Table 2: Restoration errors of the reconstructions using the galaxy test object shown in Fig. 1 (see also Table 1) with total magnitudes of $J=16.0^{\rm m}$ , $J=17.0^{\rm m}$ , and $J=18.0^{\rm m}$ . The restoration errors listed are averages of 10 statistically independent LBT data sets (see text).
J magnitude RL OSEM BB

16.0 $4.29\pm0.14$ % $4.81\pm0.10$ % $4.09\pm0.14$ %

17.0 $5.41\pm0.10$ % $5.58\pm0.08$ % $5.30\pm0.10$ %

18.0 $7.38\pm0.22$ % $7.63\pm0.16$ % $7.43\pm0.22$ %

**Table 2:** Restoration errors of the reconstructions using the galaxy test object shown in Fig. 1 (see also Table 1) with total magnitudes of $J=16.0^{\rm m}$ , $J=17.0^{\rm m}$ , and $J=18.0^{\rm m}$ . The restoration errors listed are averages of 10 statistically independent LBT data sets (see text).
J magnitude	RL	OSEM	BB
16.0	$4.29\pm0.14$ %	$4.81\pm0.10$ %	$4.09\pm0.14$ %
17.0	$5.41\pm0.10$ %	$5.58\pm0.08$ %	$5.30\pm0.10$ %
18.0	$7.38\pm0.22$ %	$7.63\pm0.16$ %	$7.43\pm0.22$ %

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