1 / 37

X-Ray Spectroscopy

X-Ray Spectroscopy. The need for high resolution X-ray spectroscopy Astrophysical Plasmas: Simulation of the emission from a gas at T = 10 7 K with normal abundances of elements. An energy resolution of ~ 10 eV is required to begin serious X-ray spectroscopy and a resolution

albany
Télécharger la présentation

X-Ray Spectroscopy

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. X-Ray Spectroscopy

  2. The need for high resolution • X-ray spectroscopy • Astrophysical Plasmas: • Simulation of the emission from • a gas at T = 107 K with normal • abundances of elements. • An energy resolution of ~ 10 eV • is required to begin serious • X-ray spectroscopy and a resolution • of ~ 1 eV is required for complete • plasma diagnostics and velocity • measurements. 1 eV 10 eV 100 eV Energy (keV)

  3. What’s a milliCrab? • The second brightest X-ray (1-10 keV) source in the sky is the Crab nebula • Its photon intensity at the top of the atmosphere of the Earth is ~ 10 cm-2 s-1 • There are about 1000 AGN (“quasars”) at a level of about .01 cm-2 s-1 =1 mC

  4. Oxygen Shock-Heated to kT ~ 0.3 keV ionized H-like He-like Ionization age

  5. X-Ray Spectrum with 100 eV Resolution 4-6 keV Cassiopeia A ACIS spectrum

  6. Estimates of H- and He-Like Energies vs Atomic Number

  7. X-Ray Spectrometers - I • Proportional counters have • High efficiency • Imaging capability • Multiplex spatial/spectral without confusion But resolving power ≡ E/(δE) ≈ 6√E(keV)

  8. X-Ray Spectrometers - II • Bragg crystal spectrometers • Dispersive, so they can use any detectors • Can achieve R > 103 • Can have high efficiency (at one E at a time) But no imaging or multiplexing capabilities (i.e. can look at only one E at a time)

  9. X-Ray Spectrometers - III • Gratings • Dispersive • Can have moderate (few %) efficiencies • Can multiplex (all E at the same time) • Can have R > 103/√E(keV) (better for low E) But image and spectral orders are mixed

  10. Capella Chandra HETG

  11. X-Ray Spectrometers - IV • Solid State (including CCDs) • High efficiency (>90%) • Non-dispersive, can multiplex all E • Imaging capability without confusion with E But cannot achieve better than R ≈ 25√E(keV) (Resolution ≈ 40√E(keV) eV)

  12. The need for high resolution • X-ray spectroscopy • Astrophysical Plasmas: • Simulation of the emission from • a gas at T = 107 K with normal • abundances of elements. • An energy resolution of ~ 10 eV • is required to begin serious • X-ray spectroscopy and a resolution • of ~ 1 eV is required for complete • plasma diagnostics and velocity • measurements. 1 eV 10 eV 100 eV Energy (keV)

  13. X-Ray Spectrometers - V • Cryogenic Microcalorimeters • High efficiency (>90%) • Non-dispersive, can multiplex all E • Imaging capability without confusion with E And can achieve R > 103 √E(keV)

  14. w Expected with XRS (12 eV) He-like Fe He-like Fe “triplet” y, x z Neutral Fe w x H-like Fe Counts z y Chandra HEG (~ 60 eV) Energy (keV) Physical Conditions Through X-Ray Spectroscopy Fe-K lines provide very clean diagnostics. One such diagnostic: excellent density-independent temperature sensitivity in the range 107–108 Kelvin.

  15. The X-ray Microcalorimeter Features high resolution, non-dispersive spectroscopy with high quantum efficiency over K- and L- atomic transition band. Moseley, Mather and McCammon 1984

  16. Simple Energy Resolution Argument • δT = E/C (temperature rise for E deposition) • C ≈ N(kT)/T (N = # of phonons with <kT>) • N ≈ C/k (fluctuation in N is the “noise”) • ΔN = √N (Poisson statistics) • R = E/(ΔE) (resolving power) • ΔE ≈ kT√N ≈ kT√(C/k) ≈ √(kT2C) • More carefully, ΔE = 2.35 ζ √(kT2C)

  17. Spectral Resolving Power: Depends on thermometer technology Temperature-sensitive resistance Resolution limited by thermal fluctuations between sensor and heat bath and Johnson noise. Doped semiconductor R (ohms) Temperature T = operating temperature (50-100 mK) C = heat capacity • ~ 2 - 4 for doped semiconductors ~ 0.2for transition edge sensors For both thermometer schemes a spectral resolution of few a eV is possible! R (ohms) Superconducting Transition Temperature

  18. Basic requirements: • • Low temperature • • Sensitive thermometer • • Thermal link weak enough that the time for restoration of the base temperature is the slowest time constant in the system yet not so weak that the device is made too slow to handle the incident flux. • • Absorber with high cross section yet low heat capacity • • Reproducible and efficient thermalization Types of thermometers: • resistive • capacitive • inductive • paramagnetic • electron tunneling

  19. . . . Microcalorimeter Arrays XQC Array: 36 array of 0.5  2 mm pixels.

  20. X-Ray Quantum Calorimeter Dewar

  21. E 6.4 eV FWHM Ion beam 1.5 m Energy (keV) (after anneal) ~ 6 times deeper thermometer Deep implants using silicon-on-insulator wafers. 625 m pixels GSFC Mn Ka1 Mn Ka2

  22. RTS – Rotating Target Source X-ray lines continuum X-ray source X-ray continuum rotating target wheel targets (one is open for continuum)

  23. motor target wheel

More Related