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J/A+AS/113/237 Ultraviolet Spectrum of the Sun (Samain, 1995)
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A High Spectral Resolution Atlas of the Balloon Ultraviolet Spectrum
of the Sun: 1950-2000 Angstroems
Samain D.
<Astron. Astrophys. Suppl. Ser. 113, 237 (1995)>
=1995A&AS..113..237S (SIMBAD/NED BibCode)
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Keywords: Sun: UV radiation - atmospheric effects - Sun: atmosphere -
lines: identification
Description:
An ultraviolet atlas of the solar spectrum with a spectral resolution
of 15mA in the region 1948-2000A is presented. It is the first part of
the spectra recorded on the quiet Sun between 1900 and 2130A.
Measurements were performed from a balloon-borne instrumentation flown
at an altitude of 39km. The wavelength atlas with a list of about 550
lines has been synthesized from data at center of the Sun ({mu}=1) and
at {mu}=0.89, smoothed out over an area of 30 arcsec.
The wavelength scale is given with respect to the average solar
spectrum. Tracings are presented at {mu}=0.89, with an intensity scale
adjusted in absolute values on the level of the continuum near 2000A.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3 82 660 Observed wavelengths, laboratory values
and identifications
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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- 3 I3 --- SpOrd Spectrum order
5- 12 F8.3 0.1nm SolLam Wavelength determination of all solar and
telluric lines measurable on the spectrum (1)
13 A1 --- n_SolLam See Note (2)
17 I1 --- Intens []? Intensity of the line in an arbitrary
scale from 0 to 9 (3)
18 A1 --- n_Intens When '?' uncertain value
20- 28 A9 --- Type Acronyms for the type of line (4)
33- 44 A12 --- Identif Possible element responsible for the
observed line (5)
49- 62 A14 0.1nm LabLam Laboratory wavelength
64- 65 A2 --- n_LabLam [St] When 'St' the line is used or
recommended as reference wavelength standard
67- 70 A4 --- r_LabLam References of the wavelength sources (6)
75- 80 F6.3 0.1nm DLam []? Difference between the observed
wavelength and the laboratory wavelength:
dlambda=lambda(Sun or O2) - lambda(lab)
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Note (1): All wavelengths are given in the vacuum, according to usage
below 2000 A. As underlined in the A&A publication, an average
shift of 7mA is to be added to the measured value of the telluric
lines for a proper comparison with their laboratory wavelengths.
Note (2): When 'a' these lines correspond to features not separated in the
observed spectrum. When we tried to take these wavelengths as
references in the wavelength tabulation, we have compared the average
measured wavelength to the arithmetic average of the two laboratory
wavelengths.
Note (3): Approximately representing the degree of absorption at the center of
the line with respect to the intensity level outside of the line; 0
is a line barely detectable.
Note (4): W: wide line(50-100mA)
VW: very wide line(>100mA)
b: blend
d: double line
e: emission line
T: terrestrial O2 line(no indication = solar line)
T*: terrestrial O2 reference line
S*: solar reference line
(S*)/(T*): solar/telluric reference line ejected
Note (5): Laboratory lines whose wavelength differences with our solar
determinations are not lower than 10 m, have not been retained
generally, unless the laboratory uncertainty exceeds that value
or the feature observed is very wide. In the case of telluric
lines, whose features listed here are all due to O2, notation of
the transition is given instead of the name of the element. To point
out the disturbed regions of the solar spectrum, we have reported all
the laboratory wavelengths of known lines belonging to the O2
Shuman-Runge system and encompassed by the spectral interval
1948-2000. However, for many weak lines (like the bands 5-1 and 4-1)
correspondence with observed values in the atlas is often given only
for the record.
Note (6): J: Junkes et al., 65
K: Kelly, 87
KE: Kaufman & Edlen, 74
KRA: Kaufman et al., 66
M: Moore, 62
MCA: MacCabe & MacAllister, 82
R: Radziemski et al., 67
WA: Wilkinson & Andrew, 63
WS: Weeks & Simpson, 67
Y: Yoshino et al., 84
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References:
Junkes J., Salpeter E.W., Milazzo G. 1965, Atomic spectra in the vacuum
ultraviolet, Part one (Specola Vaticana, Citta del Vaticano)
Kaufman V., Edlen B. 1974, J. Phys. Chem. Ref. Data 3, 825
Kaufman V., Radziemski L.J. Jr., Andrew K.L. 1966, J. Opt. Soc. Am. 56, 911
Kelly R.L. 1987, Atomic and ionic spectrum lines of hydrogen through krypton,
J. Phys. Chem. Ref. Data, Vol. 16, Suppl. 1
MacCabe M.K., McAllister H.C. 1982, ApJS 48, 437
Moore C.E. 1962, An Ultraviolet Multiplet Table, N.B.S., Circ. 488, Sec. 4,
1-65
Radziemski L.J. Jr., Andrew K.L., Kaufman V., Litzen, U. 1967, J. Opt. Soc.
Am. 57, 336
Weeks D.W., Simpson E.A. 1967, Absorption spectrum of iron in the vacuum
ultraviolet 2950-1588 A, Harvard College Obs., Sci. Report. no 19
Wilkinson P.G., Andrew, K.L. 1963, J. Opt. Soc. Am. 53, 710
Yoshino K., Freeman, D.E., Parkinson W.H. 1984, J. Phys. Chem. Ref. Data
13, 207.
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(End) Simona Mei [CDS] 08-Jun-1995