Table 1: Parameters of the computer-simulated LBT raw images (Fig. 1).
Primary mirror size 8.4 m
Primary mirror center-to-center distance 14.4 m
Optical transmission 0.5
Quantum efficiency of the detector 0.6
Number of pixels per frame 2048 $\times $ 2048
Pixel size 5.0 mas
read-out noise 11 e-
Central wavelength / 1.25/0.3 $\mu $m
bandwidth  
Object type extended galaxy based on the HST image of NGC 3504
Total object magnitude mJ = 17.0
Magnitudes of the 4 reference stars in the 2048$\times $2048 pixel FOV mJ = 20.0, 20.5, 20.5, 21.0
Magnitude of the sky background per square arcsec mJ = 16.0
Position angles of the pupil axis $0^\circ$, $30^\circ$, $60^\circ$, $90^\circ$, $120^\circ$, $150^\circ$
Strehl ratio 0.3
Exposure time 600 s for each of the above six pupil position angles

Source LaTeX | All tables | In the text

Article Contents
1 Introduction
2 The building block method
3 Reconstruction of aperture-synthesis images from computer-simulated LBT data
4 Image reconstruction from LINC-NIRVANA data obtained with a laboratory LBT simulator
5 Space-variant Building Block method: image reconstruction from LBT raw data in the case of space-variant PSFs
6 Conclusions
References
Online Material
Appendix A: The Lagrange multiplier $\mu $ in the regularized Building Block method
Appendix B: The advantage of Fourier-masked LBT raw images
Appendix C: Space-variant BB method
List of tables
List of figures