Hi Mike,

The table of emission lines that were first utilized by Probe Software for plotting KLM markers and other purposes were obtained from Dale Newbury and/or Nicholas Ritchie (I think!), back in 2000 or so (originally created by Chuck Fiori).

There are two versions. The first version was a text file called MASTER.LIN. It contains 4985 (1st order) emission lines, along with absorption edges. See attachments below. The file MASTER.TXT has a description of the data. Here is what it says:

This data base contains 4985 entries and includes all the measurable

X-ray lines, satellites and absorption edges from under 100 eV to

over 120 keV. Additionally, most of the X-ray lines and satellites

are assigned a relative intensity (relative to the alpha-1 line in

each family). The data base was assembled primarily from four

sources:

1.) B.L. Doyle, W.F. Chambers, T.M. Christensen, J.M. Hall and G.H.

Pepper "SINE THETA SETTINGS FOR X-RAY SPECTROMETERS", Atomic Data and

Nucleur Data Tables Vol. 24, No 5, 1979.

2.) E.W. White, G.V. Gibbs, G.G. Johnson Jr. and G.R. Zechman "X-RAY

WAVELENGTHS AND CRYSTAL INTERCHANGE SETTINGS FOR WAVELENGTH GEARED

CURVED CRYSTAL SPECTROMETERS" Report of the Pennsylvania State Univ.,

1964.

3.) J.A. Bearden "X-RAY WAVELENGTHS AND X-RAY ATOMIC ENERGY LEVELS"

Rev. Mod. Phys., Vol. 39, No. 78, 1967.

4.) J.A Bearden and A.F. Burr,"REEVALUATION OF X-RAY ATOMIC ENERGY

LEVELS", Rev. Mod. Phys., Vol. 31, No. 1, 1967.

Each X-ray line or edge series as a function of atomic number was fit

to a fourth degree polynomial. The fit was subtracted from the

appropriate data and the residuals plotted and examined. In this way

rogue entries could be identified and corrected. The resulting data

base is considered to be sufficiently accurate for any application

involving the Si(Li) X-ray detector and single crystal wavelength

spectrometers.

The data base is comprised of three data files: MASTER.LIN,

MASTER.TRS, and MASTER.ENG. These three files are identical except

that they have been sorted in different ways. MASTER.LIN is sorted

such that all entries belonging to a particular transition such as

KA2 are grouped together in ascending atomic number. MASTER.TRS is

sorted in such a manner that all the lines and edges associated with

a particular element are grouped together. These groups are in

ascending atomic number. And finally, MASTER.ENG is sorted in

ascending wavelength in Angstrom units.

Each data file is organized in the following manner: The first column

contains the atomic number and the second contains the atomic symbol.

The third column is the transistion or edge. Where possible the

transition is given in Siegbahn notation. If the entry is an

absorption edge the forth column contains the letters ABS, otherwise

the column is blank. the fifth column contains the wavelength in

Angstrom units. The sixth column contains the relative transition

probability expressed as a percentage of the principal line within

each family ie K, L or M alpha 1. Absorption edge entries contain the

value zero for this column with the anticipation of a future

inclusion of jump ratios. Finally, the last column gives a code for

the source of the entry. If the column is blank the source is

reference 2. If the column contains the letter "C" the source is

reference 1. If the letters "BB" appear, the source is reference 4.

The letters "W,F" mean that reference 2 was used but the relative

transition probability has been adjusted by Fiori. Reference 3 was

used as a check since it is the source of many of the entries of

reference 1.

In column 3 the notation KA1,2 means the entry is the weighted sum of

the KA1 and KA2 in the ratio 2 to 1. For low atomic number the

entries are not self consistent since the data is from different

sources. If the column begins with the capital letter S then the

entry is a satelite line due to doubly ionized atoms. The relative

transition values for these entries are only valid for electron

excited specimens, and are, at best, estimates.

For more information call Chuck Fiori (301-496 2599) or write to me

at Rm 3W-13 Bldg. 13, National Institutes of Health, Bethesda, Md.

20205. In any event, if you find this data useful please keep in

contact since we plan to write our work up formally and will no doubt

update and improve what is in the present files.

Th following are Siegbahn to shell-transition notation conversions:

You will have to use your imagination to discover which arabic letters

we used to correspond to the Siegbahn Greek notation:

KA =KA1+KA2+KA3

KA1,2=(2*KA1+KA2)/3

KA1 =K-L3

KA2 =K-L2

KA3 =K-L1

KB =SUM(KBn)

KBX =Metal

KB1 =K-M3

KB1' =KB1+KB3+KB5

KB2 =(K-N3)+(K-N2)

KB2' =K-N3

KB2''=K-N2

KB3 =K-M2

KB4 =(K-N4)+(K-N5)

KB5 =(K-M4)+(K-M5)

KB5' =K-M5

KB5''=K-M4

Kd1 =K-O3

Kd2 =K-O2

LA =LA1+LA2

LA1 =L3-M5

LA2 =L3-M4

LB1 =L2-M4

LB10 =L1-M4

LB15 =L3-N4

LB17 =L2-M3

LB2 =L3-N5

LB3 =L1-M3

LB4 =L1-M2

LB5 =(L3-O4)+(L3-O5)

LB6 =L3-N1

LB7 =L3-O1

LB9 =L1-M5

LG1 =L2-N4

LG11 =L1-N5

LG2 =L1-N2

LG3 =L1-N3

LG4 =L1-O3

LG4' =L1-O2

LG6 =L2-O4

LG8 =L2-O1

Ll =L3-M1

Ln =L2-M1

Ls =L3-M3

Lt =L3-M2

Lu =(L3-N6)+(L3-N7)

Lv =L2-N6

MA1 =M5-N7

MA2 =M5-N6

MB =M4-N6

MG =M3-N5

MG2 =M3-N4

MZ1 =M5-N3

MZ2 =M4-N2

Md =M2-N4

Me =M3-O5

Eventually we discovered that a number of Mz and Mg lines were missing from Chuck's original table and so Nicholas Ritchie created a new table which is also attached below. This table has 5713 emission lines, but no absorption edges.

But I don't have any documentation of this newer table, though Nicholas can help I am sure.

Finally, I attach below the XRAY.ELM file which is a text file I generated back in 2006, with all these lines and edges, and also higher order reflections with "nominal" intensities.

Hope this helps.