CHIANTI

An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.


Cl IV - 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]=5.00, 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)

3119.5601 0.00e+00 2.47e+00 3.98e-01 1.00e+00 1.00e+00 1.00e+00 3s2.3p2 3P1 3s2.3p2 1S0 2 5 492 32547.8
3204.5220 0.00e+00 2.62e-02 4.11e-03 1.03e-02 1.03e-02 1.03e-02 3s2.3p2 3P2 3s2.3p2 1S0 3 5 1341.9 32547.8
5324.7568 0.00e+00 2.80e+00 2.64e-01 6.64e-01 6.64e-01 6.64e-01 3s2.3p2 1D2 3s2.3p2 1S0 4 5 13767.6 32547.8
7532.6162 0.00e+00 7.23e-02 4.33e-01 7.99e-02 7.95e-02 7.95e-02 3s2.3p2 3P1 3s2.3p2 1D2 2 4 492 13767.6
8047.8359 0.00e+00 1.79e-01 1.00e+00 1.85e-01 1.84e-01 1.84e-01 3s2.3p2 3P2 3s2.3p2 1D2 3 4 1341.9 13767.6
117660.8984 0.00e+00 8.25e-03 2.90e-02 6.98e-04 6.94e-04 6.94e-04 3s2.3p2 3P1 3s2.3p2 3P2 2 3 492 1341.9
203252.0312 0.00e+00 2.14e-03 3.10e-03 6.37e-05 6.33e-05 6.33e-05 3s2.3p2 3P0 3s2.3p2 3P1 1 2 0 492

Created by Giulio Del Zanna on Wed Apr 16 17:42:36 2025