Hi Matthew,
I think the name of this .lam file is a bit misleading; to my understanding the 5 wavelengths are a combination of Kα1α2 determined by Höltzer et al. [1] and satellite reflections described by Cheary & Coelho [2]
The origin of the satellite peaks is nicely described in the "Fundamental Parameters Line Profile Fitting in
Laboratory Diffractometers" paper by Cheary[3]
Another feature of Kα emission lines which needs to
be included in an accurate line profile fitting model is
the satellite multiplet structure in the high energy tail as
shown in Fig. 27. As a group these have an intensity of
≈0.6 % of the Kα1 emission line in the case of Cu rising
uniformly with decreasing atomic number up to
≈1.4 % for Cr [35]. Satellites lines are also evident in
Kβ1β3 spectra and appear on both the low energy and
high energy tails as the Kβ' and Kβ" lines [36]. The
Kα3α4 non-diagram lines arise from the transition
1s2p → 2p2 in which the actual vacancy transition is
1s → 2p, but in the presence of a 2p spectator hole
[37,38].
[1] G. Höltzer, M. Fritsch, M. Deutsch, J. Härtwig, and E. Förster,
Phys. Rev. A 56, 4554 (1997).
[2] R.W. Cheary and A. A. Coelho, J. Appl. Cryst. 25, 109 (1992).
[3] R.W. Cheary and A. A. Coelho, J. Res. Natl. Inst. Stand. Technol. 109, 1-25 (2004)
[35] L. G. Parratt, Phys. Rev. 50, 1 (1936).
[36] R. E. LaVilla, Phys. Rev. A 19, 717 (1979).
[37] N. Maskil and M. Deutsche, Phys. Rev. A 38, 3467 (1988).
[38] M. Fritsch, C. C. Kao, K. Hämäläinen, O. Gong, E. Forster, and
M. Deutsch, Phys. Rev. A 57, 1686 (1998).
Hope that helps?
Cheers,
Luzia