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Optical interferometry is a powerful technique to achieve high angularresolution. However, its main issue is its lack of sensitivity, compared toother observation techniques. Efforts have been made in the previous decade toimprove the sensitivity of optical interferometry, with instruments such asPIONIER and GRAVITY at VLTI, or MIRC-X and MYSTIC at CHARA. While thoseinstruments pushed on sensitivity, their design focus was not the sensitivitybut relative astrometric accuracy, imaging capability, or spectral resolution.Our goal is to build an instrument specifically designed to optimize forsensitivity. This meant focusing our design efforts on different parts of theinstrument and investigating new technologies and techniques. First, we makeuse of the low-noise C-RED One camera using e-APD technology and provided byFirst Light Imaging, already used in the improvement of sensitivity in recentnew instruments. We forego the use of single-mode fibers but still favor animage plane design that offers more sensitivity than a pupil plane layout. Wealso use a minimum number of optical elements to maximize the throughput of thedesign, using a long focal length cylindrical mirror. We chose to limit ourdesign to 3 beams, to have the capability to obtain closure phases, but notdilute the incoming flux in more beam combinations. We also use in our designan edge filter to have the capability to observe H- and K-band at the sametime. We use a low spectral resolution, allowing for group delay fringetracking but maximizing the SNR of the fringes for each spectral channel. Allthese elements will lead to a typical limiting magnitude between 10 and 11 inboth H- and K-bands.

Design of the new CHARA instrument SILMARIL: pushing the sensitivity of a 3-beam combiner in the H- and K-bands