CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


Cr XVI - VERSION 11.0.1


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]=6.70, 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)

106.6170 2.44e-01 7.14e+10 1.00e+00 1.00e+00 1.00e+00 1.00e+00 2s2.2p5 2P3/2 2s.2p6 2S1/2 1 3 0 937940
115.3340 1.10e-01 2.76e+10 3.57e-01 3.57e-01 3.57e-01 3.57e-01 2s2.2p5 2P1/2 2s.2p6 2S1/2 2 3 70892 937940
1410.5959 0.00e+00 6.00e+03 7.79e-02 7.78e-02 6.43e-04 1.46e-08 2s2.2p5 2P3/2 2s2.2p5 2P1/2 1 2 0 70892

Created by Giulio Del Zanna on Wed Apr 16 17:42:44 2025