CHIANTI provides a database of atomic energy levels, wavelengths, radiative
transition probabilities, and electron excitation data for a large number
of ions of astrophysical interest. It also includes a suite of Interactive
Data Language programs to calculate optically thin synthetic spectra and to
perform spectral analysis and plasma diagnostics. This database allows the
calculation of theoretical line emissivities necessary for the analysis of
optically thin emission-line spectra. The first version (1.01) of the CHIA
NTI database was released in 1996 and published by Dere et al. in 1997 as P
aper I in this series. The second version, released in 1999 by Landi et al.
, included continuum emission and data for additional ions. Both versions o
f the CHIANTI database have been used extensively by the astrophysical and
solar communities to analyze emission-line spectra from astrophysical sourc
es. Now the CHIANTI database has been extended to wavelengths shorter than
50 Angstrom by including atomic data for the hydrogen and helium isoelectro
nic sequences, inner-shell transitions and satellite lines, and several oth
er ions. In addition, some of the ions already present in the database have
been updated and extended with new atomic data from published calculations
.