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J/A+A/289/740 Galactic abundance gradients (Kaufer+, 1994)
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The galactic abundance gradients traced by B-type stars
Kaufer A., Szeifert T., Krenzin R., Baschek B., Wolf B.
<Astron. Astrophys. 289, 740 (1994)>
=1994A&A...289..740K (SIMBAD/NED Reference)
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ADC_Keywords: Stars, B-type; Spectroscopy; Abundances
Keywords: stars: abundances, early type - Galaxy: abundances, evolution
Abstract:
We obtained high S/N, high resolution spectra of 16 B-type main sequence
stars in young open clusters and in H II regions with galactocentric
distances between 7 and 16 kpc. Chemical abundances for this sample were
derived using line-blanketed Local Thermodynamic Equilibrium (LTE) model
atmospheres and line formation in LTE. Our analyses together with published
data from similar analyses of B-type stars result in flat gradients or even
no gradients at all for oxygen and nitrogen in the outer part of the
galactic disk. It is conjectured that the larger metallicity gradients
cited for H II regions are essentially due to a steepening within the
inner 6 kpc towards the galactic center.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2 49 16 List of the stars
table6 117 43 Measured equivalent width
table7 117 109 Measured equivalent width
table8 125 175 Measured equivalent width
tables.tex 110 518 LaTeX version of tables 6, 7 and 8
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Byte-by-byte Description of file: table2
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Object name
17 I1 --- Ref. Reference (1)
27- 31 F5.2 mag V visual magnitude
41- 44 F4.1 kpc Dgal galactocentric distance
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Note (1):
1: Hoag A.A, Applequist N.L., 1965, ApJS 12, 215
2: Hiltner W.A., 1966, IAU Symp. 24, 373
3: Hoffleit D., Jaschek C., 1982, The Bright Star Catalogue, Yale University
Observatory
4: Mermilliod J.C., 1986, Catalogue of UBV Photometry and MK Spectral Types
in open clusters, Institute d'Astronomie de l'Universite de Lausanne
5: Moffat A.F.J., Vogt N., 1975, A&AS 20, 85
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Byte-by-byte Description of file: table6
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Bytes Format Units Label Explanations
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1- 79 A79 --- Ident. Laboratory wavelengths of the contributing
line components
82- 85 I4 0.1pm NGC6531/2 []? Measured equivalent width for NGC6531/2
90- 93 I4 0.1pm NGC6823/34 []? Measured equivalent width for NGC6823/34
98-101 I4 0.1pm NGC6910/2 []? Measured equivalent width for NGC6910/2
106-109 I4 0.1pm NGC1893/9 []? Measured equivalent width for NGC1893/9
114-117 I4 0.1pm NGC1893/10 []? Measured equivalent width for NGC1893/10
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Byte-by-byte Description of file: table7
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Bytes Format Units Label Explanations
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1- 79 A79 --- Ident. Laboratory wavelengths of the contributing
line components
82- 85 I4 0.1pm HR1763 []? Measured equivalent width for HR1763
90- 93 I4 0.1pm HR1765 []? Measured equivalent width for HR1765
98-101 I4 0.1pm HR1842 []? Measured equivalent width for HR1842
106-109 I4 0.1pm HR1886 []? Measured equivalent width for HR1886
114-117 I4 0.1pm HR1887 []? Measured equivalent width for HR1887
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Byte-by-byte Description of file: table8
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Bytes Format Units Label Explanations
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1- 79 A79 --- Ident. Laboratory wavelengths of the contributing
line components
82- 85 I4 0.1pm hPer/717 []? Measured equivalent width for hPer/717
90- 93 I4 0.1pm hPer/782 []? Measured equivalent width for hPer/782
98-101 I4 0.1pm S247/1 []? Measured equivalent width for S247/1
106-109 I4 0.1pm S301/3 []? Measured equivalent width for S301/3
114-117 I4 0.1pm S217/3 []? Measured equivalent width for S217/3
122-125 I4 0.1pm S208/6 []? Measured equivalent width for S208/6
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Note:
The equivalent widths of the metallic lines and non-diffuse He I lines were
measured interactively by setting the continuum individually for each line
and fitting a gaussian profile.
The equivalent widths of the Balmer lines were measured interactively
by removing strong blend components using a spline fit over the complete
profile. This profile is finally integrated in fixed wavelength intervals
of typically +/-36 Angstroms (expect for S301/3 where the wavelength interval
is +/-30 Angstroms). The diffuse He I lines were measured in the
same way.
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(End) Patricia Bauer [CDS] 03-May-1994