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CHIANTI: A Database for Astrophysical Emission Line Spectroscopy

CHIANTI: What's new in Version 3.01?

We would like to announce the release of Version 3.0 of the CHIANTI database for astrophysical spectroscopy. This now extends the database to include the 1 - 50 Å wavelength region. The additions to the database are described in a paper `CHIANTI - an atomic database for emission lines, IV - Extension to X-ray Wavelengths' by K.P. Dere, E. Landi, G. Del Zanna, and P.R. Young and has been submitted to the Astrophysical Journal Supplement Series. The new material is described below. Version 3.01 corrects a few mistakes found in the original release of Version 3.0.

The best way to access CHIANTI is through our WWW page:

http://wwwsolar.nrl.navy.mil/chianti.html

*** PLEASE NOTE ***

If you already have a previous version of CHIANTI, it is necessary to download both the new data files and the new set of IDL procedures to run Version 3. In order to include dielectronic satellite lines, it has been necessary to modify our general procedures for calculating line intensities. Consequently, the new data set is not compatible with the old procedures and vice versa.

Also, if you use the Solar Softree, it is possible that the IDL routines distributed by the Solar Softree have not been immediately updated and there is the possibility of interference between the old routines and the new Version 3 routines now available at the CHIANTI web page.

Atomic Data Updates

The updates contained in Version 3.0 of CHIANTI are primarily concerned with extending its coverage to include the 1 - 50 Å wavelength region. The inclusion of emission lines from the hydrogen and helium isoelectronic sequences and their satellite line and improved models of highly ionized iron (Fe) ions are the principal ingredients for achieving this. Below, we list the newly included ions and the ions which have been modified for improved X-ray coverage.

Updates by iso-electronic sequence are as follows:
Hydrogen sequence: C VI, N VII, O VIII, Ne X, Na XI, Mg XII, Al XIII, Si XIV, S XVI, Ar XVIII, Ca XX, Fe XXVI, Ni XXVIII
Helium sequence (including satellites to the hydrogen-like lines): C V, N VI, O VII, Ne IX, Na X, Mg XI, Al XII, Si XIII, S XV, Ar XVII, Ca XIX, Fe XXV, Ni XXVII
Lithium sequence satellites to the helium-like lines: C IV, N V, O VI, Ne VIII, Na IX, Mg X, Al XI, Si XII, S XIV, Ar XVI, Ca XVIII, Fe XXIV, Ni XXVI
Lithium sequence with inner-shell excitations: O VI, Ne VIII, Mg X, Al XI, Si XII, S XIV, Ar XVI, Ca XVIII, Fe XXIV, Ni XXV
Other dielectronic satellites to helium-lines: Fe XXI, Fe XXII, Fe XXIII
Beryllium sequence: Mg IX: R-matrix collision strengths included
Carbon sequence: N II, O III, Ne V, Na VI, Mg VII: transition probabilities updated; Fe XXI: atomic model now includes n=4 and n=5 levels
Oxygen sequence: Ne III, Na IV, Mg V: transition probabilities updated
Neon sequence: Ar IX, Ca XI, Fe XVII and Ni XIX: n=4 levels now included
Aluminum sequence: Si II: radiative data updated; S IV: radiative data updated and collision strengths to n=4 included; Fe XIV: radiative and collisional data updated
Silicon sequence: S III: radiative and collisional data updated; Fe XIII: R-matrix collision strengths included for most transitions
Sulphur sequence: Fe XI: R-matrix collision strengths within the ground configuration included
Chlorine sequence: Fe X: n=4 and n=5 levels included
Calcium sequence: Fe VIII: major update of radiative and collisional data

CHIANTI IDL Procedures Updates

Procedures for calculating the continuum due to free-free (bremsstrahlung) and free-bound (radiative recombination) are now included. Their names are 'FREEFREE' and 'FREEBOUND', respectively. A procedure ('RAD_LOSS') calculates the total radiative loss rate as a function of temperature for specified set of abundances and/or ionization equilibria.

One nice feature initiated in Version 1.03 is that by typing the name of a procedure, while in IDL, it's correct calling sequence is returned.

We have also rename some of the utility procedures ('ch_...') so that they don't conflict with IDL procedures distributed with the Solar Soft-Tree.

The continued development of the CHIANTI database is dependent on continued funding which is generally available if we can demonstrate that the CHIANTI database is of use to astrophysical research. If you find CHIANTI useful, it would be helpful to us if you could email a short description (a single sentence is fine) of how you employ CHIANTI. We are also aware that CHIANTI data is being ingested into other databases and this is fine. However, it would be useful for us if some acknowledgement of this use of CHIANTI can be given, such as in publications etc.

If you find any problems, please let us know.

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