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Technologies for microsatellites. Roberto Battiston Università and INFN Perugia. LNF March 22 nd 2006. Space is an opportunity to change system of reference……. Leonides storm seen from space Fe, 1 mm 3 , 40 km/s , E = 0.5 J 1 proton, E= 10 20 ev = 16 J. - PowerPoint PPT Presentation
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Roberto BattistonUniversità and INFN Perugia
LNF March 22nd 2006
Technologies for microsatellites
Space is an opportunity to change system of reference…….
Leonides storm seen from spaceFe, 1 mm3 , 40 km/s , E = 0.5 J1 proton, E= 1020 ev = 16 J
Credits to P. Jenniskens (NASA/Ames, SETI Inst.)
……to see things from another perspective
Half a centuryafter the Sputnik and
the discovery of Van Allen Belts, space is fully maintain its
unique potential for discovery and surprises
THE ROUTE OF “INCREASED ACCURACY”
The sensitivity of the instrumentation and the technologies Have improved dramatically
The more we understand about the Cosmos the more we are challenged to build sophisticated instruments, to match the sensitivity scale set by the physics of the Universe at different Time and Space scales.
Very complex instruments have been deployed and even more sophisticated one are scheduled or dreamed
Edwin P. HubbleMount Wilson Mount Palomar
Hubble (1929) HST (1999)
km/s/Mpc5000 H km/s/Mpc700 H
Dominated by systematic errors! 10.z
NASA Beyond Einstein Program
Not only large facilities, however, have a discovery potential, like in
today HEP at accelerators
Clever, small experiments, using new or “first time used in space” technologies
continues to give rise to fantastic surprises like at the time of Van Allen
THE ROUTE OF “GETTING THERE FIRST”
Further progress o tog rr ysa a !
COSMIC RAYS
Baby EUSO
MULTIANODEPHOTOMULTIPLIER TUBE ASSEMBLYH7546
MEGSAT 1 e 2
CONTROLLER
COMUNICATION AND POWER INTERFACE
FRONT END
HIGH VOLTAGE POWER
SUPPLIES
AURORA CH.
BACKGROUND CH.
CONNECTION BOARD
405
325
330
AURORA ON MEGSAT-2
A. Monfardini1,2, R. Stalio1,2, P. Trampus2, R. Battiston3,4,
M. Menichelli4 , N.Mahne2, P. Mazzinghi5
1 University of Trieste; 2 Carso, Area Science Park, Trieste,
3 University of Perugia, 4 INFN, Perugia, 5 INOA, Firenze
Silicon PM
Fotografia di un wafer
Fotografia di un SiPM
Functional measurement set-up (1)
Preamplifier board: received from Pisa two stage preamplifier based on THRS4303 chip (high bandwidth: 1.8 GHz, fixed gain: 10 V/V) overall gain: theoretical 10x10x2/5 = 40, measured 42
Preamplifier
SiPM
Blue light LED (470 nm)
Faraday box
50
SiPM Signal Current pulse
IN
SiPM SignalVoltage pulse
THRS4303x10
THRS4303x10
150
100
50 OUT
SiPM amplified voltage pulse
Bias 33V (2V overvoltage)
One pixel dark count signals
Two pixels dark count signals
A1
A2= 2A1
Bias 34V (3V overvoltage)
One pixel dark count signals
A1’ > A1
A2’ = 2A1
’
Two pixels dark count signals
Dark count signals
Threshold(see next slide)
Recovery time: ~ 20ns
Rise time: ~ 1ns
1.E+02
1.E+03
1.E+04
1.E+05
1.E+06
1.E+07
0 50 100 150 200 250 300 350
threshold (mV)
dar
k ra
te (
Hz)
32 V
32.5 V 33 V
33.5 V 34 V
34.5 V 35 V
36 V
T = 23°C, Vbreakdown = 31 V
Dark count ratePlateau of one pixel dark count signals
Plateau of two pixels dark count signals
Single pixels dark count rate: our SiPMs: 5 MHz (5V overvoltage, T=23°C) Russian SiPMs: 2 MHz (5V overvoltage)
Russian SiPM from CPTAVbreakdown = 47 V
Gain
SiPM gain: linear variable with overvoltage in the range 5x105 2x106
Histogram of the signals area
Markers delimitating the integration zone of the signal
0.0E+00
5.0E+05
1.0E+06
1.5E+06
2.0E+06
2.5E+06
3.0E+06
0 1 2 3 4 5 6
Overvoltage [Vbias - Vbreakdown] (V)
On
e p
ixel
gai
n
gain - single pick area
Lineare (gain - single pick area)
Vbreakdown = 31V
