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Figure 1: Left panel: Sketch of the AMBER instrument. The light enters the instrument from the left and is propagating from left to right until the raw data are recorded on the detector. Further details are given in the text. Right panel: AMBER reconstituted image from the raw data recorded during the 3-telescope observation of the calibrator HD135382 in February 2005, in the medium spectral resolution mode. DK corresponds to a dark region, Pk are the vertically dispersed spectra obtained from each telescope, and IF is the spectrally dispersed interferogram. |
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Figure 2:
Outputs of the calibration procedures. Examples have been chosen for one given wavelength:
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Figure 3: Contrast loss due to polarization effects and partial resolution of the internal source as a function of the wavelength. The 3-telescope P2VM used is the same as the one presented in Fig. 2. The errors bars are roughly at the level of the contrast loss rms along the wavelength. In other words, the contrast loss is constant over the wavelength range. |
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Figure 4: Example of fringe-fitting by the carrying waves in the 3-telescope case. The DC-corrected interferogram is plotted (dashdot line) with the error bars. The result of the fit is overplotted (solid line). |
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Figure 5:
Left: sample of 100 successive interferograms as recorded during the observation with two telescopes of
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Figure 6:
Visibility as a function of the fringe SNR criterion. Left: for jitter-free simulated data, using the real photometry observed on
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Figure 7:
Estimation of the raw squared visibility and its error-bars as a function of the wavelength for the observed calibrator
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Figure 8: Histogram of the bootstrapped population of estimated squared visibilities for a given wavelength. The fit of this histogram by a Gaussian function is superimposed. The mean value and the root mean square of the Gaussian distribution give the statistics of the estimated visibility. |
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Figure 9:
Example of differential phases and closure
phase computation on an observed object with a rotating feature in
the
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Figure 10:
Piston estimation from the fringe
pattern. From left to right is (i) the raw fringe pattern, the
corresponding phase; (ii) the estimated linear component of the phase from the least square fit; and (iii) a piston time-sequence over 250 s. Note that the piston rms is around
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