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J/A+AS/125/149   CHIANTI - An Atomic Database For Emission Lines I. (Dere+ 1997)
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CHIANTI - an atomic database for emission lines.
I. Wavelengths greater than 50 Angstroms
      Dere K.P., Landi E., Mason H.E., Monsignori Fossi B.C., Young P.R.
     <Astron. Astrophys. Suppl. Ser. 125, 149 (1997)>
     =1997A&AS..125..149D      (SIMBAD/NED BibCode)
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ADC_Keywords: Atomic physics
Keywords: atomic data - astronomical data bases: miscellaneous -
          ultraviolet: general - Sun: atmosphere - stars: atmosphere

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 (1992A&A...254..436B). The
    current version is essentially complete for specifying the emission
    spectrum at wavelengths greater than 50{AA}. A list of observed lines
    in the spectral region between 50 and 1100{AA} 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.

File Summary:
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  FileName      Lrecl  Records   Explanations
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ReadMe             80        .   This file
table3             96     1768   A list of observed lines and lines in the
                                  CHIANTI database between 50 and 1100 Angstroms
table3.tex        137     2020   LaTeX version of table3
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Byte-by-byte Description of file: table3
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   Bytes Format Units   Label    Explanations
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   1-  8  F8.3  0.1nm   LamObs   Observed wavelength from literature sources (1)
  10- 17  F8.3  0.1nm   LamCH    ? Wavelength in CHIANTI database
  20- 27  A8    ---     Ion      Ion (spectroscopic notation)
  29- 46  A18   ---     Level1   Description of lower level of transition
      48  A1    ---     ---      [-] Separation dash
  50- 75  A26   ---     Level2   Description of upper level of transition
  77- 83  E7.2 mW/m2/sr Int      ? Predicted intensity of line in a small
                                    solar flare (2)
  86- 94  A9    ---     Ref     Literature sources of observed wavelength (3)
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Note (1): The observed wavelength is given as 0. if there is not report of an
           observed line at the wavelength of a reasonably intense line
           predicted by CHIANTI
Note (2): The intensity is given a 0. if the line is identified but is not
           included in the CHIANTI database.
Note (3): References:
           1:  Acton et al. (1985ApJ...291..865A)
           2:  Behring et al. (1972ApJ...175..493B)
           3:  Behring et al. (1976ApJ...203..521B)
           4:  Dere (1978ApJ...221.1062D)
           5:  Freeman & Jones (1970SPh....15..288F)
           6:  Thomas & Neupert (1994, Cat. <J/ApJS/91/461>)
           7:  Widing & Sandlin (1968ApJ...152..545W)
           8:  Kastner et al. (1974ApJ...191..261K)
           9:  Burton & Ridgeley (1970SPh....14....3B)
          10:  Feldman & Doschek (1991ApJS...75..925F)
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Acknowledgements: Ken Dere <dere@halcyon.nrl.navy.mil>
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(End)                                         Patricia Bauer [CDS]   22-Apr-1997