Two pixels dark count signals
One pixeldark count signals
SiPM signals under pulsed lightVery preliminary and qualitatively results
BLUE pulsed light (470 nm)
SiPM sensible to the blue light
Dark count signals
Pisa measurements Very good resolution of single photoelectrons
Trigger
SiPM signal
RED pulsed light
N. Dinu (Irst)
DaSipm Bologna Group
As we have done for the PMT, we developed a Montecarlo model that allows us to simulate the SiPM behaviour. Even if the model is phenomenological and not physical the results reproduced the real mesuraments.These means that the SiPM behaviour is quite understood at least in his main characteristics.
G. Levi et al.
DaSipm Bologna Group
Scintillator
SiPMs + FE
future TOF counter
Beeing unsensible to magnetic field, SiPMs do not need light guides.Scintillators will be read through WLS fibers directly coupled to the SiPM.A first evaluation of weight saving is around 50-60kg, considering only the light guide and PMT.Lighter and simpler supporting structure and low voltage power supplies will increase this figures.
Light guide + PMT = 25 cm SiPM + FE = 2.5 cm
MEMS Space Telescope for UHECR Study
(MEMSTEL)
IL H. PARK (Ewha W. University, Seoul)
Research Center for MEMS Space Telescope
funded by Ministry of Science and Technology in Mar. 2006
Principle of MEMS Tracking Telescope
•Archimedes Mirror : Mirror Segments, Soldiers Operation
•Park’s Mirror : Micromirrors, VLSI Control
•Aberration free focusing & Wide FOV•Tracking capability
VLSI Micromirror
Photodetector
ObjectAir Shower
Micromirror & Circuits
Photodetctor
Prestudy 1-axis Analog Micromirror Design, Fabrication, Test
Electrostatic Comb-drive Actuator
Specification• 1-axis • Max angle: 4 degrees
at 100V • Frequency: > 5 kHz • Cell size: 372 x 970
um2 • Micromirror size : 372
x 150 x 30 um3 • Comb size: 260 x 6 x
30 um3 • Torsion spring size :
120 x 3.5 x 30 um3
Design
Fab Test
Prestudy 2-axis Micromirror Fab. Simulation
Hidden comb drive actuator (1-axis at present, 2-axis under way)
2-axis Side comb drive actuator
Prestudy MEMS Tracking Simulation
Fresnel mirror
Incident angle = 20o
MEMS mirror
Incident angle = 20o
Micromirrorarray
Detector plane
Mirrorplane
Fresnel mirror
Incident angle = 0o
Analog Board
Digital Board
PMT or SiPM (1296 ch)
PMT Power Supply
NIR Detector
NIR Electronics
Micromirror Array
MEMS Telescope Payload Design
MEMSTEL ParametersMEMSTEL Payload parameters
Orbit height 400 km
Mirror diameter 1 m
Focal distance0.34 ~ 0.8 m
(variable)
No. of Photodetector Ch
1296
FOV 40 ~ 70o (variable)
Field resolution10 - 2.5 - 0.6 km
(variable)
Trigger latency 3 ~ 10 usec
Aperture 85,000 ~ 300,000
km2
Payload weight 20 kg
Power 20 Watt
Micromirror Parameters
Power/cell < 0.1 μA
tilting angle5 ~ 10 degree
angle resolution
0.1 degree
Cell size
100x100 μm2 ~ 1000x1000 μm2
Rotation x, y axis
Fill factor 95 %
cost (for 4"wafer)
$1000
High Energy Quantum Optics: Compton Gamma Detectors
A stack of Si/CdTe strips/pixels
in a BGO well (10,000 ch)
Takahashi et al.SPIE 2003
Micro-particle detector
What’s next in the “NeXT” mission
Narrow FOV Compton Telescope(100 keV- 1 MeV)
• Extremely Low Background( High S/B ratio)• Capability of the polarization measurement
E1
E2
Quantum optics
Photoelectric effect and polarization (R. Bellazzini)
4
222
4
5
2
cos1
24
137cossin2
7
h
mcZro
The photoelectric effect is very sensitive to photon polarization
2cos
Projecting on the plane orthogonal to the
propagation direction…
8-layer PCB fan out to front end hybrid
Angle and amount of polarization is computed from the angular distribution of the photoelectron tracks
GEM: provides gas amplification and fast trigger
The detector
Readout plane: 512 pixels, 260 um pitch, 2.4 x 2.4 mm2 active area
The new detector!
