accuracy <5% . An exception is represented by the case of a star with a faint companion, where we have been able to investigate in detail the bias on the diameter determination, and hence on the effective temperature, which would be caused if the companion had not been included in the analysis. We suggest that faint undetected companions could explain at least some of the hitherto known cases of stars with effective temperatures remarkably lower than the standard calibration. For seven of the stars in the sample, we have used our own photometry in conjunction with values from the literature, to compute the bolometric fluxes and the effective temperatures, which we discuss in the context of existing calibrations. With the achieved accuracy level in the angular diameter, such measurements are also valuable as calibrators or science verification targets for modern large ground-based interferometers.

Angular diameter

Giant star

Effective temperature

10.1051/0004-6361:20011451

Cite

Citations (2)

Science opportunities with AMBER, the near-IR VLTI instrument

Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE (2000)

A. Richichi T. Bloêcker Renaud Foy Didier Fraix‐Burnet Bruno Lopez

AMBER is the near-IR instrument for the VLTI, which will offer the possibility of combining two or three beams from either the 8 meter VLT main telescopes or the 1.8 meter auxiliary telescopes. With spectral dispersion up to 10,000 high visibility accuracy and the ability to obtain closure phases, AMBER will offer the means to perform high quality interferometric measurements in the 1 - 2.5 micron range initially, with later extensions to other portions of the spectrum. These design characteristics, coupled to the VLT interferometer potential, open up the access to investigation of several classes of objects, from stellar to extragalactic astronomy. We will review the projected performance in terms of sensitivity and angular resolution, and illustrate the potential applications in some key research areas. In particular, we will present the work of the AMBER Science Group, which is evaluating simulated data of source models and interferometric outputs for the purpose of defining the criteria for observations.

Visibility

Very Large Telescope

Spectral resolution

10.1117/12.390266

Cite

Citations (5)

High‐Resolution Infrared Observations of GGD 27

The Astrophysical Journal (1997)

B. Stecklum M. Feldt A. Richichi G. Calamai P. O. Lagage

We present new high spatial resolution data of the GGD 27 complex, obtained both by speckle interferometry and by lunar occultation observations. Additionally, we performed imaging in the wavelength intervals 8-9 μm and 10-13 μm. The combination of these data with earlier VLA radio maps of Marti, Rodríguez, & Reipurth yields new hints on the nature of IRS 7. It also confirms the interpretation by Aspin et al. that their GGD 27 ILL is the illuminator of the reflection nebula north of IRS 2 as well as of IRS 2 itself. By using precise astrometric calibration, we show that IRS 7 is detected at all three wavelengths and presumably is an embedded B2 star. IRS 1 and IRS 17 still appear pointlike in the K band, although the 8.5 μm data indicate some extended emission around IRS 1, which is presumably caused by heated dust. Other objects in the region targeted by lunar occultation observations, such as HL 17, HL 47 (from Hartigan & Lada) and a hitherto anonymous star, hereafter denoted star 11, also appear pointlike in the K' band. These data complete our picture of the formation of massive stars in the region of GGD 27.

Occultation

Speckle imaging

Star (game theory)

10.1086/303864

Cite

Citations (19)

The VLTI and Its Subsystems

HAL (Le Centre pour la Communication Scientifique Directe) (2002)

Andreas Glindemann J. Algomedo R. Amestica P. Ballester B. Bauvir

Source

Cite

Citations (0)