J/A+AS/126/281 Solar disk spectrum (660-1175A) (Curdt+ 1997)
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 1997A&AS..126..281C (SIMBAD/NED BibCode)
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 660-1175Å wavelength range
including some 2nd order lines below 590Å 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 20Å 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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See also:
J/A+A/375/591 : SUMER Spectral Atlas of Solar Disk Features (Curdt+, 2001)
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
(End) Patricia Bauer [CDS] 24-Apr-1997