The University of New Hampshire
EOS Space Science Center
Measuring Space Radiation with the Angle Detecting Inclined Sensor (ADIS) Method 
J.J. Connell, C. Lopate and R.B. McKibben
Space Science Center
Institute for the Study of Earth, Ocean and Space
and Department of Physics 
University of New Hampshire
Durham, NH 03824

Slide 2
The University of New Hampshire
EOS Space Science Center
Measuring Energetic Ions in Space

Delta E/ Delta x versus residual energy (E')

Slide 3
The University of New Hampshire
EOS Space Science Center
Fig. VI-2. Cross section of telescope showing sensors. Labels for FIN, Particle Direction, 20 degrees, Mylar Windows, Absorbers, Ga-As Diodes, D1, D2, D3
IMP-4 Telescope (circa 1967)

Slide 4
The University of New Hampshire
EOS Space Science Center
Measuring Energetic Ions in Space

Delta E/Delta x versus residual energy (E')

Slide 5
The University of New Hampshire
EOS Space Science Center
Charge resolution improved by using curved detectors
Curved detectors reduce the variations in thickness with angle of incidence
Used on IMP-6, 7 & 8
Pioneer-10 & 11
Voyager-1 & 2
Design of IMP-7/8 University of Chicago with labels for PM Tube, D1, D2, D3, D4, D5, D6, PM Tube with scale 2 cm

Slide 6
The University of New Hampshire
EOS Space Science Center
Ulysses High Energy Telescope (HET)
Drawing with labels S, PMT, D1, D2, D3, D4, D5, D6, K1, K2, K3, K4, K5, K6
Drawing of Detector Position Sensing Strips
Orientation of Detector Position Sensing Strips

Slide 7
The University of New Hampshire
EOS Space Science Center
Ulysses HET flight data with (A) and without (B) correcting for particle angle of incidence - corrections need to identify elements.

Two graphs.
Graph 1 indicates Angle Corrected Energy Loss in K1 (MeV) to Residual Energy (MeV)
Graph 2 indicates Energy Loss in K1 (MeV) to Residual Energy (MeV)

Slide 8
The University of New Hampshire
EOS Space Science Center
Angle Detecting Inclined Sensor (ADIS)
Different geometry in telescope stack

Uses standard Si detector technology

Low risk

Low mass

Low power

On-board event processing possible

Tested at an accelerator, and it works!

Slide 9
The University of New Hampshire
EOS Space Science Center
ADIS Concept
formula E1/Ex = sec(theda)/sec (theda + phi)

Slide 10
Design of Scintiller Cup with a scale of 2 cm

Slide 11
The University of New Hampshire
EOS Space Science Center
Simplest ADIS instrument just uses four solid state detectors.

Can add detectors for specific applications.

Not limited to solid state detectors.

Can add others below:

Scintillator for thicker detector (as on IMP)

Cherenkov to extend energy range

Slide 12
The University of New Hampshire
EOS Space Science Center
If you approximate the range of a ion as power law:

(Basis of charge and mass analysis for Ulysses HET)

formulas:
R = Ko*A/Z squared (E/A)alpha 
= Ko*1/Z squared * A alpha to the -1 * E alpha

Slide 13
The University of New Hampshire
EOS Space Science Center
D sub x =2*T sub 2/T sub 1[(E sub 4 + E sub 3 + E sub 2 + E sub 1) to the power of alpha - (E sub 4 + E sub 3 + E sub 2) to the power of alpha / (E sub 4 + E sub 3 + E sub 2) to the power of alpha - (E sub 4 + E sub 3) to the power of alpha] - square root of 3
D sub y =2*T sub 3/T sub 1[(E sub 4 + E sub 3 + E sub 2 + E sub 1) to the power of alpha - (E sub 4 + E sub 3 + E sub 2) to the power of alpha / (E sub 4 + E sub 3) to the power of alpha - (E sub 4) to the power of alpha] - square root of 3
and
Z = K/T sub 1[(E sub 4 + E sub 3 + E sub 2 + E sub 1) to the power of alpha - (E sub 4 + E sub 3 + E sub 2) to the power of alpha / (1 + D to the power of 2 sub x + D to the power of 2 sub y) to the power of 1/2] to the power of 1 / (alpha + 1)

Slide 14
The University of New Hampshire
EOS Space Science Center
Calculation simple enough to be done by on-board processor 

Greatly reduces telemetry requirements

Slide 15
The University of New Hampshire
EOS Space Science Center
ADIS Tested with 48Ca at the National Superconducting Cyclotron Laboratory
1. Instrument rotated in beams to simulate omni-directional flux in space
2. Energies varied by a moving absorber
3. Primary and fragmented beams use
4. Data taken with 50, 100, and 200 mm D1-3 detectors at 15, 30 and 45 degrees inclination
5. D2-3 detectors circular, NOT oval

