The Maunakea Spectroscopic Explorer Book 2018

(Abridged) This is the Maunakea Spectroscopic Explorer 2018 book. It is intended as a concise reference guide to all aspects of the scientific and technical design of MSE, for the international astronomy and engineering communities, and related agencies. The current version is a status report of MSE's science goals and their practical implementation, following the System Conceptual Design Review, held in January 2018. MSE is a planned 10-m class, wide-field, optical and near-infrared facility, designed to enable transformative science, while filling a critical missing gap in the emerging international network of large-scale astronomical facilities. MSE is completely dedicated to multi-object spectroscopy of samples of between thousands and millions of astrophysical objects. It will lead the world in this arena, due to its unique design capabilities: it will boast a large (11.25 m) aperture and wide (1.52 sq. degree) field of view; it will have the capabilities to observe at a wide range of spectral resolutions, from R2500 to R40,000, with massive multiplexing (4332 spectra per exposure, with all spectral resolutions available at all times), and an on-target observing efficiency of more than 80%. MSE will unveil the composition and dynamics of the faint Universe and is designed to excel at precision studies of faint astrophysical phenomena. It will also provide critical follow-up for multi-wavelength imaging surveys, such as those of the Large Synoptic Survey Telescope, Gaia, Euclid, the Wide Field Infrared Survey Telescope, the Square Kilometre Array, and the Next Generation Very Large Array.Comment: 5 chapters, 160 pages, 107 figure

The E-ELT first light spectrograph HARMONI: capabilities and modes

Trabajo presentado en SPIE Astronomical Telescopes, celebrado en San Diego (California), del 26 de junio al 1 de julio de 2016HARMONI is the E-ELT's first light visible and near-infrared integral field spectrograph. It will provide four different spatial scales, ranging from coarse spaxels of 60 × 30 mas best suited for seeing limited observations, to 4 mas spaxels that Nyquist sample the diffraction limited point spread function of the E-ELT at near-infrared wavelengths. Each spaxel scale may be combined with eleven spectral settings, that provide a range of spectral resolving powers (R 3500, 7500 and 20000) and instantaneous wavelength coverage spanning the 0.5 - 2.4 ¿m wavelength range of the instrument. In autumn 2015, the HARMONI project started the Preliminary Design Phase, following signature of the contract to design, build, test and commission the instrument, signed between the European Southern Observatory and the UK Science and Technology Facilities Council. Crucially, the contract also includes the preliminary design of the HARMONI Laser Tomographic Adaptive Optics system. The instrument's technical specifications were finalized in the period leading up to contract signature. In this paper, we report on the first activity carried out during preliminary design, defining the baseline architecture for the system, and the trade-off studies leading up to the choice of baseline

