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Figure 2
(a) Binding energies of the electron orbitals of the rare gases versus photon energy and wavelength in the FLASH wavelength range. (b) Example of an average electron time-of-flight spectrum from 572 single shots of FLASH at λ = 13.6 nm. For a decreasing FEL wavelength the xenon photolines shift towards smaller arrival times as illustrated by the arrows. The shift will be larger for the low kinetic energy 4d lines than for the faster 5p electrons due to the non-linear energy scale. To give an idea of the energy scale, the markers indicate the Xe 4d energy splitting and the difference in kinetic energy between the 5p and 5s photoelectrons.

Journal logoJOURNAL OF
SYNCHROTRON
RADIATION
ISSN: 1600-5775
Volume 23| Part 1| January 2016| Pages 10-20
doi:10.1107/S1600577515022675
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