CHIANTI - an atomic database for emission lines*
I. Wavelengths greater than 50 Å
Naval Research Laboratory, Washington DC, U.S.A.
2 Department of Astronomy and Space Science, University of Florence, Italy
3 Department of Applied Mathematics and Theoretical Physics, University of Cambridge, UK
4 Arcetri Astrophysical Observatory, Florence, Italy
Send offprint request to: K.P. Dere
Accepted: 5 November 1996
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.
Key words: atomic data / astronomical data bases: miscellaneous / ultraviolet: general / Sun: atmosphere / stars: atmosphere
Table 3 only available in electronic form at CDS via anonymous ftp to cdsarc.u.strasbg.fr (184.108.40.206) or via http://cdsweb.u-strasbg.fr/Abstract.html
© European Southern Observatory (ESO), 1997