We would like to announce the release of Version 2.0 of the CHIANTI
database for astrophysical spectroscopy. The additions and corrections
to the database have been described in a paper `CHIANTI - an atomic
database for emission lines, III - Continuum radiation and extension of
the ion database' by E. Landi, M. Landini, K.P. Dere, P.R. Young, H.E.
Mason and has been published in Astronomy and Astrophysics Supplement
Series, 135, 339 ,1999, (Paper III). The new material is described
below but the primary goal of this release is to provide atomic data
for many of the minor elements.
The best way to access CHIANTI is through our WWW page:
*** PLEASE NOTE ***
The new tar files include a new version of the procedure
'read_ioneq.pro' which will be put in the !xuvtop/pro directory. If
this is not your standard CHIANTI IDL procedures directory, it should
be moved to that directory. We had not intended to change any of the
procedures at this time but this was unavoidable.
Also, since we no longer distribute the .elvl files, which are made
redundant by the .elvlc files, it is necessary to download Version 1.03
of the CHIANTI IDL procedures in the unix compressed tar file
CHIANTI_1.03_pro.tar.Z. The updated programs no longer search for the
.elvl files. This is an incremental update of the CHIANTI IDL
procedures. One nice feature of Version 1.03 is that by typing the
name of a procedure, while in IDL, it's correct calling sequence is
New data includes the minor elements Na, P, Cl, K, Ti, Cr, Mn, Co and Zn as
discussed by Landi and Landini, 1999, A&ASS, 133, 411.
- Updates by iso-electronic sequence are as follows:
- Beryllium sequence
- Ne VII: new R-matrix calculations of Ramsbottom
- Mg IX: new A values from SUPERSTRUCTURE calculations
- S XIII, Ar XV, Ca XVII, Fe XXIII, Ni XXV: n=3 levels now included
- Boron sequence
- O IV: a collision strength affecting the lines at 608.397A and
609.829A has been corrected.
- Ca XVI: a missing collision strength included
- Carbon sequence
- Al VIII, Ni XXIII: now included
- Si IX: R-matrix calculations of Aggarwal used for ground transitiions
- Nitrogen sequence
- Ne IV: new R-matrix calculations of Ramsbottom
- Mg VI: new Distorted Wave calculations of Bhatia and Young
- Al VII, Ni XXII: now included
- Fe XX: now includes 72 levels through n=3 from the DW calculations of Bhatia (1989)
- Ni XXII: is not included (contrary to Paper III) because the
interpolation was not considered reliable
- Zn XXIV: data are included (contrary to Paper III)
- Oxygen sequence
- Al VI: now included
- Fluorine sequence
- Al V: now included
- Aluminum sequence
- Ni XVI: DW calculations of Bhatia and Doschek (1998)
- Sulphur sequence
- Fe XI: model refined
- Ni XIII: DW calculations of Bhatia and Doschek (1998)
- Chlorine sequence
- Fe X: model refined
- Ni XII: R-matrix calculations of Matthews et al (1998)
- The references in the elemental abundance file feldman.abund has been
- Ionization equilibria
- The new ionization equilibria calculations of Mazzotta et al. 1998,
A&ASS, 133, 403 have been included (mazzotta_etal.ioneq)
- Other ionization equilibria calculations included:
- - the calculations of Arnaud and Rothenflug, 1986, A&AS, 60, 425.
- - the calculations of Arnaud and Rothenflug plus those of Landini
and Monsignori Fossi, 1991, A&AS, 91, 183 for the minor elements
- - the calculations of Arnaud and Rothenflug plus those of Arnaud
and Raymond, 1992, ApJ, 398, 39 for the Fe ions.
- - the same as arnaud_raymond.ioneq plus those of Landini and Monsignori Fossi for the minor elements
- - calculations of Shull and van Steenberg, 1982, ApJSS, 48, 95
- Differential Emission Measures
- We have found the the DEM file for the quiet sun (quiet_sun.dem) is
characteristic of a more active sun and have renamed this
'quiet_sun_old.dem' and have replaced this with a new file
'quiet_sun.dem' derived from the OSO-6 quiet sun spectra of Dupree.
- It should be noted that many of the differential emission measures
were derived with the coronal abundances of meyer. Consequently,
using these DEMs with other abundance sets could be inappropriate
and produce misleading intensities.
The continuum procedure will soon be adapted to the CHIANTI formats and
will be released soon in an update to the CHIANTI IDL procedures. We
are currently working to complete the database at X-ray wavelengths in
time for the launch of AXAF.
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
If you find any problems, please let us know.