The Maunakea Spectroscopic Explorer (MSE) project will transform the CFHT 3.6m optical telescope into an 11.25m multi-object spectroscopic facility with a 1.5 square degrees field of view. It will get the ability to simultaneously measure 4,332 objects with two spectral resolution modes respectively low/moderate resolution of R=3,000/6,000, and high resolution of R≥30,000. Multi-object high resolution (HR) spectrographs take the challenge of simultaneously producing a thousand high-resolution spectra respectively at blue, green, and red channels. A few different optical designs have been investigated deeply by scientific and technical groups since 2018. With the trade-off studies between science cases and technical capability in dispersers, the paper describes a new design proposal based on using the echelle gratings and taking reference to the industrialized production process. It enables to reduce the technical risk in dispersers and switch the observing wavelength bandpasses quickly by sorting filters.
MSE is a massively multiplexed spectroscopic survey facility that will replace the Canada-France-Hawaii-Telescope. This 11.25-m telescope, with its 1.5 square degrees field-of-view, will observe 4,332 astronomical targets in every pointing by using fibers to pick up the light at the prime focus w and transmitting it to banks of low/moderate (R=3,000/6,000) and high (R=30,000) resolution spectrographs. Piezo actuators position individual fibers in the field of view to enable simultaneous full field coverage for both resolution modes. A Calibration system ensures good quality and reliable raw data. This instrument suite, dedicated to large scale surveys, will enable MSE to collect a massive amount of data: equivalent to a full SDSS Legacy Survey every 7 weeks. Since 2018, MSE has made progress by refining the science cases, exploring design space for the instrumentation and understanding the limits of chosen telescope and instrument architecture to achieve the science cases. To improve performance and reduce risk, challenging conceptual designs for spectrographs have been reconsidered. As well, the science calibration plan and associated technical hardware system have been developed to a conceptual design level. This paper includes a discussion of the trades, design decisions and outstanding risks for the entire instrument suite with a focus on recent developments for the spectrographs and calibration system.
"A joint project has been proposed by the Chinese and Spanish astronomy communities, to develop a high-resolution, ultra- stable spectrograph for the Gran Telescopio Canarias (GTC) at La Palma. Being expected to conduct precise radial velocity (PRV) measurement with extreme precision of up to 10 cm s−1, the instrument would promote the very high, present interest in the astronomical community to detect and characterize exoplanets. The project successfully passed the conceptual design review (CoDR) in 2019. The instrument is composed of a near-UV band spectrograph (UVS) and a visible band spectrograph (VIS). They provide a spectral resolving power of R ≥100,000 in the visible band (420 nm – 780 nm), and R≥25,000 in the UV band (310 nm – 420 nm). The VIS subsystem will be enclosed in an ultra-stable environment in the Coudé room for the stellar precise radial velocity (PRV) measurements. T he UVS subsystem will be located near the Nasmyth focus to improve the total throughput at the wavelength shorter than 400 nm, to ensure various additional science cases ranging from stellar evolution to the measurement of fundamental constants. This paper gives an overview of the project background, science cases, and technical considerations during the conceptual design phase."
The Maunakea Spectroscopic Explorer (MSE) project will transform the CFHT 3.6m optical telescope to an 11.25 m multi- object spectroscopic facility with an ability to simultaneously detect thousands of objects with three spectral resolution modes, low resolution of R ~ 3,000, moderate resolution of R ~ 5,000, and high resolution of R 20,000 ~ 40,000, respectively. The multi-object high resolution (HR) spectrographs can derive simultaneously around one thousand high- resolution spectra of Blue, Green, and Red channels, respectively. Based on the discussion of the science cases in 2019, the design team suggested that the optimal design of HR spectrograph should balance between the new scientific requirements and technical feasibility. Here, the HR design team shows the trade-off study's progress and introduces a new preliminary design.
The Manfred Hirt Planet Spectrograph (MaHPS) — formerly also referred to as FOCES — is a high-resolution echelle spectrograph at the 2m telescope of the Wendelstein Observatory. One of its main scientific goals is the detection of planets at the few m/s level. To achieve such high precisions on a long-term scale, environmental stabilization of the instrument is required. The currently used temperature and pressure control systems are introduced and we present two different temperature control setups, with two and three actively controlled layers respectively. A series of measurements with an Astro Frequency Comb (AFC) as calibrator is shown to illustrate the system performance.
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