1 / 18

Effects of LCLS X-Ray Mirrors

This presentation by John Arthur discusses the impact of offset mirrors in the FEE on removing background radiation, the locations of X-ray mirrors in FEE for different experiments, and the effects of mirror imperfections on beam quality and imaging.

johnc
Download Presentation

Effects of LCLS X-Ray Mirrors

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. Effects of LCLS X-Ray Mirrors John Arthur Presenting work by Peter Stefan and Mike Pivovaroff

  2. Offset mirrors in the FEE Upstream of all LCLS experiments Will remove high-energy background radiation FEL radiation reflected (>95%) SiC 1.5mrad SiC 1.5mrad 24mm offset Background from high harmonics and Bremsstrahlung not reflected

  3. X-ray mirror locations in FEE Soft x-ray mirrors Hard x-ray mirrors ~14m

  4. NEH AMO SXR X-ray pump-probe soft x-ray line hard x-ray line Hutch 1 Hutch 2 Hutch 3

  5. FEH XPCS Coherent x-ray imaging High energy density science Hutch 4 Hutch 5 Hutch 6

  6. Effects of Mirror Imperfections • Imperfections happen on all length scales • Power Spectral Density function (PSD) typically shows fractal power law behavior (with smaller errors at shorter wavelengths) • Roughness • Errors on x-ray wavelength scale • Cause scatter far out of direct beam • Slope errors • Errors on micron scale (larger than l, but small compared to beam footprint) • Cause broadening of beam divergence

  7. Beam profile downstream of imperfect mirror Broadening due to slope error Beam distorted by mirror Scatter due to roughness Ideal beam

  8. For the LCLS, mirror roughness should not be a big problem. Realistic values of roughness will remove <5% of the beam intensity from the central spot. Slope errors will broaden the beam and reduce its brightness. This is our major concern.

  9. We considered three cases for slope error: rms = 1 µrad, 0.5µrad, and 0.1µrad The state of the art for 1m-length mirrors: 1 µrad mirrors are readily available from several vendors 0.5 µrad mirrors are probably available, for a price 0.1 µrad mirrors may not be available today, but will be within a few years

  10. Note: shorter mirrors are better (World record: 0.01µrad rms, for a 100mm-long mirror) The 1m length of the LCLS hard x-ray mirrors is driven by the desire to reflect 24keV radiation, and the desire to accept all of the beam at 2 keV, and still not hit the end regions of the mirror. Also note: the soft x-ray mirrors are short. They operate at a steeper angle, so a length of only 100-200mm is needed.

  11. NEH Hutch 1 z=117.1m (distance from end of undulator) Using short B4C mirrors at 15mrad incidence 2keV 800eV 2keV 800eV 800eV 2keV 2keV 800eV

  12. NEH Hutch 2 z=128.1m Using short B4C mirrors at 15mrad incidence 800eV 2keV 800eV 2keV 800eV 800eV 2keV 2keV

  13. NEH Hutch 3 z=138.8m Using 1m SiC mirrors at 1.3mrad incidence 8keV 2keV 8keV 8keV 8keV 2keV 2keV 2keV

  14. FEH Hutch 4 z=364.9m Using 1m SiC mirrors at 1.3mrad incidence 2keV 8keV 2keV 8keV 2keV 8keV 2keV 8keV

  15. FEH Hutch 5 z=385.5m Using 1m SiC mirrors at 1.3mrad incidence 2keV 8keV 8keV 8keV 2keV 2keV 8keV 2keV

  16. FEH Hutch 6 z= 406.1m Using 1m SiC mirrors at 1.3mrad incidence 2keV 8keV 2keV 8keV 8keV 8keV 2keV 2keV

More Related