CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


Fe III d - VERSION 6.0


Here you find various information on the brightest lines, ordered in wavelength:
Wavelengths (Angstroms); weighted oscillator strengths (gf); transition probabilities (A); intensities (normalised) at 106 , 1010, 1015, 1020 cm-3; together with:
Configuration; Term; Index of the level (1=ground); Energy (observed if available - otherwise theoretical); of the lower (l) and upper levels (u)
Note that intensities have been calculated at log T[K]=4.80, where the ion fraction peaks in ionization equilibrium. Only lines brighter than 0.001 the strongest line (at all densities) are retained.


Wavelength

gf

Aul

R

R

R

R

Cl

Tl

Cu

Tu

Il

Iu

El

Eu

(A)

(s-1)

(106)

(1010)

(1015)

(1020)

(cm-1)

(cm-1)

1.7547 1.40e-01 2.76e+13 -NaN -NaN -NaN -NaN 3p5.3d6.4s 7F12/2 1s.3d6.4s 7D10/2 2 46 444428.21 57437709

Created by Giulio Del Zanna on Fri Sep 4 09:45:44 2009