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Performance limits of astronomical arrayed waveguide gratings on a silica platform.

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    Phase errors in arrayed waveguide gratings (AWG) impact astronomical spectroscopy. Post-processing effectively corrects these errors, removing them as a performance limitation for H-band observations.

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    Area of Science:

    • Optics and Photonics
    • Astronomy Instrumentation
    • Materials Science (Silica)

    Background:

    • Arrayed waveguide gratings (AWGs) are crucial for high-resolution spectroscopy in astronomy.
    • Phase errors arising from variations in optical waveguide lengths can degrade AWG performance.
    • Understanding and mitigating these errors is essential for advancing astronomical observation capabilities.

    Purpose of the Study:

    • To numerically and experimentally investigate the impact of phase errors on large, high-resolution AWGs.
    • To evaluate the effectiveness of a numerical phase error correction technique.
    • To determine the phase-error limited size of state-of-the-art waveguide arrays.

    Main Methods:

    • Scalar diffraction modeling to simulate AWG transmission spectra with random waveguide length variations.
    • Numerical simulation of phase error correction by trimming waveguide lengths.
    • Frequency-domain interferometry and Monte-Carlo fitting to measure optical length errors in a fabricated silica AWG.

    Main Results:

    • Phase errors significantly affect the performance of large, high-resolution AWGs.
    • Numerical post-processing effectively corrects phase errors by adjusting waveguide lengths.
    • The optical length error distribution of a custom silica AWG was accurately measured.
    • An estimate for the phase-error limited size of advanced waveguide arrays was determined.

    Conclusions:

    • Post-processing eliminates phase errors as a limiting factor for astronomical spectroscopy in the H-band.
    • This correction method enables the use of larger, high-resolution AWGs for astronomical applications.
    • The study provides critical insights for designing future AWG-based spectroscopic instruments.