A4 Vertaisarvioitu artikkeli konferenssijulkaisussa
The NIR spectrograph for the new SOXS instrument at the NTT
Tekijät: 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
Toimittaja: Christopher J. Evans, Luc Simard, Hideki Takami
Konferenssin vakiintunut nimi: SPIE Astronomical Telescopes + Instrumentation
Kustantaja: SPIE
Julkaisuvuosi: 2018
Journal: Proceedings of SPIE : the International Society for Optical Engineering
Kokoomateoksen nimi: Ground-based and Airborne Instrumentation for Astronomy VII
Tietokannassa oleva lehden nimi: Proceedings of SPIE - The International Society for Optical Engineering
Vuosikerta: 10702
Sivujen määrä: 13
ISBN: 978-1-5106-1957-9
ISSN: 0277-786X
DOI: https://doi.org/10.1117/12.2311466
Rinnakkaistallenteen osoite: 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.
