SOXS will be a unique spectroscopic facility 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 (800-1800 nm). In this article, we describe the
design of the visible camera cryostat and the architecture of the acquisition
system. The UV-VIS detector system is based on a e2v CCD 44-82, a custom
detector head coupled with the ESO continuous ow cryostats (CFC) cooling system
and the NGC CCD controller developed by ESO. This paper outlines the status of
the system and describes the design of the different parts that made up the
UV-VIS arm and is accompanied by a series of contributions describing the SOXS
design solutions.Comment: 9 pages, 13 figures, to be published in SPIE Proceedings 1070

Achrén, Jani

Aliverti, Matteo

Araiza-durán, José Antonio

Arcavi, Iair

Baruffolo, Andrea

Ben-ami, Sagi

Bianco, Andrea

Biondi, Federico

Brucalassi, Anna

Campana, Sergio

Capasso, Giulio

Cappellaro, Enrico

Claudi, Riccardo U.

Colapietro, Mirko

Cosentino, Rosario

D'alessio, Francesco

D'avanzo, Paolo

D'orsi, Sergio

Della Valle, Massimo

Diner, Oz

Evans, Christopher J.

Fantinel, Daniela

Fynbo, Johan

Gal-yam, Avishay

Genoni, Matteo

Hirvonen, Mika

Ives, Derek

Kotilainen, Jari

Kumar, Tarun

Kuncarayakti, Hanindyo

Landoni, Marco

Lehti, Jussi

Li Causi, Gianluca

Marafatto, Luca

Mattila, Seppo

Mehrgan, Leander H.

Munari, Matteo

Pariani, Giorgio

Pignata, Giuliano

Rappaport, Michael

Ricci, Davide

Riva, Marco

Rubin, Adam

Salasnich, Bernardo

Schipani, Pietro

Scuderi, Salvatore

Simard, Luc

Smartt, Stephen

Takami, Hideki

Turatto, Massimo

Vitali, Fabrizio

Zánmar Sánchez, Ricardo

English

arXiv

Schipani

Aliverti

Biondi

Brucalassi

Capasso

Claudi

Zanmar Sánchez

Ricci

Rubin

Vitali

Leander

Crossref

The VIS detector system of SOXS

SOXS will be a unique spectroscopic facility 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 (800-1800 nm). In this article, we describe the design of the visible camera cryostat and the architecture of the acquisition system. The UV-VIS detector system is based on a e2v CCD 44-82, a custom detector head coupled with the ESO continuous flow cryostats (CFC) cooling system and the NGC CCD controller developed by ESO. This paper outlines the status of the system and describes the design of the different parts that made up the UV-VIS arm and is accompanied by a series of contributions describing the SOXS design solutions (Ref. 1-12)

COSENTINO, Rosario

SCUDERI, Salvatore

CAMPANA, Sergio

CLAUDI, Riccardo

SCHIPANI, Pietro

BARUFFOLO, Andrea

Ben-Ami, Sagi

Mehrgan, L. H.