• 2101 pixels (80 um pitch) comprehensive of preamplifier/shaper, S/H and routing (serial readout)• 200 electrons ENC• External trigger for parallel S/H on all channels• 200 us for complete readout• 100 uW/channel power consumption
Full custom ASIC (CMOS technology) directly used as a multi pixels readout electrode.
Reconstruction algorithms, data analysis
New reconstruction algorithms now under study:• Exploit higher moments of reconstructed charge distribution• Improve imaging capabilities• Enhance accuracy in angular reconstruction• Study the effect of cuts on polarimetric sensitivity.
GRAVITATION
A gravitationally Hyper sensitive experiment !
HYPER
Bose Enstein condensates
Interferometry: 109 atoms an unique wave function
Space Time fluctuation:getting to the Plank scale
by cold atoms interferometry
HYPER - precision cold atom interferometry in space
NEW HIGHLIGHTS IN ATOM OPTICSPARIS2001/2
1st BEC ON A CHIP
Highest gradients with minimum Currents
= Lower Magnetic Fields (Metrology)
= Lower Power (Transportable Microsensors)
Simpler Production
FUTURE EFFORTS
APPLYING THESE TECHNIQUES FOR FUNDAMENTAL PROBLEMS IN METROLOGY
Who can build a cheap micro/nano satellite ?
Universtities + Research Centers +Small Hightech industries
Best example: University of Surrey (UK)
Most impressive example : China DhF CAST
• PHD TOPICS WITHIN SSC • SMALL SATELLITE SAR • CHIPSAT • FORMATION FLYING . • COST-EFFECTIVE NAVIGATION AND RANGING FOR LUNAR AND INNER
PLANETS MISSIONS • IR SENSORS • HYPERSPECTRAL IMAGERY • SATELLITE AUTONOMY • MULTI_USER ACCESS TO SATELLITES • DEBRIS MITIGATION • RENDEZVOUS/DOCKING • LUNAR LANDER & MARTIAN HELICOPTERS
Additional benefits of this approach
• New way of doing “fundamental physics”• the most effective things that a small satellite can
do.• ways in which everyone can involve in space
science
Think of
Lower hurdles for easier access to space
Small but Smart and Quick
It is not easy to “involve in the field of Space Science”
Only many possibilities can encourage many players to take part in;
10cm x 10cm x 10cmCube Sat. (U. Tokyo)2003/June/30 LaunchCost < $ 100K (including launch)
Conclusion
• The universe is the current frontier for new exciting physics
• Space is a privileged reference frame to study the universe• Very large, powerful facilities will bring us to new
frontiers in knowledge• Small satellites, as intermediate steps to reach the most
ambitious goal set by major satellites, both testing new technologies and educating a new generation of laboratory oriented astroparticle physicsts
……and hopefully bringing us some big surprises