Polarization is a fundamental property of the light and is very useful to measure the magnetic field vector of the various features that can be observed in the solar atmosphere. Ideally, a solar telescope should not introduce any polarization to the incoming light that could mask the one coming from the Sun. However, some instrumental polarization

Model-based systems engineering has as one of its central pillars the single source of truth that is usually a CAD model, or a model defined using a language such as SysML. However, having a single point of truth is not incompatible with using multiple modeling languages. A simple DSL like PORIS allows us to make instrument sketches much more

This paper describes the preliminary design of the Adaptive Secondary Mirror (ASM) for the European Solar Telescope (EST), as designed by TNO. This ASM will contain 1950 actuators over an optical aperture of Ø80cm. The mirror-shell of this ASM is concave with a radius of 2.156m and has a thickness of 2.5mm. To cope with the high optical heat-load

Small-ELF is a 3.5-meter telescope currently in development that will serve as a technology demonstrator for the much larger telescope named ELF (Exo-Life Finder). The ELF is proposed to be built with a minimum effective diameter of 12- meters and is designed to be scalable to a much larger size. The primary objective of the proposed design

The New Robotic Telescope (NRT) is a new UK/Spain 4-m optical telescope on La Palma. When complete it will be the world's largest and fastest, fully autonomous optical observatory and is being designed to address the coming era of time-domain and transient astrophysics. We summarise the planned software architecture, presented as a complete

The BIFROST instrument will be the first VLTI instrument optimised for high spectral resolution up to R=25,000 and operate between 1.05 and 1.7 μm. A key component of the instrument will be the spectrograph, where we require a high throughput over a broad bandwidth. In this contribution, we discuss the four planned spectral modes (R=50, R=1000, R