PRAXIS: low thermal emission high efficiency OH suppressed fibre spectrograph

TL;DR

PRAXIS is an advanced fibre spectrograph that significantly improves near-infrared observations by using fibre Bragg gratings for OH suppression, high efficiency coatings, and low thermal noise design, enabling higher signal-to-noise ratios.

Contribution

PRAXIS introduces a new spectrograph design optimized for OH suppression using fibre Bragg gratings, achieving higher throughput and lower noise compared to previous instruments.

Findings

Potential sky background signal-noise ratio gain up to 9 with GNOSIS OH suppression.

Projected signal-noise ratio gain up to 17 with multicore fibre Bragg gratings.

Design successfully minimizes thermal emission and noise in the spectrograph.

Abstract

PRAXIS is a second generation instrument that follows on from GNOSIS, which was the first instrument using fibre Bragg gratings for OH background suppression. The Bragg gratings reflect the NIR OH lines while being transparent to light between the lines. This gives a much higher signal-noise ratio at low resolution but also at higher resolutions by removing the scattered wings of the OH lines. The specifications call for high throughput and very low thermal and detector noise so that PRAXIS will remain sky noise limited. The optical train is made of fore-optics, an IFU, a fibre bundle, the Bragg grating unit, a second fibre bundle and a spectrograph. GNOSIS used the pre-existing IRIS2 spectrograph while PRAXIS will use a new spectrograph specifically designed for the fibre Bragg grating OH suppression and optimised for 1470 nm to 1700 nm (it can also be used in the 1090 nm to 1260 nm band by changing the grating and refocussing). This results in a significantly higher transmission due to high efficiency coatings, a VPH grating at low incident angle and low absorption glasses. The detector noise will also be lower. Throughout the PRAXIS design special care was taken at every step along the optical path to reduce thermal emission or stop it leaking into the system. This made the spectrograph design challenging because practical constraints required that the detector and the spectrograph enclosures be physically separate by air at ambient temperature. At present, the instrument uses the GNOSIS fibre Bragg grating OH suppression unit. We intend to soon use a new OH suppression unit based on multicore fibre Bragg gratings which will allow increased field of view per fibre. Theoretical calculations show that the gain in interline sky background signal-noise ratio over GNOSIS may very well be as high as 9 with the GNOSIS OH suppression unit and 17 with the multicore fibre OH suppression unit.