The Electronic Workshop
IASF-PA Electronic Workshop designs and develops
electronic equipments for astrophysical experiments. Other than his institutional
work with INAF, IASF-PA Electronic Workshop also collaborates with other Scientific
Institution to design specific electronic equipments (INFN, CNR, Physics Department
of Palermo University, Private Companies). IASF-PA Electronic Workshop designs electronic
apparatuses starting from specific requirements and uses the latest technology for
the ultimate scientific instruments development.
IASF-PA Electronic Workshop activity fully covers the experiment development
IASF-PA Electronic Workshop
activities is mainly related to design & development of:
- instruments manufacturing
- experimental set-up
arrangement for physical data measurements
- experiment management
using Host Computers
- Front-End for very fast
- high speed storage &
data acquisition systems
- high speed transmission
To reach the excellence
in the field of electronic design, IASF-PA Electronic Workshop uses the latest and
advanced techniques and a continuous effort is done to maintain the know-how up
to date following the state of the art in the field of:
- very fast & low
noise Front-End design
- microelectronic high
density PCB design (SMD components)
- high density and high
speed firmware design (FPGA)
- high speed transmission
interface design (std BUS like SATA, USB, ultra-SCSI )
- CAD development &
simulation design (OrCad, Pspice, Quartus, VHDL)
- software drivers development
& hardware management (.NET SDK Platform, C, Visual C++, C#, LabView)
Today IASF-PA Electronic
Workshop has know-how and technical resources to perform activities suitable for
new and manifold scientific investigation criteria.
Equipments for hardware development, test & measuring:
Computer Aided Design for electronic prototypes development & simulation:
Termo-Vacuum Chamber, -80°C ÷ +120°C, 1mBar, cm 50 x 50 x 50 useful space, Angelantoni
4 channels, 1.5 Ghz bandwith, 8 G/sample Digital Oscilloscope, Le Croy LC684D
4 channels, 0.5 Ghz bandwith, 2 G/sample Digital Oscilloscope, Tektronix TDS640A
1 G/sample Arbitrary Waveform Generator, Tektronix AWG510
Dual channels, 150 Mhz Pulse Generator, HP 8110A
225 Mhz Universal Counter, HP 53131A
Programmable Automatic RLC Meter, Philips PM6304
Synthesizer Function Generator, HP 3325A
EG&G Ortec model 439 Digital Current Integrator
Others NIM EG&G Ortec standard modules
Power Supply, several voltage & power range, HP series, Elind series
Pcs Windows platform
TFT Panasonic portable ruggized computer
Solder apparatus for Surface Mount Devices
Software for drivers development & hardware management:
.NET SDK Platform
C, Visual C++, C# (Sharp)
LabView, graphic development language for programming & testing
GAW, FOV Calculation.
Range of possible Field Of View investigation.
Simple Target SCSI core.
Board with Target SCSI core. Fast & safe data transfer between host and any
Enhanced Photon counting & Integrating Uv Detector.
2002. “ULTRA” Experiments.
UVScope detector for atmospherical and Cherenkov phenomena observation at see level.
A IFSI -Tourin, Grenoble Institut des Science Nucléaires & LIFE-Lisboa collaboration.
2001. Co-ordinate Project - Agency 2001: “CdTe Detector”.
CdTe & CdZnTe X ray detector ( Hard X ray and soft gamma ray, EDEX).
A TESRE-Bologna, Politecnico-Milan & Brera-Observatory collaboration.
2001. “GAW” (Gamma Air Watch) Cherenkov image Telescope.
High energy (>150 Gev) wide angle multianode photomultipliers array
1996-2001. “BA.BY.” (Background Bypass) Experiment.
Balloons Campaign Milo 1998, 1999, 2001.
300 - 400 nm band, UV background
1990-95. England. "PLASTEX", "STAR CLUSTER", "T&T" Experiments.
LST (Limited Streamer Tubes) & RPC (Resistive Plate Chambers) in a large Array
Detectors for EAS observation.
Leeds Physics’ Department and INFN-Naples collaboration.
1989. “HPGSPC”. SAX satellite Experiment.
"Dual Constant Fraction Timing" for HPGSPC detector. Burst Lenght
electronic discriminating X ray from Cosmic background, in 3÷120 Kev energy range.
1978-89. “FIGARO” Experiment. Balloons Campaign Milo 1982, 1986, Australia 1988.
Crab & Vela pulsars observation. cmq 3600 NaI(Tl) detector.
A CESR-Tolouse, CEN-Saclay, Rome Physics’ Department and IAS-Frascati collaboration.
1972-73. “Gamma 1.10 Mev”. Balloons Campaign Birgi 1972, Milo, 1973.
1-10 Mev". Gamma radiation observation, phenomena originated by Cherenkov effects.
A LFCTR-Milan collaboration
Last Modification: Friday, April 21 2017
Edit by Francesco Russo