Laboratory test of the VIS detector system of SOXS for the ESO-NTT telescope
: Cosentino Rosario, Hernandez Marcos, Ventura Hector, Campana Sergio, Claudi Riccardo, Schipani Pietro, Aliverti Matteo, Baruffolo Andrea, Ben-Ami Sagi, Biondi Federico, Capasso Giulio, D'Alessio Francesco, D'Avanzo Paolo, Hershko Ofir, Kuncarayakti Hanindyo, Landoni Marco, Munari Matteo, Pignata Giuliano, Rubin Adam, Scuderi Salvatore, Vitali Fabrizio, Young David, Achrén Jani, Araiza-Durán José Antonio, Arcavi Iair, Brucalassi Anna, Bruch Rachel, Cappellaro Enrico, Colapietro Mirko, Della Valle Massimo, De Pascale Marco, Di Benedetto Rosario, D'Orsi Sergio, Gal-Yam Avishay, Genoni Matteo, Kotilainen Jari, Li Causi Gianluca, Marty Laurent, Mattila Seppo, Rappaport Michael, Radhakrishnan Kalyan, Ricci Davide, Riva Marco, Salasnich Bernardo, Slemer Alessandra, Smartt Stephen, Sanchez Ricardo Zanmar, Stritzinger Maximilian
: Christopher J. Evans, Julia J. Bryant, Kentaro Motohara
: SPIE Astronomical Telescopes + Instrumentation
Publisher: SPIE-INT SOC OPTICAL ENGINEERING, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
: 2022
: Proceedings of SPIE : the International Society for Optical Engineering
: Proceedings of SPIE: Ground-based and Airborne Instrumentation for Astronomy IX
: GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY IX
: PROC SPIE
: 121845I
: Proceedings of SPIE : the International Society for Optical Engineering
: 12184
: 121845I
: 9
: 0277-786X
: 1996-756X
DOI: https://doi.org/10.1117/12.2628246
: https://doi.org/10.1117/12.2628246
SOXS is the new spectrograph for the ESO NTT telescope able to cover the optical and NIR bands thanks to two different arms: the UV-VIS (350-850 nm), and the NIR (800-2000 nm). In this article, we describe the final design of the visible camera cryostats, the test facilities for the CCD characterization, and the first results with the scientific detector. The UV-VIS detector system is based on a e2v CCD 44-82, a custom detector head coupled with the ESO Continuous Flowing Cryostat (CFC) cooling system and the New General Detector Controller (NGC) developed by ESO. The laboratory facility is based on an optical bench equipped with a Xenon lamp, filter wheels to select the wavelength, an integrating sphere, and a calibrated diode to measure the flux. This paper outlines the visible camera cryostat, the test facilities for the CCD characterization and the first results with the scientific detector in the laboratory and after the integration to the instrument.
