CHIANTI - an atomic database for emission lines

TLDR

Accurate atomic data are essential for analyzing astrophysical and solar spectra. CHIANTI offers a database of atomic energy levels, wavelengths, radiative and electron excitation data for abundant ions in cosmic plasmas. CHIANTI compiles recent electron excitation data (Burgess & Tully 1992), covers wavelengths >50 Å, compares observed 50–1100 Å lines to predictions, and supplies IDL routines for synthetic spectra and diagnostics, all available via anonymous FTP. The database reproduces most observed lines in the 50–1100 Å range.

Abstract

A comprehensive set of accurate atomic data is required for analyses of astrophysical and solar spectra. CHIANTI provides a database of atomic energy levels, wavelengths, radiative data and electron excitation data for ions which are abundant in cosmic plasmas. The most recent electron excitation data have been assessed and stored following the method of Burgess & Tully (1992). The current version is essentially complete for specifying the emission spectrum at wavelengths greater than 50 Å. A list of observed lines in the spectral region between 50 and 1100 Åhas been compiled and compared with the lines predicted by the CHIANTI database. The CHIANTI database reproduces the vast majority of lines observed at these wavelengths. CHIANTI includes IDL (Interactive Data Language) routines to calculate optically thin synthetic spectra for equilibrium conditions. IDL routines to calculate theoretical line intensities required for electron density or temperature diagnostics and emission measure studies are also included. The CHIANTI atomic database and supporting IDL routines are available by anonymous FTP.