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A&A Supplement Series, Vol. 125, October I 1997, 149-173

Received July 24; accepted November 5, 1996

CHIANTI - an atomic database for emission lines

I. Wavelengths greater than 50 Ågif

K.P. Dere tex2html_wrap3520 - E. Landi tex2html_wrap3522 - H.E. Mason tex2html_wrap3524 - B.C. Monsignori Fossi tex2html_wrap3526 - P.R. Young tex2html_wrap3524

Send offprint request: K.P. Dere

tex2html_wrap3530  Naval Research Laboratory, Washington DC, U.S.A.
tex2html_wrap3532  Department of Astronomy and Space Science, University of Florence, Italy
tex2html_wrap3534  Department of Applied Mathematics and Theoretical Physics, University of Cambridge, UK
tex2html_wrap3536  Arcetri Astrophysical Observatory, Florence, Italy


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 Å has 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.

keywords: atomic data -- astronomical data bases:miscellaneous -- ultraviolet: general -- Sun: atmosphere -- stars: atmosphere

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