AMBER performances: signal-to-noise ratio analysis

Details AMBER performances: signal-to-noise ratio analysis AMBER performances: signal-to-noise ratio analysis

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000spie.4006..233m&link_type=abstract

Proc. SPIE Vol. 4006, p. 233-242, Interferometry in Optical Astronomy, Pierre J. Lena; Andreas Quirrenbach; Eds.

Astronomy and Astrophysics

Astronomy

Scientific paper

We present the method which computes the expected signal-to- noise ratio of the observations carried out by AMBER, the near-infrared focal instrument of the VLTI. We include photon noise, detector read-out noise, thermal noise as well as the instrument OPD stability and Strehl fluctuations. We believe that this algorithm can be extended to any other optical interferometers. The performances are computed in a variety of conditions: size of the apertures (8-m Unit telescopes or 1.8-m Auxiliary telescopes), adaptive optics correction (tip-tilt, 64 actuators), atmospheric conditions (averaged 0.7 arcsecond seeing and excellent 0.5 arcsecond seeing), wavelengths (from the J-band to the K-band), fringe tracking accuracy (from no to perfect fringe tracking), elementary exposure times, spectral resolution (35, 1000 and 10000), off-axis/on-axis operation.

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