A4 Refereed article in a conference publication
The NIR spectrograph for the new SOXS instrument at the NTT
Authors: F. Vitali, M. Aliverti, G. Capasso, F. D'Alessio, M. Munari, M. Riva, S. Scuderi, R. Zanmar Sanchez, S. Campana, P. Schipani, R. Claudi, A. Baruffolo, S. Ben-Ami, F. Biondi, A. Brucalassi, R. Cosentino, D. Ricci, P. D'Avanzo, O. Diner, H. Kuncarayakti, A. Rubin, J. Achrén, J. A. Araiza-Duran, I. Arcavi, A. Bianco, E. Cappellaro, M. Colapietro, M. Della Valle, S. D'Orsi, D. Fantinel, J. Fynbo, A. Gal-Yam, M. Genoni, M. Hirvonen, J. Kotilainen, T. Kumar, M. Landoni, J. Lehti, G. Li Causi, L. Marafatto, S. Mattila, G. Pariani, G. Pignata, M. Rappaport, B. Salasnich, S. Smartt, M. Turatto
Editors: Christopher J. Evans, Luc Simard, Hideki Takami
Conference name: SPIE Astronomical Telescopes + Instrumentation
Publisher: SPIE
Publication year: 2018
Journal: Proceedings of SPIE : the International Society for Optical Engineering
Book title : Ground-based and Airborne Instrumentation for Astronomy VII
Journal name in source: Proceedings of SPIE - The International Society for Optical Engineering
Volume: 10702
Number of pages: 13
ISBN: 978-1-5106-1957-9
ISSN: 0277-786X
DOI: https://doi.org/10.1117/12.2311466
Self-archived copy’s web address: https://arxiv.org/abs/1809.01511
We present the NIR spectrograph of the Son Of XShooter (SOXS) instrument
for the ESO-NTT telescope at La Silla (Chile). SOXS is a R~4,500 mean
resolution spectrograph, with a simultaneously coverage from about 0.35
to 2.00 μm. It will be mounted at the Nasmyth focus of the NTT. The two
UV-VIS-NIR wavelength ranges will be covered by two separated arms. The
NIR spectrograph is a fully criogenic echelle-dispersed spectrograph,
working in the range 0.80- 2.00 μm, equipped with an Hawaii H2RG IR
array from Teledyne, working at 40 K. The spectrograph will be cooled
down to about 150 K, to lower the thermal background, and equipped with a
thermal filter to block any thermal radiation above 2.0 μm. In this
poster we will show the main characteristics of the instrument along
with the expected performances at the telescope.
