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J/A+AS/126/281      Solar disk spectrum (660-1175A)                (Curdt+ 1997)
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The solar disk spectrum between 660 and 1175 A.
(First Order) obtained by SUMER on SOHO
       Curdt W., Feldman U., Laming J.M., Wilhelm K., Schuehle U., Lemaire P.
      <Astron. Astrophys. Suppl. Ser. 126, 281 (1997)>
      =1997A&AS..126..281C      (SIMBAD/NED BibCode)
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ADC_Keywords: Sun ; Spectra, ultraviolet
Mission_Name: SOHO
Keywords: Sun: atmosphere - chromosphere - transition region - UV radiation

Description:
    The near-limb quiet-Sun spectrum recorded on January 25, 1996 near the
    solar North pole is presented in tabular form and in graphical form.
    Table 1 - the line list - lists all lines found in the spectrum
    providing absolute peak intensities, measured and literature
    wavelengths, identification, and classification of the transition.
    Fig. 4 is a display the composite spectrum. The most prominent lines
    are labelled. In this figure intensities are given in instrumental
    units and logarithmic scale.

File Summary:
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  FileName        Lrecl  Records   Explanations
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ReadMe             80        .   This file
table1.dat        104      496  *Line list
table1.tex         83     1072   LaTeX version of table1
fig4.ps           109     1624  *Composite spectrum
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Note on table1.dat: 
    This list of spectral lines in the 660-1175{AA} wavelength range
    including some 2nd order lines below 590{AA} was compiled from a
    spectrum which was recorded with detector B on the solar disk near the
    north limb. It was generated from a number of sections recorded on the
    KBr photocathode each about 20{AA} wide, and complemented by bare
    photocathode lines at the lower wavelength limit.
Note on fig4.ps: 
    The most prominent lines are labelled. In this figure
    intensities are given in instrumental units and logarithmic scale.
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Byte-by-byte Description of file: table1.dat
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   Bytes Format     Units       Label      Explanations
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   1-  4  I4    10mW/m2/sr/nm   Peak       ? Peak intensity (1)
       5  A1        ---       n_Peak       [)] Note on peak
   7- 17  A11       0.1nm       lambda     ? wavelength (literature) (2)
  18- 24  F7.2      0.1nm       lambdaObs  ? wavelength as observed (3)
      25  A1        ---       n_lambdaObs  [*] Note (4)
  27- 35  A9        ---         Ion        Ion or atom
  37- 60  A24       ---         Transu     Transition, upper level
      62  A1        ---         ---        [-] dash
  64- 85  A22       ---         Transl     Transition, lower level
  87- 88  A2        ---         bl         [p n] Blend (5)
  90-109  A20       ---         Rem        Remarks (6)
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Note (1): The continuum background is not subtracted. These entries have been
           corrected for the instrument spectral response by applying the
           radiometric calibration. Intensities of EUV lines in the upper solar
           atmosphere changes on short time scales. Since the various parts of
           the spectrum were not recorded simultaneously, the numbers in the
           first column should be used only as rough indications to the relative
           strengths of the particular transition. Blends normally have no
           intensity (or wavelength measurement entry) except for some cases
           where they could partially be separated. The same applies for members
           of the Lyman series since their line shape is strongly affected by
           the self-absorption. Blends are indicated in bl column.
Note (2): Wavelengths are mostly from the compilation by 
           R.L. Kelly (1987, J. Phys. Chem. Ref. Data 16, 1).
           For lines with blends more than one wavelength is given, including
           unresolved lines if there is evidence (e.g. from the second order
           spectrum) that they may contribute to some extent.
Note (3): The wavelengths were obtained by averaging measurements from two
           different detector recordings. Lines without identification are
           included as well and indicated by a '?'
Note (4): *: Lines taken as reference lines for the wavelength calibration.
Note (5): p: blended with preceding line
          n: blended with next line
Note (6): Questionable identifications are marked by a '?'
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Acknowledgements: Werner Curdt <CURDT@linsu1.mpae.gwdg.de>
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(End)                                         Patricia Bauer [CDS]   24-Apr-1997