Portal de Periódicos da CAPES

ERIS: preliminary design phase overview

2014; SPIE; Volume: 9147; Linguagem: Inglês

10.1117/12.2055140

1996-756X

H. Kuntschner, L. Jochum, Paola Amico, Johannes Klaas Dekker, F. Kerber, Enrico Marchetti, Matteo Accardo, R. Brast, Martin Brinkmann, Ralf Conzelmann, Bernard Délabre, Michel Duchateau, Enrico Fedrigo, Gert Finger, Christoph Frank, Fernando G. Rodriguez, Barbara Klein, J. Knudstrup, Miska Le Louarn, Lars Lundin, A. Modigliani, Michael Müller, Mark Neeser, Sébastien Tordo, E. Valenti, Frank Eisenhauer, E. Sturm, H. Feuchtgruber, E. M. George, Michael Hartl, Reiner Hofmann, Heinrich J. Huber, Markus Plattner, J. Schubert, Karl Tarantik, E. Wiezorrek, Michael R. Meyer, Sascha P. Quanz, Adrian M. Glauser, Harald Weisz, Simone Esposito, Marco Xompero, Guido Agapito, J. Antichi, Valdemaro Biliotti, Marco Bonaglia, Runa Briguglio, Luca Carbonaro, G. Cresci, Luca Fini, Enrico Pinna, Alfio Puglisi, Fernando Quirós-Pacheco, Armando Riccardi, Gianluca Di Rico, Carmelo Arcidiacono, M. Dolci,

Advanced Data Storage Technologies

The Enhanced Resolution Imager and Spectrograph (ERIS) is the next-generation adaptive optics near-IR imager and spectrograph for the Cassegrain focus of the Very Large Telescope (VLT) Unit Telescope 4, which will soon make full use of the Adaptive Optics Facility (AOF). It is a high-Strehl AO-assisted instrument that will use the Deformable Secondary Mirror (DSM) and the new Laser Guide Star Facility (4LGSF). The project has been approved for construction and has entered its preliminary design phase. ERIS will be constructed in a collaboration including the Max- Planck Institut für Extraterrestrische Physik, the Eidgenössische Technische Hochschule Zürich and the Osservatorio Astrofisico di Arcetri and will offer 1 - 5 μm imaging and 1 - 2.5 μm integral field spectroscopic capabilities with a high Strehl performance. Wavefront sensing can be carried out with an optical high-order NGS Pyramid wavefront sensor, or with a single laser in either an optical low-order NGS mode, or with a near-IR low-order mode sensor. Due to its highly sensitive visible wavefront sensor, and separate near-IR low-order mode, ERIS provides a large sky coverage with its 1' patrol field radius that can even include AO stars embedded in dust-enshrouded environments. As such it will replace, with a much improved single conjugated AO correction, the most scientifically important imaging modes offered by NACO (diffraction limited imaging in the J to M bands, Sparse Aperture Masking and Apodizing Phase Plate (APP) coronagraphy) and the integral field spectroscopy modes of SINFONI, whose instrumental module, SPIFFI, will be upgraded and re-used in ERIS. As part of the SPIFFI upgrade a new higher resolution grating and a science detector replacement are envisaged, as well as PLC driven motors. To accommodate ERIS at the Cassegrain focus, an extension of the telescope back focal length is required, with modifications of the guider arm assembly. In this paper we report on the status of the baseline design. We will also report on the main science goals of the instrument, ranging from exoplanet detection and characterization to high redshift galaxy observations. We will also briefly describe the SINFONI-SPIFFI upgrade strategy, which is part of the ERIS development plan and the overall project timeline.