Large amounts of dead material degraded performance


Slide 16
The University of New Hampshire
EOS Space Science Center
image of scintollator cup


Slide 17
The University of New Hampshire
EOS Space Science Center
ADIS NSCL 48Ca Fragment Beam D1, D2 and 
D3 200 µm thick 30 degree D2, D3 inclinations

graph of All raw data uncorrected for angle of incidence. No selection criteria. Axis labels Charge (Z) from 12 - 22 and Counts from 0 - 8000


Slide 18
The University of New Hampshire
EOS Space Science Center
ADIS NSCL 48Ca Fragment Beam D1, D2 and 
D3 200 µm thick 30 degree D2, D3 inclinations

two graphs - one for All raw data uncorrected for angle of incidence and No selection criteria. Second graph for All raw data corrected for angle of incidence and No selection criteria. Axis labels Charge (Z) from 12 - 22 and Counts from 0 - 8000

Slide 19
The University of New Hampshire
EOS Space Science Center
ADIS NSCL 48Ca Fragment Beam D1, D2 and 
D3 200 µm thick 30 degree D2, D3 inclinations

three graphs - one for All raw data uncorrected for angle of incidence and No selection criteria. Second graph for All raw data corrected for angle of incidence and No selection criteria. Third graph of All raw data corrected for angle of incidence and Stopping particle only. Axis labels Charge (Z) from 12 - 22 and Counts from 0 - 8000

Slide 20
The University of New Hampshire
EOS Space Science Center
ADIS Compared to Other Instrument Architectures

System			Flight Examples		Complexity 	PHA channels	Power	Risk

Curved detectors	IMP-8,			Medium		~5		~4 W	High
(Not made since 	Pioneer,
1970’s)			Voyager

Segmented detectors	SOHO			High		~10		~8 W	Low

Position Sensing	Ulysses, 		Very High	18		4.5 W	Low	
detectors		CRRES,					20		6 W
			ACE/SIS					>500		18 W

ADIS						Low		~5		~4 W	Low


Slide 21
The University of New Hampshire
EOS Space Science Center
An ADIS based Instrument had been selected for the High Energy Particle Sensor (HEPS) for NPOESS
Image of Instrument. Image of NPOESS patch for Northrop Grumman and Raytheion with DoD DOC NASA

Slide 22
The University of New Hampshire
EOS Space Science Center
The High Energy Particle Sensor (HEPS) will be a component of the Space Environment Sensor Suite (SESS).
The goal: A simple but capable instrument.
HEPS design draws on the heritage of earlier instruments from our group on IMP-8, Ulysses and CRRES. 
It combines an instrument of complexity comparable to our IMP-8 instrument with electronics concepts used on Ulysses and CRRES.
The Angle Detecting Inclinded Sensor (ADIS) system provides good charge resolution without the complexity of position sensing detectors

Slide 23
The University of New Hampshire
EOS Space Science Center
The High Energy Particle Sensor (HEPS)

Fluxes of H ions in six logarithmic energy intervals from 10 to ~320 MeV/u plus a seventh integral flux.
Fluxes of He ions in three logarithmic energy intervals from 10 to ~320 MeV/u plus a fourth integral flux.
Heavy ion fluxes through Ni at corresponding energies (but no integral) with individual charge resolution (s< 0.25 e). 
Linear Energy Transfer (LET) calculated from these data.
The geometrical factor will be ~1 cm2-sr 
HEPS is designed not to saturate at the highest fluxes of SEPs thus far observed.


Slide 24
The University of New Hampshire
EOS Space Science Center
HEPS will provide data on Solar Energetic Particles (SEP), Galactic Cosmic Rays (GCR) and Anomalous Cosmic Rays (ACR) as well as trapped


Slide 25
The University of New Hampshire
EOS Space Science Center
Present HEPS Resource Estimates are Preliminary

drawing of HEPS resource
Mass: ~4 k
gPower: ~3.6 
Telemetry: 350bps


Slide 26
The University of New Hampshire
EOS Space Science Center
HEPS

design of scintillator blocks and structure wire guides

Slide 27
The University of New Hampshire
EOS Space Science Center

HEPS is based on the Angle Detecting Inclined Sensor (ADIS) system.
There are three thin 50 micron detectors D1, D2 and D3:
D1 is a circular detector of ~600 mm2 area.
D2 and D3 are oval and inclined at 30 degrees.
D2 and D3 have a semi-minor and semi-major axis equal to the D1 radius and semi-major axis a factor 1.155 longer.
D4 and D5 are logical detector each consisting of a pair of 2000 micron thick, 600mm2 detectors.
D1-D5 are pulse-height analyzed.
R is a single detector to flag penetrating particles. It is not pulse-height analyzed.