BIONDI, FEDERICO

BRUCALASSI, ANNA

CAPASSO, Giulio

D'ALESSIO, Francesco

D'AVANZO, Paolo

MUNARI, MATTEO

VITALI, Fabrizio

Araiza-Durán, José Antonio

BIANCO, ANDREA

CAPPELLARO, Enrico

COLAPIETRO, MIRKO

DELLA VALLE, Massimo

D'ORSI, SERGIO

FANTINEL, Daniela

Gal-Yam, Avishay

LANDONI, Marco

LI CAUSI, Gianluca

MARAFATTO, Luca

PARIANI, Giorgio

RICCI, DAVIDE

RIVA, Marco

SALASNICH, Bernardo

SANCHEZ CASTELAN, Ricardo Zanmar

TURATTO, Massimo

OA@INAF - Istituto Nazionale di Astrofisica

2018Publication Year2021-04-22T11:33:27ZAcceptance in OA@INAFThe VIS detector system of SOXSTitleCOSENTINO, Rosario; Aliverti, Matteo; SCUDERI, Salvatore; CAMPANA, Sergio; CLAUDI, Riccardo; et al.Authors10.1117/12.2312539DOIhttp://hdl.handle.net/20.500.12386/30852HandlePROCEEDINGS OF SPIESeries10702NumberPROCEEDINGS OF SPIESPIEDigitalLibrary.org/conference-proceedings-of-spieThe VIS detector system of SOXSCosentino, Rosario, Aliverti, Matteo, Scuderi, Salvatore,Campana, Sergio, Claudi, Riccardo, et al.Rosario Cosentino, Matteo Aliverti, Salvatore Scuderi, Sergio Campana, RiccardoClaudi, Pietro Schipani, Andrea Baruffolo, Sagi Ben-Ami, L. H. Mehrgan, Derek  Ives,Federico Biondi, Anna Brucalassi, Giulio Capasso, Francesco D'Alessio, PaoloD'Avanzo, Oz Diner, Hanindyo Kuncarayakti, Matteo Munari, Adam Rubin, FabrizioVitali, Jani Achrén, José Antonio  Araiza-Durán, Iair Arcavi, Andrea Bianco, EnricoCappellaro, Mirko Colapietro, Massimo Della Valle, Sergio D'Orsi, Daniela Fantinel,Johan Fynbo, Avishay Gal-Yam, Matteo Genoni, Mika Hirvonen, Jari Kotilainen,Tarun Kumar, Marco Landoni, Jussi Lehti, Gianluca Li Causi, Luca Marafatto, SeppoMattila, Giorgio Pariani, Giuliano Pignata, Michael Rappaport, Davide Ricci, MarcoRiva, Bernardo Salasnich, R. Zanmar Sanchez, Stephen Smartt, Massimo Turatto,"The VIS detector system of SOXS," Proc. SPIE 10702, Ground-based and AirborneInstrumentation for Astronomy VII, 107022J (6 July 2018); doi: 10.1117/12.2312539Event: SPIE Astronomical Telescopes + Instrumentation, 2018, Austin, Texas, UnitedStatesDownloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 21 Apr 2021  Terms of Use: https://www.spiedigitallibrary.org/terms-of-useThe VIS detector system of SOXSRosario Cosentinoa,c, Matteo Alivertib, Salvatore Scuderic, Sergio Campanab, RiccardoClaudid, Pietro Schipanie, Andrea Baruffolod, Sagi Ben-Amii,f, L. H. Mehrgang, Derek Ivesg,Federico Biondid, Anna Brucalassig,m, Giulio Capassoe, Francesco D’Alessioh, PaoloD’Avanzob, Oz Dineri, Hanindyo Kuncarayaktis,u, Matteo Munaric, Adam Rubini, FabrizioVitalih, Jani Achrénl, José Antonio Araiza-Duranm, Iair Arcavin, Andrea Biancob, EnricoCappellarod, Mirko Colapietroe, Massimo Della Vallee, Sergio D’Orsie, Daniela Fantineld,Johan Fynboo, Avishay Gal-Yamp, Matteo Genonib, Mika Hirvonenq, Jari Kotilainens,u, TarunKumarr, Marco Landonib, Jussi Lehtiq, Gianluca Li Causis, Luca Marafattod, Seppo Mattilaj,Giorgio Parianib, Giuliano Pignatam, k, Michael Rappaporti, Davide Riccid, Marco Rivab,Bernardo Salasnichd, R. Zanmar Sanchezc, Stephen Smarttt, and Massimo Turattoda INAF – Fundación Galileo Galilei, – Breña Baja, SpainbINAF - Osservatorio Astronomico di Brera, Merate, ItalycINAF - Osservatorio Astrofisico di Catania, Catania, ItalydINAF - Osservatorio Astronomico di Padova, Padua, ItalyeINAF - Osservatorio Astronomico di Capodimonte, Naples, ItalyfHarvard-Smithsonian Center for Astrophysics, Cambridge, USAgESO - European Southern Observatory, Garching, GermanyhINAF - Osservatorio Astronomico di Roma, Rome, ItalyiWeizmann Institute of Science, Rehovot, IsraeljUniversity of Turku, Turku, FinlandlIncident Angle Oy, Turku, FinlandkMillennium Institute of Astrophysics (MAS), Santiago, ChilemUniversidad Andres Bello, Santiago, ChilenTel Aviv