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Metallic Magnetic Calorimeter

Metallic Magnetic Calorimeter. H. Au:Er. Calorimeter Signal. satisfying agreement of theory and experiment signal size can be predicted !. 122 keV in Au :Er 300ppm. Resolution of optimized detector:. Gradiometer With Two Sensors: Two-Pixel Detector. 50 μ m. commercial SQUID chip

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Metallic Magnetic Calorimeter

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  1. Metallic Magnetic Calorimeter H Au:Er 2

  2. Calorimeter Signal • satisfying agreement of theory and experiment • signal size can be predicted! 122 keV in Au:Er 300ppm Resolution of optimized detector: 3

  3. Gradiometer With Two Sensors: Two-Pixel Detector 50 μm commercial SQUID chip M.B. Ketchen, IBM 1992 performance of pixels almost identical 4

  4. Kα Kβ MMC Detector 2003 160 μm x 160 μm x 5 μm 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 clean spectrum 5

  5. natural linewidth Resolution: Kα-Line 55Mn Raw Data energy resolution 3.4 eV 6

  6. Kβ-Line 55Mn A. Fleischmann, M. Linck, T. Daniyarov, H. Rotzinger, C. Enss, G.M. Seidel, Nucl. Instr. and Meth. A 520, 27 (2004). 7

  7. Baseline Noise twoAu:Er 300 ppm sensors Gold absorber: 160 x 160 x 5 m3 oneAu:Er 300 ppm sensors Gold absorber: 160 x 160 x 5 m3 Spectrum: 3.5 eV because of Temperature stabilization problems 8

  8. 3.4 eV 6 eV E/E at 6 keV 2 eV ionisation detectors 9

  9. Predicted Resolution for Different Detectors Resolution: Energy range: 1 ... 6 keV Energy range: 0.25 ... 0.6 keV T = 50 mK, 0 = 10-6 s, 1 = 10-4 s T = 50 mK, 0 = 10-6 s, 1 = 10-4 s 250 x 250 x 5 m3, Bi absorber 120 x 120 x 0.5 m3, Bi absorber Au:Er 900 ppm sensor,  35m, h = 14m Au:Er 900 ppm sensor,  20m, h = 8m EFWHM = 0.7 eV EFWHM = 0.1 eV 10

  10. spot welded detector heat capacity 10-9 J/K MMC Detectors for X Ray Astronomy increase detector speed not a problem micro-fabrication of MMCs a problem, but likely to be solvable schemes for arrays and multiplexing a very complex problem 11

  11. 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 12

  12. Informal Collaboration on MMCs for Astronomy A. Fleischmann M. Linck T. Daniyarov H. Rotzinger A. Burg C. Enss S. Romaine R. Bruni SAO S.R. Bandler T.R. Stevenson F.S. Porter E. Figueroa-Feliciano C.K. Stahle R. Kelley Heidelberg J. Beyer D. Drung T. Schurig Goddard K.D. Irwin B.L. Zink G.C. Hilton D.P. Pappas J.N. Ullom M.E. Huber, Uni. Colorado Berlin H.-G. Meyer R. Stolz S. Zarisarenko Boulder Jena G.M. Seidel Y.H. Kim Y.H. Huang H. Eguchi 13

  13. SAO development of deposition techniques for Au:Er integrate Au:Er sensors on SQUID chips 14

  14. NASA - GSFC development of suitable absorbers Bi:Cu develop means of fabricating MMC mushrooms investigating different transformerschemes development of position sensitive MMCs MMC MMC 15

  15. NIST Boulder development of integrated MMCs investigating new schemes for MMCs: self-inductance MMCs develop optimized SQUIDs explore new multiplexing techniques develop fabrication methods Optimized SQUID Self-Inductance Meander Transformer Co-evaporated Au:Er Sensor Film 16

  16. PTB Berlin development of optimizied SQUIDs high speed low-noise readout electronics 17

  17. IPTH Jena development of optimized SQUIDs low noise readout electronics optimized sensor design 18

  18. Brown/Heidelberg investigate alternative sensor materials study fundamental noise develop new sensor geometries develop deposition techniques for Au:Er optimize single pixel performance study properties of small arrays 19

  19. Summary MMCs can be a new exciting tool for X-ray astronomy Let’s work to make it happen SOHO 304 Å 20

  20. Problem: Slewrate too low slew rate of SQUID too low (100 0/ms) limits the usable signal size feedback of Ketchen-SQUID to weak 21

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