Publications of the MPIfR
Optical & Infrared
Interferometry Group
Interferometric data
reduction with AMBER/VLTI.
Principle,
estimators and illustration
E. Tatulli, F. Millour, A. Chelli, G.
Duvert, B. Acke, O. Hernandez Utrera, K.-H. Hofmann,
S. Kraus, F. Malbet, P. Mège, R.G. Petrov, M. Vannier, G. Zins, P.
Antonelli, U. Beckmann,
Y. Bresson, M. Dugué, S. Gennari, L. Glück, P. Kern, S.
Lagarde, E. Le Coarer, F. Lisi,
K. Perraut, P. Puget, F. Rantakyrö, S. Robbe-Dubois, A. Roussel,
G. Weigelt, M. Accardo,
K. Agabi, E. Altariba, B. Arezki, E. Aristidi, C. Baffa, J.
Behrend, T. Blöcker, S. Bonhomme,
S. Busoni, F. Cassaing, J.-M. Clausse, J. Colin, C. Connot, A.
Delboulbé, A. Domiciano de Souza,
T. Driebe, P. Feautrier, D. Ferruzzi, T. Forveille, E. Fossat, R.
Foy, D. Fraix-Burnet, A. Gallardo,
E. Giani, C. Gil, A. Glentzlin, M. Heiden, M. Heininger, D. Kamm, M.
Kiekebusch,
D. Le
Contel, J.-M. Le Contel, T. Lesourd, B. Lopez, M. Lopez, Y.
Magnard, A. Marconi, G. Mars,
G. Martinot-Lagarde, P. Mathias, J.-L. Monin, D. Mouillet, D. Mourard,
E. Nussbaum,
K. Ohnaka, J. Pacheco, C. Perrier, Y. Rabbia, S. Rebattu, F.
Reynaud, A. Richichi, A. Robini,
M. Sacchettini, D. Schertl, M. Schöller, W. Solscheid, A. Spang,
P. Stee, P. Stefanini, M. Tallon,
I. Tallon-Bosc, D. Tasso, L. Testi, F. Vakili, O. von der Lühe,
J.-C. Valtier, and N. Ventura
Astronomy & Astrophysics, vol.464, pg.29-42
(2007)
Abstract
Aims.In this paper, we present an innovative
data reduction method for single-mode interferometry. It has been
specifically developed for the AMBER instrument, the three-beam
combiner of the Very Large Telescope Interferometer, but it can be
derived for any single-mode interferometer.
Methods.The
algorithm is based on a direct modelling of the fringes in the detector
plane. As such, it requires a preliminary calibration of the instrument
in order to obtain the calibration matrix that builds the linear
relationship between the interferogram and the interferometric
observable, which is the complex visibility. Once the calibration
procedure has been performed, the signal processing appears to be a
classical least-square determination of a linear inverse problem. From
the estimated complex visibility, we derive the squared visibility, the
closure phase, and the spectral differential phase.
Results.The
data reduction procedures have been gathered into the so-called amdlib
software, now available for the community, and are presented in this
paper. Furthermore, each step in this original algorithm is illustrated
and discussed from various on-sky observations conducted with the VLTI,
with a focus on the control of the data quality and the effective
execution of the data reduction procedures. We point out the present
limited performances of the instrument due to VLTI instrumental
vibrations which are difficult to calibrate.
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