University, Tel Aviv, IsraeloDark Cosmology Centre, Copenhagen, DenmarkpWeizmann Institute of Science, Rehovot, IsraelqASRO - Aboa Space Research Oy, Turku, FinlandrUniversity of Turku, Turku, FinlandsINAF - Istituto di Astrofisica e Planetologia Spaziali, Rome, ItalytQueen’s University Belfast, Belfast, UKuFINCA - Finnish Centre for Astronomy with ESO, Turku, FinlandABSTRACTSOXS will be a unique spectroscopic facility for the ESO NTT telescope able to cover the optical and NIR bandsthanks to two different arms: the UV-VIS (350-850 nm), and the NIR (800-1800 nm). In this article, we describethe design of the visible camera cryostat and the architecture of the acquisition system. The UV-VIS detectorsystem is based on a e2v CCD 44-82, a custom detector head coupled with the ESO continuous flow cryostats(CFC) cooling system and the NGC CCD controller developed by ESO. This paper outlines the status of thesystem and describes the design of the different parts that made up the UV-VIS arm and is accompanied by aseries of contributions describing the SOXS design solutions (Ref. 1–12).∗Keywords: spectrograph, VIS, detector∗Author: cosentino@tng.iac.esGround-based and Airborne Instrumentation for Astronomy VII, edited by Christopher J. Evans, Luc Simard, Hideki Takami, Proc. of SPIE Vol. 10702, 107022J · © 2018 SPIE · CCC code: 0277-786X/18/$18 · doi: 10.1117/12.2312539Proc. of SPIE Vol. 10702  107022J-1Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 21 Apr 2021Terms of Use: https://www.spiedigitallibrary.org/terms-of-use1.000.900.800.70F 0.60LL, 0.50cr 0.400.300.200.100.00250Typical spectral responsedeep depletion, basic -100Cmai '̀EIN7i% - Near-IR alMidband MEWMIA MIMI\/. -Broadband Mil L.\\..Uncoated350 450 550 650 750 850 950 1050nm1. THE DETECTOR SYSTEMThe UV-VIS CCD Detector System for SOXS is designed to reach a wavelength response from 350 to 850 nmand consists of the following sub-systems:1. e2v CCD44-82 2K x 4K CCD2. CFC cooling system3. detector head4. CCD controller unit and power supply to operate the CCD detector head, with cable set to connect them5. shutter6. commercial shutter control unit with cable set7. temperature controller with cable set1.1 VIS DetectorThe detector chosen for the SOXS UV-VIS arm is an e2v CCD44-82. This detector is a high performance, backilluminated CCD with a 15.0 µm square pixel and an image area of 30.7x61.4 mm and is characterized by ahigh Quantum Efficiency (QE). In figure 1 is shown the QE of this detector for different coatings. This detectortechnology was chosen for the following reasons:1. devices manufactured with this technology meet or exceed the requirements2. INAF has experience with devices with this technology and it is considered to be of low riskFigure 1. QE vs. wavelength for different coatings as provided by themanufacturer. The selected CCD is the midband, the purple points areour specific CCD QE data, taken from the e2v technical noteFigure 2. CCD44-82 back-illuminated CCD sensorProc. of SPIE Vol. 10702  107022J-2Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 21 Apr 2021Terms of Use: https://www.spiedigitallibrary.org/terms-of-useTable 1. CCD main characteristics.Detector CCD44-82Chip type Thinned back illuminatedPixel size 15 µmArea (pixels) 2048 x 4096Area (mm) 30.7 x 61.4QE at 500 nm 90%Coating yesFlatness Better than 20 µm peak to valleyPeak signal 200 ke-/pixelCTE Serial OSL 99.9993%CTE Serial OSR 99.9999%CTE Parallel 99.9998%1.2 The camera housingThe detector head and wiring are based on the heritage of existing instruments at ESO. The head is coupled witha Continuous Flow Cryostat (CFC) cooling system , successfully adopted in several ESO projects. The UV-VIScamera is made up by the ESO CFC cooling system coupled through a bellows with