AMICA Antarctic Multiband Infrared CAmera Favio Bortoletto INAF – Osservatorio Astronomico di Padova on behalf of the AMICA collaboration Telescope and Instrument Robotization at Dome C Puerto Santiago, Tenerife, March 26-29, 2007

AMICA People L. Corcione, F. Porcu F.M. Zerbi, A. Riva, V. De Caprio, E. Molinari, P. Conconi F. Bortoletto, C. Bonoli, M. D’Alessandro, E. Giro, D. Fantinel, D. Magrin O. Straniero (PI), M. Dolci (PM), G. Valentini, C. Giuliani, A. Di Cianno, G. Di Rico, M. Ragni, D. Pelusi, A. Valentini

The Camera in Summary Near- and mid-infrared photometry (2 – 5.5  m and 7 – 28  m) Two independent channels Remotely operated To be mounted at the f / IRAIT Nasmyth focus Telescope and Instrument Robotization at Dome C Puerto Santiago, Tenerife, March 26-29, 2007 Standard broadband plus narrow band filter set

AMICA Optical Layout: Medium IR Channel  from the telescope FM PM1 Cold Stop and filters position PM2 Si:As BIB 128x128 8K Scale Reduction : to “/mm

AMICA Optical Layout: Near IR Channel  from the telescope FM PM1 Cold Stop and filters position PM2 TM InSb 256x K Scale Reduction : to “/mm

Detectors: 7 – 28  m 2 – 5.5  m Telescope and Instrument Robotization at Dome C Puerto Santiago, Tenerife, March 26-29, 2007 Si:As BIB MF-128 by DRS Technologies, Inc. Field Coverage: 2.86 arcmin Scale: 1.34”/pix 128  128 format 75  m pitch T op  4 – 10 K 8 K > 60 % Well capacity = 9.1  10 6 e Hz frame rate = 282 e - r.m.s. 8 K = 3.5 e - / sec / pixel Maximum frame rate: 500 Hz 256  256 format 30  m pitch T op  25 – 35 K 35 K > 80 % Well Capacity  2  10 5 e - RON  50 e - r.m.s. (typical) 35 K < 3 e - / sec /pixel 4 outputs InSb array by Raytheon Corp. Field Coverage: 2.29 arcmin Scale: 0.54 “/pixel

AMICA the Cryostat Telescope and Instrument Robotization at Dome C Puerto Santiago, Tenerife, March 26-29, 2007

Telescope and Instrument Robotization at Dome C Puerto Santiago, Tenerife, March 26-29, 2007 The AMICA Control System: Sytem supervision is assured by a PLC interfaced to the CPCI host : - vacuum system - dual-stage cryocooler - instrument temperature monitoring - racks temperature monitoring - cryogenic step- motors control

Telescope and Instrument Robotization at Dome C Puerto Santiago, Tenerife, March 26-29, 2007 The AMICA Control System: CPCI Computer The AMICA detector control electronics is built on a CPCI-Pentium host with a SKYTECH PMC array- control I/F. The PMC array controller drives via a dedicated fiber-link the analog unit providing detector biasing, clocking and video signal processing. Secondary chopper drive and monitoring can be done by the detector controller sequencer or, off line, by a CPCI process.

Telescope and Instrument Robotization at Dome C Puerto Santiago, Tenerife, March 26-29, 2007 MIR simulation box NIR simulation box Detector controller The AMICA Control System: Detector Controller 1.2 Gbaud Fiber Link

AMICA System Operation : The AMICA detector-controller commanding will be possible from three different sources : Telescope and Instrument Robotization at Dome C Puerto Santiago, Tenerife, March 26-29, 2007 “Local unit” (CPCI Camera Driver, Test) “Remote UIF” (Test, Commissioning) - Build camera commands - Build readout waveforms - Configure detector tables - Retrieve telemetry - Retrieve data - Quick look check - Archive data “Remote Command Flow”

Telescope and Instrument Robotization at Dome C Puerto Santiago, Tenerife, March 26-29, 2007 Commanding, camera configuration and data exchange is based on files. So the test operator interface can reside with simple files redirection on every networked computer. Command and Data exchange :

The remote test Interface with the acquisition software is based on the IDL-atv standard interface Boot MIR Load bias table Load clock table Read Telemetry Boot……OK Bias table….loaded Clock table….loaded Telemetry….. The AMICA Test Interface :

Telescope and Instrument Robotization at Dome C Puerto Santiago, Tenerife, March 26-29, 2007 Telemetry retrieval :

Image data files are stacked in core memory buffers: object and sky for chopper assisted observations. Frames are then summed up following the selected readout mode (single, multiple sampl. Etc.) to build the final image accumulators. Images (buffers and/or accumulators) are retrieved by the remote UIF via Ethernet for quick-look analysis and archiving. Telescope and Instrument Robotization at Dome C Puerto Santiago, Tenerife, March 26-29, 2007 Scientific Data Organization: