Context — The Large Interferometer for Exoplanets (LIFE) is a proposed space mission to characterise the atmosphere of terrestrial exoplanets, which is planned to operate in the mid-infrared wavelength region from 6μm to 16μm. A key requirement needed to study the feasibility of this mission is to demonstrate broadband nulling at cryogenic temperatures (15K), at flux levels comparable to the astronomical sources that LIFE will detect. The Nulling Interferometer Cryogenic Experiment (NICE) is a technology demonstrator built to fulfil this purpose.

Aim — The objective of NICE is to demonstrate a broadband null with a null depth of 10⁻⁵ and stability of 10⁻⁸ while maintaining a high system throughput, and consequently a high level of sensitivity, sufficient to detect an Earth twin at 10pc. We describe the optical requirements, the current progress of NICE in the warm phase, and future plans.

Methods — NICE is a Single-Bracewell nuller with closed loop optical path-length control, currently operating at ambient conditions. We use a 3.85μm laser with 150nm bandwidth to demonstrate achromatic nulling capability, and a narrowband (< 0.5nm bandwidth) 4.5μm laser to demonstrate stability.

Results — We achieve an achromatic null depth of 4.39 · 10⁻⁴ with a stability of σ = 5.02 · 10⁻⁴ over a duration of 60s without closed loop control, and a stabilised narrow-band null of 2.05 · 10⁻⁴ with σ = 9.36 · 10⁻⁵ over a duration of 120s.

Conclusions — NICE has both demonstrated achromatic operation and closed loop control to stabilise the null. However, the mean null depth and the null stability achieved do not yet meet the requirements, by a factor of 20 and 104 respectively. This will be improved in future iterations.

Modern precise radial velocity spectrometers are designed to infer the existence of planets orbiting other stars by measuring few-nm shifts in the positions of stellar spectral lines recorded at high spectral resolution on a large-area digital detector. While the spectrometer may be highly stabilized in terms of temperature, the detector itself may undergo changes in temperature during readout that are an order of magnitude or more larger than the other optomechanical components within the instrument. These variations in detector temperature can translate directly into systematic measurement errors. We explore a technique for reducing the amplitude of CCD temperature variations by shuffling charge within a pixel in the parallel direction during integration. We find that this “dither clocking” mode greatly reduces temperature variations in the CCDs being tested for the NEID spectrometer. We investigate several potential negative effects this clocking scheme could have on the underlying spectral data.

Teledyne’s H2RG detector images suffer from crosshatch like patterns, which arise from subpixel quantum efficiency (QE) variation. We present our measurements of this subpixel QE variation in the Habitable-Zone Planet Finder’s H2RG detector. We present a simple model to estimate the impact of subpixel QE variations on the radial velocity and how a first-order correction can be implemented to correct for the artifact in the spectrum. We also present how the HPF’s future upgraded laser frequency comb will enable us to implement this correction.