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J/AJ/134/926        Chemical composition of V2314 Oph        (Kim+, 2007)

Chemical composition and differential time-series CCD photometry of V2314 Ophiuchi: a new λ Bootis-type star. Kim C., Yushchenko A.V., Gopka V.F., Dorokhova T.N., Musaev F.A., Kim S.-L., Jeon Y.-B., Ibrahimov M., Tarasov A.E. <Astron. J., 134, 926-933 (2007)> =2007AJ....134..926K
ADC_Keywords: Stars, variable ; Spectroscopy ; Abundances Keywords: stars: abundances - stars: oscillations - stars: individual (V2314 Ophiuchi, SX Phoenicis, delta Scuti, lambda Bootis) Abstract: We investigated V2314 Oph using high-resolution (R=45000) spectral observations. The atmospheric parameters were determined using iron-line abundance analysis. We derived a mean effective temperature of Teff=7510K, mean surface gravity of logg=3.30, metallicity of [Fe/H]=-0.59, and rotation velocity of vsini=38km/s. The abundances of 19 chemical elements were determined. Description: Seven spectra of V2314 Oph were obtained during three nights in 2002 using a coude-echelle spectrometer mounted on the 2m Zeiss telescope at the Peak Terskol Observatory located near Mount Elbrus (Northern Caucasus, Russia), 3124m above sea level. Objects: --------------------------------------------------- RA (2000) DE Designation(s) --------------------------------------------------- 17 44 03.6 +06 03 43 V2314 Oph = V* V2314 Oph --------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 36 168 Iron lines in the spectrum of V2314 Oph table4.dat 85 111 Lines of other elements in the spectrum of V2314 Oph
See also: B/gcvs : General Catalogue of Variable Stars (Samus+ 2007-2009) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 8 F8.3 0.1nm Wave Wavelength in Angstroms 10- 14 A5 --- Ion Iron species 16- 18 I3 0.1pm EW Equivalent width in milli-Angstroms 20- 24 F5.2 [-] log(gf) Log of the oscillator strength 26- 30 F5.3 eV Elow Energy of the low level 32- 36 F5.3 [-] logN Log of the iron number abundance (logH=12)
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 5 F5.2 --- Ion Ion identification code (e.g. FeI = 26.00) 7- 14 F8.3 0.1nm Wave Wavelength in Angstroms 16- 21 F6.3 [-] log(gf) Log of the oscillator strength 23- 28 F6.3 eV Elow Excitation energy 30- 35 F6.3 [-] DlogN Log of abundance difference from solar (2) 37- 41 F5.3 [-] logN Log of V2314 Oph element abundance 43- 47 F5.3 [-] logNSun ? Log of solar element abundance (2) 49- 53 F5.3 --- bld [0,1] Level of synthetic spectrum line blending in V2314 Oph (3) 55- 59 F5.3 --- bldSun [0,1]? Level of synthetic spectrum line blending in Sun (3) 61- 65 F5.3 --- Depth [0,1] Synthetic spectrum line depth in V2314 Oph 67- 71 F5.3 --- DepthSun [0,1]? Synthetic spectrum line depth in Sun 73- 78 F6.3 [-] dlog(gf) Change of log of the abundance for atmosphere model with log(gf) shifted by -0.2dex 80- 85 F6.3 [-] dTeff Change of log of the abundance for atmosphere model with Teff shifted by +100K
Note (2): If the value of solar abundance in the column marked as 'logNSun' is NULL the abundance from Grevesse & Sauval (1998, Space Sci. Rev., 85, 161) is used. Note (3): where 1.0 = clean line, and 0.0 = strongly blended line
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 03-Oct-2009
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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