Table 3: Parameters of our laboratory simulation.
Optical transmission 0.5

Quantum efficiency of the detector 0.6

Pixel size 18.0 $\mu$ m

Number of detector pixels 512 $\times$ 512

RON 17 e^-

Central wavelength / filter width 1.65/0.3 $\mu$ m

total object magnitudes m_H = 16.2/17.1/17.8/19.1

PSF star magnitude m_H = 19.2

Magnitude of the sky background per square arcsec m_H = 14.0

Pupil position angles $0^\circ$ , $30^\circ$ , $60^\circ$ , $90^\circ$ , $120^\circ$ , $150^\circ$

Simulated Strehl ratio 0.10

Exposure time per pupil position angle 600 s

**Table 3:** Parameters of our laboratory simulation.
Optical transmission	0.5
Quantum efficiency of the detector	0.6
Pixel size	18.0 $\mu$ m
Number of detector pixels	512 $\times$ 512
RON	17 e^-
Central wavelength / filter width	1.65/0.3 $\mu$ m
total object magnitudes	m_H = 16.2/17.1/17.8/19.1
PSF star magnitude	m_H = 19.2
Magnitude of the sky background per square arcsec	m_H = 14.0
Pupil position angles	$0^\circ$ , $30^\circ$ , $60^\circ$ , $90^\circ$ , $120^\circ$ , $150^\circ$
Simulated Strehl ratio	0.10
Exposure time per pupil position angle	600 s

Source LaTeX | All tables | In the text

	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