the custom detector headthat allows its placement into the UV-VIS arm of the spectrograph figure 3. Due to the reduced space availablein the spectrograph, the front part of the camera, where the light will be incoming, has a special rectangulardesign called ’nose’.Figure 3. Drawing of the VIS detector system1.3 Detector head and wiringThe detector wiring, i.e. the baseplate and flex circuits, will provide the components to safely mount the CCDand to conduct signals from the CCDs to the external wall of the cryostat. It also provides the mounting andwiring for the temperature sensors and heater that stabilize the detector temperature and monitor cryostatperformance. The detector wiring will place minimal heat load on the cooling system. It should not introducenoticeable crosstalk or readout noise, and it should also be flexible enough to accommodate shrinkage duringcooling down. It should not add appreciably to the outgassing and should use as much as possible previouslytested cryogenic compatible materials and components. In the design and choice of fabrication materials andtechniques for the detector head wiring, the following rules have been followed:Proc. of SPIE Vol. 10702  107022J-3Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 21 Apr 2021Terms of Use: https://www.spiedigitallibrary.org/terms-of-use• the preamplifiers are directly attached to the cryostat or very close to it• the clocks-filters and wave-shaping (passive components) are placed in a shielded box attached to thecryostat• clock, bias, output, and temperature signal groups are kept separate, with ground shields in between• the thermal load of wiring on cryogenic cooling is kept as low as possible1.4 CCD controller unitThe detector controller provides the biases and the correct sequences of clocks and analog video processing todrive and acquire the images of the CCDs. The dead time is defined as the interval between the end of oneexposure (closed shutter) to the start of the next one (open shutter) and it obviously includes the read time andalso other software overheads, e.g. for data storage and shutter control. The CCD controller will be the NGC(New General detector Controller) system. This controller, designed by ESO to replace the former FIERA andIRACE devices, is a single multipurpose controller able to manage both CCDs and IR arrays.The NGC is thecurrent controller for ESO instrumentation and it will be adopted in SOXS project as well to comply with ESOstandards and to reduce any compatibility failure with ESO hardware and software systems. The NGC is basedon newest hardware standard (FPGA), it has the same hardware core for both optical and IR controllers and,in addition, is full compatible with ESO software and it includes all the good features of previous systems.The NGC consists of five major components:• Data Acquisition Computer with integrated PCI interface (DAQC)• Detector Front-End (DFE)• Detector Cryostat Cables (DCC)• Detector Front-end Power Supply (DFPS)• Detector Preamplifier (DPA)The main NGC features are:• high speed link• the core element on each board is a Xilinx FPGA• digital parts and the sequencer are implemented in the FPGA• compact system• full compatibility with ESO software standardThe controller has to be located near the detector, because the maximum cable length must be 2 m.The control system is composed by:1. LLCU, which is a Linux machine (DELL or an industrial PC)2. PCI-Express card3. front-end box (preamplifier)4. power supply, including the cable to the NGC5. two NGC modules for operations with CCD detectors6. fiber interfaces, including fiber cable7. CCD temperature control8. shutter driverProc. of SPIE Vol. 10702  107022J-4Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 21 Apr 2021Terms