Métrologie en milieu cryogénique grâce à un périscope de pointe

International audienceThe PIC (Photogrammetry Inside Cryostat) is a cutting-edge periscope designed to be used during the prototyping, testing and alignment phase of HARMONI, one of the first-generation instruments of the Extremely Large Telescope. The challenge posed by operating the HARMONI instrument at a temperature of 130 K required the development of different non-contact measurement techniques to qualify optical and mechanical parts without touching them. Photogrammetry is a non-contact measurement technique, but it needed to be adapted to be used in a cryostat ; this led to the development of the PIC. The periscope consists of a combination of six lenses, two mirrors, and three motorized degrees of freedom (the whole is mounted upside down on the lid of the test cryostat at CRAL in Lyon) and work together with an external camera to capture images at various angles. This is essential for obtaining accurate photogrammetric measurements. The motorized rotation systems allow for precise and controlled movements, and the combination of lenses and mirrors ensure that the images captured by the external camera are of the highest quality. The goal of the PIC is to obtain an accuracy of 25 µm + 5 µm/m, making it an essential component of the HARMONI tools and a major advancement in cryogenic photogrammetry.Le PIC (Photogrammetry Inside Cryostat) est un périscope de pointe conçu pour être utilisé pendant la phase de prototypage, de test et d'alignement de HARMONI, l'un des instruments de première génération de l'Extremely Large Telescope. Le défi posé par le fonctionnement de l'instrument HARMONI à une température de 130 K a nécessité le développement de différentes techniques de mesure sans contact pour qualifier les pièces optiques et mécaniques sans les toucher. La photogrammétrie est une technique de mesure sans contact, mais elle devait être adaptée pour être utilisée dans un cryostat, ce qui a conduit au développement du PIC. Le périscope se compose d'une combinaison de six lentilles, de deux miroirs et de trois degrés de liberté motorisés (l'ensemble est monté à l'envers sur le couvercle du cryostat d'essai du CRAL à Lyon) et fonctionne avec une caméra externe pour capturer des images sous différents angles. Ceci est essentiel pour obtenir des mesures photogrammétriques précises. Les systèmes de rotation motorisés permettent des mouvements précis et contrôlés, et la combinaison de lentilles et de miroirs garantit que les images capturées par la caméra externe sont de bonne qualité. L'objectif du PIC est d'obtenir une précision de 25 µm + 5 µm/m, ce qui en fait une composante essentielle des outils d'AIT d'HARMONI et une avancée majeure dans la photogrammétrie cryogénique

The E-ELT first light spectrograph HARMONI: capabilities and modes

HARMONI is the E-ELT’s first light visible and near-infrared integral field spectrograph. It will provide four different spatial scales, ranging from coarse spaxels of 60 × 30 mas best suited for seeing limited observations, to 4 mas spaxels that Nyquist sample the diffraction limited point spread function of the E-ELT at near-infrared wavelengths. Each spaxel scale may be combined with eleven spectral settings, that provide a range of spectral resolving powers (R ~3500, 7500 and 20000) and instantaneous wavelength coverage spanning the 0.5 – 2.4 μm wavelength range of the instrument. In autumn 2015, the HARMONI project started the Preliminary Design Phase, following signature of the contract to design, build, test and commission the instrument, signed between the European Southern Observatory and the UK Science and Technology Facilities Council. Crucially, the contract also includes the preliminary design of the HARMONI Laser Tomographic Adaptive Optics system. The instrument’s technical specifications were finalized in the period leading up to contract signature. In this paper, we report on the first activity carried out during preliminary design, defining the baseline architecture for the system, and the trade-off studies leading up to the choice of baseline

The Maunakea Spectroscopic Explorer Book 2018

(Abridged) This is the Maunakea Spectroscopic Explorer 2018 book. It is intended as a concise reference guide to all aspects of the scientific and technical design of MSE, for the international astronomy and engineering communities, and related agencies. The current version is a status report of MSE's science goals and their practical implementation, following the System Conceptual Design Review, held in January 2018. MSE is a planned 10-m class, wide-field, optical and near-infrared facility, designed to enable transformative science, while filling a critical missing gap in the emerging international network of large-scale astronomical facilities. MSE is completely dedicated to multi-object spectroscopy of samples of between thousands and millions of astrophysical objects. It will lead the world in this arena, due to its unique design capabilities: it will boast a large (11.25 m) aperture and wide (1.52 sq. degree) field of view; it will have the capabilities to observe at a wide range of spectral resolutions, from R2500 to R40,000, with massive multiplexing (4332 spectra per exposure, with all spectral resolutions available at all times), and an on-target observing efficiency of more than 80%. MSE will unveil the composition and dynamics of the faint Universe and is designed to excel at precision studies of faint astrophysical phenomena. It will also provide critical follow-up for multi-wavelength imaging surveys, such as those of the Large Synoptic Survey Telescope, Gaia, Euclid, the Wide Field Infrared Survey Telescope, the Square Kilometre Array, and the Next Generation Very Large Array

HARMONI at ELT: overview of the capabilities and expected performance of the ELT's first light, adaptive optics assisted integral field spectrograph.

International audienc