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J/A+AS/113/237 Ultraviolet Spectrum of the Sun (Samain, 1995) ================================================================================ 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) ================================================================================ 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: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table3 82 660 Observed wavelengths, laboratory values and identifications -------------------------------------------------------------------------------- Byte-by-byte Description of file: table3 -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 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) -------------------------------------------------------------------------------- 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 -------------------------------------------------------------------------------- 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. -------------------------------------------------------------------------------- ================================================================================ (End) Simona Mei [CDS] 08-Jun-1995