of Use: https://www.spiedigitallibrary.org/terms-of-usePCI boardFront -end canbe attached to instrumentstructure for passive coolingFront -end electronicsUp to 6 boardsPovner supply(remote)Figure 4. The NGCwater-cooled housingFigure 5. The NGC Two-Slot system housingThe NGC system has three possible housings: compact, fan-less and water-cooling. The housing is selectedaccording to the setup where the controller is located. In SOXS we need to locate the controller close to theinstrument because the cable between the cryostat and the device must be shorter than 2 m. Therefore, weselected the water-cooled housing to prevent any thermal dissipation into the telescope Nasmyth room.The power supply for the NGC device is a 19-inch 3HE rack-mountable unit, which may be at a distancefrom the detector Front End (DFE) of up to 12 meters (see figure 9).Figure 6. The ESO New Generation Controller functional diagram.1.4.1 PCI interface Board (DAQC)An ESO custom-made PCI64 board (figure 7) with a fiber-optic connection to the Front End is installed in theData Acquisition Computer (DACQ). The maximum theoretical bandwidth per interface is 256MB/s, whichmatches the 2.5 GBit/s fiber transmission rate. The bandwidth for actual data transmission is about 20% lower.Proc. of SPIE Vol. 10702  107022J-5Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 21 Apr 2021Terms of Use: https://www.spiedigitallibrary.org/terms-of-userr- -, - -. 0000Ó 4s{`'°s7 1+35' rl E¡. ai'Àitï6fÏi1iI r`¡.¡ iy ri i¡r- r xSl -i f ', .+i.:. ` ' rji!(r+ h-^' ar-!R'a''..!e 'r7 . .Ir < rr .. '. .< o , is+.<' rtFigure 7. The PCIe interface board.1.4.2 Detector front-end (DFE)The DFE has to be located close to or on the instrument (maximum detector cable length 2m; depending on theapplication, an extension up to 3m may be possible). The module, from which the VIS NGC DFE can be built,is one Basic Board that contains four video channels and clock/bias generation. In order to prevent damage fromoverheating, all housings should be equipped with a thermal sensor that can shut off the power to the NGC box.Figure 8. NGC system with Basic Board, Backplane and Transition Board (VIS arm).1.4.3 Detector Cryostat Cables (DCC)The Detector Cryostat Cable is the connection between the DFE and the VIS camera (figure 6). It contains theclock and bias lines and the video signals. The maximum length depends on application (2-3 m).Proc. of SPIE Vol. 10702  107022J-6Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 21 Apr 2021Terms of Use: https://www.spiedigitallibrary.org/terms-of-use$II!...LAIVIáI1.4.4 Detector Front-end Power Supply (DFPS)The power supply for the DFE is a 19-inch 3HE rack-mountable unit which may be at a distance from the DFEof up to 12 meters.Figure 9. Power supply (front view).1.4.5 Detector Preamplifier (DPA)The CCD preamplifier is placed between the cryostat and the DFE. The location of the Detector Preamplifier isapplication dependent; in the SOXS case of an optical detector the preamplifier is located outside the cryostat.It features 4 video channels with 16 software-selectable gains and 8 software-selectable bandwidths per channel.Its outer dimensions are 100 x 120 x 40 mm3. The preamp is show in figure 10.Figure 10. Detector Preamplifier (DPA).1.5 Shutter controlThe shutter is driven by the NGC through its own commercial controller; it is upstream from the detector unit,at the entrance slit of the spectrograph (figure 11), which allows us to use a small shutter aperture. The selectedmodel is an Uniblitz ES6B with its VED24 controller. (figure 12).Features:• 6 mm aperture• bi-stable operation• extremely low-profile form-factor• RoHS compliant• transfer time on opening: 1.9 milliseconds• total opening time: 3.7 milliseconds• can be configured