Slide 28
The University of New Hampshire
EOS Space Science Center
Detail design of HEPS with labels for Top Cover, Backplane, analog boards, ADC/IFC, shield, logic board, memory board, CPU board, low voltage power converter, high voltage power converter, enclosure, front cover, window, collimator, telescope assembly, reflecting tube, and PMt
HEPS


Slide 29
The University of New Hampshire
EOS Space Science Center
The instrument will be housed in a single box that includes electronics boards. 
The box is divided to isolate the converter boards,the analog electronics boards and the digital boards.
Board attachment is modular for relatively simple replacement.
Minimal box thickness for NPOESS is currently 0.25 cm (100mils) to reduce exposure.
This would hardly be needed on a manned flight.


Slide 30
The University of New Hampshire
EOS Space Science Center
Preliminary workflow of HEPS System Functional block diagram. 
flow from D1, D2, D4, D5 thought the linar boards to the ADC/IFC board to the CPU board. HNH Space Science 10/6/2005 HEPS System Funcitonal Block Diagram V1.10


Slide 31
The University of New Hampshire
EOS Space Science Center
The HEPS electronics will consists of eight main boards plus a backplane motherboard 
3 Linear boards 
1 ADC /IFC board
1 Logic board
1 CPU board
Power converter board
HV board
A small I/O board supports the RS422 interface.


Slide 32
The University of New Hampshire
EOS Space Science Center
HEPS uses the standard approach of combining discriminator 
based logic rates with pulse height analysis of a sample of
events to determine fluxes for the measured species.

Priority system used to give preference to heavy ion species for PHA. 

On-board analysis means relatively large sample of PHA events: 1000’s identified per second.

HEPS does not measure electrons, but logic could be added to 
give electron measurements as in Ulysses and IMP-8. Energy 
range would be ~0.5 to ~10 MeV.


Slide 33
The University of New Hampshire
EOS Space Science Center
Detailed work flow of HEP D1 and D2 items on Linear A Board.


Slide 34
The University of New Hampshire
EOS Space Science Center
Two slower amps are used for events that will be pulse height analyzed. 
Because of the large dynamic range of the signals (~7000)
there is both a high gain and a low gain shaping amplifier.
These feed via an analog mux to a peak detect sample and 
hold (PDSH). 
The highest level discriminator determins which amplifier
(the high or low gain) feeds the sample and hold.
Thus, small signals are processed through the high gain amp
while large signals are processed through the low gain amp.


Slide 35
The University of New Hampshire
EOS Space Science Center
ADIS
Simple
Capable


Slide 36
The University of New Hampshire
EOS Space Science Center
A Phoswich-based Detector for Fast (~0.5-10 MeV) Neutrons
R.B. McKibben, J.M. Ryan, J.J. Connell, and J.R. Macri
Space Science Center
Institute for the Study of Earth, Ocean and Space
and Department of Physics 
University of New Hampshire
Durham, NH 03824

Slide 37
The University of New Hampshire
EOS Space Science Center
Side View and Face-On view diagram indicating position to Sun. scale 1 cm . labels for plastic and Csl (TI)
1/2" PMT and 1/2" PMT Side View and Face-On View. Labels Plastic and CsI(Tl) and To Sun 
1 cm 


Slide 38
The University of New Hampshire
EOS Space Science Center
A) Incident neutron spectra. B) Energy distribution of 
recoil protons in the detector from spectra in (A), C) Ratio
of numbers of recoil protons in two energy bands vs.
spectral index of incident neutrons.

Normalized to netrons expected in 1 day on 0.78 cm squared detector for flux of 1 n/(cm squared s) in range 1 < E < 20 MeV
Graph 1 - Neutron Energy (MeV)
Graph 2 - Recoil Proton Energy (MeV)
Graph 3 - Neutron Spectral Index (?)


Slide 39
The University of New Hampshire
EOS Space Science Center
Scattering cross-section and effective cross-section for producing a>0.25 MeV recoil proton

Graph of Neutron Energy (MeV) with the Power law approximation to elastic n-p cross section and Cross-Section for n-p scattering yielding proton energy > 0.25 MeV.
Neutron Energy (MeV)


Slide 40
The University of New Hampshire
EOS Space Science Center
A Phoswich-based Detector offers the potential for a very simple, low mass, low power monitor neutrons.