2-09
Akira Endo
Delft University of Technology
From DESHIMA to airborne integral field spectrometers
3D imaging spectrometers with ultra-wide instantaneous bandwidths (~octave) and wide fields of view in the sub-THz band (0.1-1 THz) can be realized by integrating many spectroscopic pixels (spaxels) on a wafer using superconducting electronics. The integrated spectrometer design is especially advantageous for airborne observatories, because it makes the instrument compact, lightweight, and reliable. Furthermore, the spatial and spectral sampling of the ISS can be tailored towards different science cases, by exchanging the integral-field-unit (IFU) wafer. This IFU technology also enables a future generation of high-resolution spectroscopy instrument architectures by offering a compact order-sorting scheme in Fabry-Pérot or FTS-based spectroscopic imaging systems. The upper frequency limit is ~1 THz, limited by the gap frequencies of superconductors that are suited for transmission line circuits (e.g., NbTiN, NbN). This makes ~0.5–1 THz a territory uniquely suited for an airborne ISS, where the atmospheric transmission from ground is limited, even above the best observing sites, especially in the H2O absorption bands. Potential targets include multi-line mapping, high-redshift galaxies, and line-intensity mapping. I will present the instrument design, performance, and on-sky measurements of the first-generation ISS spectrometer DESHIMA on the ground-based ASTE telescope, including atmospheric noise removal techniques that we test with measured data and simulations.
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