for the VED24 shutter driverProc. of SPIE Vol. 10702  107022J-7Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 21 Apr 2021Terms of Use: https://www.spiedigitallibrary.org/terms-of-useFigure 11. The entrance slit ofthe spectrograph and the UV-VIS shutter.Figure 12. Shutter Uniblitz ES6B and controller VED241.6 Temperature controllerFor the CCD temperature control two options can be take into account:• The CCD controller integrated control• A commercial temperature controller (i.e. Lakeshore 336.)The characteristics of the Lakeshore 336 are summarized in the following list:• operates down to 300 mK with appropriate NTC RTD sensors.• four sensor inputs and four independent control outputs• two PID control loops: 100 W and 50 W into a 50 Ω or 25 Ω load• auto-tuning automatically determines PID parameters• automatically switch sensor inputs using zones to allow continuous measurement and control from 300 mKto 1505 K• custom display set-up allows you to label each sensor input• Ethernet, USB, and IEEE-488 interfaces• supports diode, RTD, and thermocouple temperature sensors• sensor excitation current reversal eliminates thermal EMF errors for resistance sensors• ±10 V analog voltage output, alarms, and relaysProc. of SPIE Vol. 10702  107022J-8Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 21 Apr 2021Terms of Use: https://www.spiedigitallibrary.org/terms-of-useLake ShoreN: Sanrlo <c5. 26 14 K F.AU 5.2000 K 3T. . C 0000 l' 0%:c.4.6103 K 35.ó387:" 0.0009 K O< <n- 0.000C K e<Model 336'8'perar,re Amtronw5- Cif ITO< k.9SETPOWT (.77lP° l'1"Figure 13. Temperature controller Lakeshore 336.2. CONCLUSIONSThe VIS-UV detector system is part of the VIS arm of the SOXS spectrograph that will be installed at the ESONTT telescope located at La Silla observatory. The project is going to conclude the final design phase in 2018.Afterward, the plan is to integrate the instrument in Italy and then have the first light within 2020.REFERENCES[1] Schipani, P. et al., “The new SOXS instrument for the ESO NTT,” in [Proc. SPIE 9908, 990841 ], (2016).[2] Aliverti, M. et al., “The mechanical design of SOXS for the NTT,” in [Proc. SPIE 10702 ], (2018).[3] Biondi, F. et al., “The assembly integration and test activities for the new SOXS instrument at NTT,” in[Proc. SPIE 10702 ], (2018).[4] Brucalassi, A. et al., “The acquisition camera system for SOXS at NTT,” in [Proc. SPIE 10702 ], (2018).[5] Capasso, G. et al., “SOXS control electronics design,” in [Proc. SPIE 10702 ], (2018).[6] Claudi, R. et al., “The common path of SOXS (Son Of X-Shooter),” in [Proc. SPIE 10702 ], (2018).[7] Zanmar Sánchez, R. et al., “Optical design of the SOXS spectrograph for ESO NTT,” in [Proc. SPIE 10702 ],(2018).[8] Schipani, P. et al., “SOXS: a wide band spectrograph to follow up the transients,” in [Proc. SPIE 10702 ],(2018).[9] Ricci, D. et al., “Architecture of the SOXS instrument control software,” in [Proc. SPIE 10702 ], (2018).[10] Rubin, A. et al., “MITS: the multi-imaging the transient spectrograph for SOXS,” in [Proc. SPIE 10702 ],(2018).[11] Vitali, F. et al., “The NIR spectrograph for the new soxs instrument at the ESO-NTT,” in [Proc. SPIE10702 ], (2018).[12] Leander, M. et al., “State-of-the-art detector controller for eso instruments,” in [SDW 2013 Florence ],(2013).Proc. of SPIE Vol. 10702  107022J-9Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 21 Apr 2021Terms of Use: https://www.spiedigitallibrary.org/terms-of-use

Copenhagen University Research Information System

https://openaccess.inaf.it/bitstream/20.500.12386/30852/1/107022J.pdf

The VIS detector system of SOXS

Abstract

Similar works

Full text

Available Versions

Crossref

OA@INAF - Istituto Nazionale di Astrofisica

Copenhagen University Research Information System