(Krause 2004)
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(Krause 2004)Steven BoggsUC BerkeleyDepartment of Physics
MeV Gamma Ray Nuclear Astrophysics
Yesterday: Science and ObservationsToday: Instrumentation
Nuclear Gamma-Rays
Atmosphere is opaque at these energies.
Gamma-ray interactions
Index of refraction ~1.0000
Penetration ≥ cm into materials
Standard mirrors & lenses don’t work
CZT Semiconductor
Liquid Xe
Si Semiconductor
Ge Semiconductor
Gamma Ray Detectors
NaI, CsI, BGO
Scintillators• high Z• large volume• room temperature• moderate/poor resolution (3-10%)
Solid State• good/excellent resolution (<2%)• may require cooling• finer position resolution• more channels/power
The radiation environment
The Space Radiation EnvironmentThe Space Radiation Environment
Secondaries induced by cosmic-ray
interaction with upper atmosphere:
Albedo photons, neutrons, electrons,
positrons
Radiation belts:
Trapped protons (SAA) & resulting activation, electrons
Cosmic rays:• Photons• Protons (& activation)
• Alphas• Ions• Electrons• Positrons
Sun through solar flares: photons, charged particles
Compton Gamma-Ray Observatory(1991-2000)
COMPTEL (0.8-30 MeV)
EGRET(20 MeV – 30 GeV)
BATSE(20-600 keV)
OSSE(50 keV – 10 MeV)
Spectroscopy, no Imaging
“light bucket”
Galactic Center Positrons
(Purcell et al., 1993)
(from P. von Ballmoos)
Coded Aperture Imaging
pinhole camera…. with lots of pinholes
Good for: point sources photons that stop in the mask (<0.2 MeV)
IBIS (15 keV-10 MeV)
JEM-X(3-35 keV)
SPI(30 keV-8 MeV)
OMC(500-600 nm)
INTErnational Gamma-Ray Astrophysics Laboratory (launched October 2002)
E/E ~ 500, ~ 2º
E/E ~ 10, ~ 20’
IBIS/INTEGRAL
ISGRI: 128x128 CdTe array (4x4x2 mm3)PICsIT: 64x64 CsI array (8.4x8.4x30 mm3)
IBIS Galactic Plane Survey
(Bird & Walter 2004)
SPI/INTEGRAL
19 Ge detectors
(Weidenspointner et al., 2008)
SPI Positron Map
Compton Gamma-Ray Observatory (1991-2000)
COMPTEL (0.8-30 MeV)
EGRET(20 MeV – 30 GeV)
BATSE(20-600 keV)
OSSE(50 keV – 10 MeV)
(Schoenfelder et al., 1993, ApJS 86, 657)
COMPTEL DetectorsD1: 4188 cm2 liq. scint.D2: 8620 cm2 NaIE: 5-8% (FWHM)X ~ Y ~ 2 cm (1)Z ~ 3 cm (1)t ~ 0.25ns
COMPTEL Performance0.8-30 MeVE/E ~ 9-14 (FWHM) ~3º
Aeff < 20 cm2
FOV ~ 1str
COMPTEL - Compton Imaging cos = 1+mc2(1/E2-1/E)
26Al (1.809 MeV), ~1Myr
(Oberlack et al., 1996; Pluschke et al., 2001)
Compton Telescopes: Then & Now
CGRO/COMPTEL• ~40 cm3 resolution• E/E ~ 10%• 0.1% efficiency
ACT Enabling Detectors• 1 mm3 resolution• E/E ~ 0.2-1%• 10-20% efficiency• background rejection• polarization
3 decades…
Overview of the Overview of the Nuclear Compton TelescopeNuclear Compton Telescope
A balloon-borne A balloon-borne -ray spectrometer, polarimeter & imager-ray spectrometer, polarimeter & imager
Steven Boggs, UCBNCT Collaboration: Berkeley, NTHU, NCU, NSPO, NUU, LBNL, CESR
Heart of NCT:Cross Strip 3-D GeDs • 37x37 strips• 2-mm pitch• 15-mm thickness• 81000 mm3 volume• 1.6 mm3 localization• ~2.1-keV noise resolution
Nuclear Compton Telescopeballoon payload
3D GeD Design
(Luke et al. 1992, 1994)
Single-Pixel Spectra (56Co)• excellent GeD Spectroscopy• plus full 3-D positioning
60Co Laboratory Tests1.173, 1.333 MeV
1.173 MeV processed image
Source Decay Energy Goal SNe Ia (?) e+e- 0.511 36 map SNe II/Ib 26Al 1.809 MeV 36 map 60Fe 1.173, 1.333 5 detect SNe 44Ti 1.157 resolved line BHs e+e- ≤0.511 discovery
Next flight, May 2009• northern hemisphere• primarily compact objects
The 2005 balloon flight from Fort The 2005 balloon flight from Fort SumnerSumnerImpressions from the NCT 2009 Balloon flightImpressions from the NCT 2009 Balloon flight
BGO shieldBGO shield
lNlN22 dewar dewar
Pre-AmpsPre-Amps
Differential Differential GPSGPS
RotorRotor
DetectorDetector
Electronics BayElectronics Bay
CSBF SIPCSBF SIP
Solar PanelsSolar Panels
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4D sin = n
Alternate layers of high/low Z materialsex. W/Si
D ~ 25 Å (technological limit) < 1 Å (0.18 Å @ 68 keV)~ 30’f ~ 10 m
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SN 1987A in the LMC
(Suntzeff et al.1992; Diehl & Timmes 1998)
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Blue supergiant (~20 M, 6 M He core) (Arnett et al., 1989)
Spherical models predict 44Ti < 1000 km/s
56Ni mixed out to ~3000 km/s (0.7 keV at 68 keV)
(Motizuki & Kumagai 2004)
~110-4 M
2D sin = n
Use a crystal to bend (“focus”) the -rays
D ~ 1 Å (crystal spacing) < 1 Å (0.014 Å @ 0.847 MeV) ~ 10’f ~ 60 m
Bragg Scattering
von Ballmoos et al., CESR, Toulouse
Laue Lens: Focusing -rays