Post on 15-Jan-2016
description
Status of Development of
Metallic Magnetic Calorimeters
A. Fleischmann, T. Daniyarov H. Rotzinger, M. Linck, C. Enss
Kirchhoff-Institut für PhysikUniversität Heidelberg
H. Eguchi, Y.H. Yong, G.M. SeidelDepartment of Physics
Brown University
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Metallic Magnetic Calorimeter
Au:Er
H
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Calorimeter Signal
122 keV in Au:Er 300ppm
• satisfying agreement of theory and experiment
• signal size can be predicted!
Resolution of optimized detector:
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Gradiometer With Two Sensors: Two-Pixel Detector
performance of pixels almost identical
commercial SQUID chipM.B. Ketchen, IBM 1992
50 μm
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two Au:Er 300 ppm sensors
Gold absorber: 160 x 160 x 5 m3
Heat capacity corresponds to a Bi absorber of 250 x 250 x 28 m3
MMC Detector 2003
160 μm x 160 μm x 5 μm
clean spectrum
Kα
Kβ
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Resolution: Kα-Line 55Mn
energy resolution 3.4 eV
Raw Data
natural linewidth
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Kβ-Line 55Mn
A. Fleischmann, M. Linck, T. Daniyarov, H. Rotzinger, C. Enss, G.M. Seidel, Nucl. Instr. and Meth. A 520, 27 (2004).
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Baseline Noise
two Au:Er 300 ppm sensorsGold absorber: 160 x 160 x 5 m3
one Au:Er 300 ppm sensorsGold absorber: 160 x 160 x 5 m3
Spectrum: 3.5 eV because of Temperature stabilization problems
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E/E at 6 keV
ionisation detectors
2 eV
6 eV
3.4 eV
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Predicted Resolution for Different Detectors
Resolution:
Energy range: 1 ... 6 keV
250 x 250 x 5 m3, Bi absorber
Au:Er 900 ppm sensor, 35 m, h = 14 m
T = 50 mK, 0 = 10-6 s, 1 = 10-4 s
EFWHM = 0.7 eV
Energy range: 0.25 ... 0.6 keV
120 x 120 x 0.5 m3, Bi absorber
Au:Er 900 ppm sensor, 20 m, h = 8 m
T = 50 mK, 0 = 10-6 s, 1 = 10-4 s
EFWHM = 0.1 eV
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MMC Detectors for X Ray Astronomy
increase detector speed
not a problem
micro-fabrication of MMCs
schemes for arrays and multiplexing
a problem, but likely to be solvable
a very complex problem
spot welded detector heat capacity 10-9 J/K
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MMC Arrays for X Ray Astronomy
speed
cross talk
efficiency
homogeneity
power dissipation
signal to noise
complexity
stability
coupling schemes
fabrication techniques
layout and wiring schemes
signal analysis
schemes
readout schemes
?
?MMC specific : non-contact readout
non-dissipative method
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Informal Collaboration on MMCs for Astronomy
S.R. BandlerT.R. StevensonF.S. PorterE. Figueroa-FelicianoC.K. StahleR. Kelley
S. Romaine R. Bruni
A. FleischmannM. LinckT. DaniyarovH. RotzingerA. BurgC. Enss
Berlin
SAO
G.M. SeidelY.H. KimY.H. HuangH. Eguchi
K.D. IrwinB.L. ZinkG.C. Hilton D.P. Pappas J.N. UllomM.E. Huber, Uni. Colorado
Heidelberg
Goddard
Boulder
J. BeyerD. DrungT. Schurig
H.-G. MeyerR. StolzS. Zarisarenko
Jena
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SAO
development of deposition techniques for Au:Er
integrate Au:Er sensors on SQUID chips
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NASA - GSFC
development of suitable absorbers Bi:Cudevelop means of fabricating MMC mushrooms investigating different transformer schemes development of position sensitive MMCs
MMC MMC
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NIST Boulder
development of integrated MMCsinvestigating new schemes for MMCs: self-inductance MMCsdevelop optimized SQUIDs explore new multiplexing techniquesdevelop fabrication methods
OptimizedSQUID
Co-evaporatedAu:Er Sensor
Film
Self-InductanceMeander
Transformer
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PTB Berlin
development of optimizied SQUIDs
high speed low-noise readout electronics
10-1 100 101 102 103 104 105 106 107
1
10
f / Hz
T = 4.2 K
SI
/ (p
A/
Hz)
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IPTH Jena
development of optimized SQUIDs
low noise readout electronics
optimized sensor design
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Brown/Heidelberg
investigate alternative sensor materialsstudy fundamental noisedevelop new sensor geometries develop deposition techniques for Au:Eroptimize single pixel performancestudy properties of small arrays
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MMCs can be a new exciting tool for X-ray astronomy
Let’s work to make it happen
Summary
SOHO 304 Å
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Problem: Slewrate too low
slew rate of SQUID too low (100 0/ms)
limits the usable signal size
feedback of Ketchen-SQUID to weak