Calibration of gamma -ray instruments for Nuclear...

CalibrationCalibration ofof gammagamma--rayrayinstrumentsinstruments forfor Nuclear Nuclear

AstrophysicsAstrophysics

José Manuel Alvarez (IEEC-CSIC, Barcelona)Margarita Hernanz (IEEC-CSIC, Barcelona)Peter von Ballmoos (CESR, Toulouse)

OutlineOutline

• Gamma-rays in astrophysics

• Detection of gamma-rays

• How to focus γ-rays?

• Steps towards a γ�rays lens for nuclear astrophysics� CLAIRE: a focusing γ�� lens � The MAX mission

• Experimental proposals for the GRL

RadioactiveRadioactive isotopesisotopes relevantrelevant forfor γγ--ray ray line astronomyline astronomy

Isotope Decay chain Lifetime Line energy (keV)

56Ni 56Ni 56Co 8.8 d 158, 812, 750, 480

56Co 56Co 56Fe 111 d 847, 1238

57Ni 57Ni 57Co 57Fe (52 h) 390 d 122

44Ti 44Ti 44Sc 44Ca 89 y (5.4 h) 78, 68, 1157

26Al 26Al 26Mg 1.0 x 106 y 1809

60Fe 60Fe 60Co 60Ni 2.0 x 106 y (7.6 y) 1173, 1332

7Be 7Be 7Li 77d 478

22Na 22Na 22Ne 3.8 y 1275

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γγ--rayray emission from galactic radioactivityemission from galactic radioactivity

� Relevant radioactive nuclei for galactic γ-ray line emission:� how and where they are synthesized:

� nucleosynthesis (hydrostatic and explosive), in stars� interaction with cosmic rays, in the interstellar medium

� Electron-positron annihilation emission (line and continuum): � e+ from β+- unstable nuclei � BUT other sources of e+ (≠ radioactivity) exist

SitesSites ofof explosiveexplosive nucleosynthesisnucleosynthesis relevantrelevantforfor γγ--ray line astronomyray line astronomy

• SUPERNOVAE:� Thermonuclear supernovae (SN Ia): exploding whitedwarfs in binary systems (no remnant)� Core collapse supernovae (SN II, SN Ib/c): explodingmassive stars (M ≥ 10 M

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remnant)

v ∼ 104 km/s, E ∼ 1051 erg, Mej ∼ M�

• CLASSICAL NOVAE:Explosion of the external H-rich accreted shells of a whitedwarf in a binary system

v ∼ 102 - 103 km/s, E ∼ 1045 erg, Mej ∼ 10-4 - 10-5 M�

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Compton GammaCompton Gamma--Ray Observatory: Ray Observatory: COMPTEL map of the 1.8 MeV line of COMPTEL map of the 1.8 MeV line of 2626AlAl

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γγ--ray detectionray detection

How to focus How to focus γγ--rays?rays?•Diffraction: Bragg condition

•Crystal plane spacing:

•(h,k,l: Miller indices of crystal planes)

•d smaller for outer rings

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L E N S L E N S A gammaA gamma--ray lens for nuclear astrophysicsray lens for nuclear astrophysics

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CLAIRE: a CLAIRE: a γγ--ray lens prototyperay lens prototype8 rings - 576 Ge crystals – 45 cm diameter – 511 cm2 area

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Does it work? What’s expected for sources at infinity?Does it work? What’s expected for sources at infinity?

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CLAIRE TGD: CLAIRE TGD: atat 200m200m

Is the lens performing as expected for sources at infinity?Is the lens performing as expected for sources at infinity?

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CLAIRE:balloonCLAIRE:balloon--borne borne γγ--raysrays lens telescopelens telescope

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Telescope components :• Tracker (layers of Si strip detectors)• Calorimeter (CsI or CdTe)• Shielding (plastic scintillator)

Detection Principle:• Compton (< 10 MeV)• Pair creation (> 10 MeV)• Electron tracking• Polarimeter

Parameters :• energy range : 400 keV - 50 MeV• spectral resolution : 3-4 % (FWHM) • field of view : 120° (FWHM)• angular resolution : 2-4° (FWHM)• effective surface : 100 cm2

• sensitivity : > 10 × COMPTEL• new science: polarimetry

Mega Mega γγ--ray telescoperay telescope

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Calibration of gamma -ray instruments for Nuclear...

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