Efficient ultra-broadband low-resolution astrophotonic spectrographs

Abstract

Broadband low-resolution near-infrared spectrographs in a compact form are crucial for ground- and space-based astronomy and other fields of sensing. Astronomical spectroscopy poses stringent requirements including high efficiency, broad band operation (> 300 nm), and in some cases, polarization insensitivity. We present and compare experimental results from the design, fabrication, and characterization of broadband (1200 - 1650 nm) arrayed waveguide grating (AWG) spectrographs built using the two most promising low-loss platforms - Si 3 N 4 (rectangular waveguides) and doped-SiO 2 (square waveguides). These AWGs have a resolving power ( λ /Δ λ ) of ∼200, free spectral range of ∼ 200-350 nm, and a small footprint of ∼ 50-100 mm 2 . The peak overall (fiber-chip-fiber) efficiency of the doped-SiO 2 AWG was ∼ 79% (1 dB), and it exhibited a negligible polarization-dependent shift compared to the channel spacing. For Si 3 N 4 AWGs, the peak overall efficiency in TE mode was ∼ 50% (3 dB), and the main loss component was found to be fiber-to-chip coupling losses. These broadband AWGs are key to enabling compact integrations such as multi-object spectrographs or dispersion back-ends for other astrophotonic devices such as photonic lanterns or nulling interferometers.