sox22tem:	basic analysis tool to obtain single Te and volume EM with iron ion fractions of H/He and Li/He as free parameters. Iron abundance is adopted to be [Fe/H] = 7.4 (Scott et al., 2015)

wav_cal:	optimize spectral wavelength scale for integrated time span

wav_cal1: 	re-calibrate SOX1 wavelength scale using FeXXVI Lyƒ¿, if exists, and FeXXV w line locations

lsf_7p:	least square fit to quadratic equation

fbd_jd:	routine to estimate single Te and iron ion fractions H/He Li/He via method of Bely-Dubau et al. (1981) 

add_lp:  adding profiles of lines missing in CHIANTI* line list to synthetic spectrum created by make_chianti_spec procedure (in CHIANTI* software package)


save-file database:

ch_ss_int_f7MN.genx:  structure for iron line data derived by ch_ss procedure (in CHIANTI* software package). MN represents; log Te = 7.MN (MN = 10 ~ 70).

fe_ioneq.sav: 	     Iron ion fraction against temperature created from CHIANTI.ioneq file

slines.sav: 	     excitation & recombination rates for lines w, x, y z, j, and q (Bely-Dubau et al., 1981), and intensity ratios for lines around FeXXVI Lyƒ¿ wavelength region

*CHIANTI�@- http://www.chiantidatabase.org/
CHIANTI consists of a critically evaluated set of atomic data, that together with a set of user-friendly Interactive Data Language (IDL) and Python programs can provide diagnostic information from observed emission line spectra of astrophysical plasmas.

References:
Bely-Dubau, F., Dubau, J., Faucher, P., and Gabriel, A. H.: 1982, Mon. Not. Roy. Astron. Soc. 198, 239 - 254.
Scott, P. et al.: 2015, AA, 573, A26.