J/A+AS/102/269 Lab. and solar highly-excited levels of Fe I (Nave+ 1993)
Highly-excited levels of Fe I obtained from laboratory and solar Fourier transform and grating spectra. II. Laboratory and solar identifications NAVE G., JOHANSSON S. <Astron. Astrophys. Suppl. Ser. 102, 269 (1993)> =1993A&AS..102..269N
ADC_Keywords: Atomic physics ; Sun Keywords: atomic data - line: identification - infrared: general - ultraviolet: general Abstract: New identifications of about 2200 FeI lines between 170nm and 5µm (59000 to 2000 cm-1) due to highly-excited configurations are presented. These have been observed in hollow cathode lamps using Fourier transform and grating spectroscopy. About 1700 if the lines have been observed in the solar spectrum. A companion paper presents the experimental energy levels. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 104 2199 Fe I lines from 4941.6 to 170.1nm
See also: J/A+A/274/555 : Asymmetry of FeI lines in solar spectrum (Stathopoulou+ 1993) J/A+A/340/300 : Fe II oscillator strengths (Raassen+ 1998) J/A+A/347/348 : Solar abundance of iron (Grevesse+, 1999) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 5 A5 --- Ilab Intensity (laboratory data) (2) 6- 9 I4 0.001cm-1 FWHM ? Full width at half maximum of line in FT spectra (laboratory data) 11- 20 F10.4 0.1nm Lambda [1701/49500]-= Wavelength (laboratory data) Lambda(air) for lambda > 200nm Lambda(vac) for lambda < 200nm 22- 30 F9.3 cm-1 Sigma Wavenumber (laboratory data) 31- 34 I4 0.001cm-1 o-c Difference between observed wavenumber (wavelength below 306 nm) and that derived from the energy levels in paper 1 38- 60 A23 --- Trans Transition designation (5) 63 A1 --- bl. Species of blended line. Lines marked `G' are blended with a ghost. 66- 74 F9.3 0.1nm LamSun ? wavelength in solar spectrum (6) 76- 84 F9.3 cm-1 SigSun ? wavenumber in solar spectrum (6) 86- 90 F5.1 --- Isun ? Intensity (solar data) 93-104 A12 --- Comments Previous identifications (7)
Note (2): Intensity in arbitrary units. These are given as log(I) for FT spectra. Grating intensities are from the continuous hollow cathode spectra, except those in italics, which are from the pulsed hollow cathode spectra. Symbols are: d: diffuse b: blended *: unresolved ?: questionable Note (5): Abbreviated term designations are taken from Sugar & Corliss (1985, J. Phys. Chem. Ref. Data 14 suppl. 2), Brown et al. (1988OSAJB...5.2125B) or are listed in table 1 of paper 1. Note (6): Is specified either as wavelength or wavenumber. Solar data is taken from: Geller (1992 NASA Ref. Publ 1224 vol.III) 2000 cm-1 < sigma < 4788 cm-1 Biemont et al.(1985A&AS...61..107B) 4788 cm-1 < sigma < 8375 cm-1 Delbouille et al.(1981, Kitt Peak) 4788 cm-1 < sigma < 8375 cm-1 Livingston and Wallace (1991, Tucson) 4788 cm-1 < sigma < 8375 cm-1 Swensson et al. (1970sslt.book.....S ; Mem. Soc. R. Sci. Liege 5) 8375 cm-1 < sigma < 11100 cm-1 Pierce & Breckinridge (1975, Kitt Peak) 11100 cm-1 < sigma < 32650 cm-1 Moore et al. (1966, NBS Monograph 61) 11100 cm-1 < sigma < 32650 cm-1 Moore et al. (1982, NRL Report 8653) 32650 cm-1 < sigma < 47500 cm-1 Moore et al. (1992) sigma > 47500 cm-1 Note (7): Previous identification in solar table. Lines between 4788 cm-1 and 8375 cm-1 are marked `P' if a line is present in the atlases of Delbouille et al. (1981, Kitt Peak Obs.) or Livingston and Wallace (1991, Tucson), but is not listed in Biemont et al. (1985A&AS...61..107B) `T' if they are in a region of telluric absorption. The ionization stage is neutral unless otherwise specified.
History: * 31-Jul-2001: added bibcodes, converted "decimal part" of numbers for the solar wavelength / wavenumbers into full numbers.
(End) Patricia Bauer [CDS] 06-Oct-1993
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