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J/A+A/324/435   Chemical composition of six K supergiants in the SMC (Hill 1997)

Chemical composition of six K supergiants in the Small Magellanic Cloud. Hill V. <Astron. Astrophys. 324, 435 (1997)> =1997A&A...324..435H (SIMBAD/NED BibCode)
ADC_Keywords: Stars, supergiant ; Abundances Keywords: stars: abundances - stars: supergiants - galaxies: Magellanic Clouds - galaxies: abundances Abstract: A sample of six SMC cool stars (K supergiants) are analysed by high resolution spectroscopy in order to investigate their chemical content, which should reflect that of the current interstellar medium within the SMC. The abundance of Na, Al, α-elements, Fe peak and heavy elements are derived through an LTE analysis of the lines, compared to a Galactic "standard" (the well-studied K giant Arcturus) and discussed in terms of chemical evolution of the SMC. The following results were obtained: 1. All the stars from this sample are metal deficient ([Fe/H] ranges from -0.59 to -0.89dex). The abundance varies little from star-to-star (0.10dex rms, comparable with the expected error due to uncertainties on the effective parameters of the stars), in agreement with the very small chemical composition variations among the H II regions within the SMC found by Pagel et al. (1978MNRAS.184..569P). 2. Sodium is not strongly enhanced in these stars, and the star-to-star scatter is larger than expected. 3. At variance with metal-poor stars in our Galaxy, the so-called α-elements do not seem to be enhanced. 4. Nickel displays a noticeable depletion with respect to iron ([Ni/Fe]≃-0.3dex), at variance with what is found in the SMC F supergiants and in Arcturus. 5. Except for PMMR 144, the s and r process elements heavier than Ba are enhanced in all of our stars by ≃+0.4dex. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 00 48.8 -73 28 PMMR 23 = SkKM 36 00 49.2 -73 14 PMMR 27 = SkKM 43 00 51.9 -72 12 PMMR 48 = SkKM 79 00 59.8 -72 21 PMMR 102 = SkKM 191 01 03.3 -72 07 PMMR 144 = SkKM 250 01 03.3 -72 40 PMMR 145 = SkKM 248 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file appen 109 185 Lines used in the analysis
Byte-by-byte Description of file: appen
Bytes Format Units Label Explanations
2- 8 F7.2 0.1nm Lambda Central wavelength of the line 10- 11 A2 --- Element Name of the element 12 I1 --- n_Element [1/2] Degree of ionization 1 for neutral, 2 for ionized species 14- 17 F4.2 eV Pext Excitation potential of the line 20- 24 F5.2 --- log(gf) ? Line transition probability in log scale 27- 31 F5.1 0.1pm EW23 ? Equivalent width of the line for star PMMR23 32 A1 --- n_EW23 [*] Note (1) 34- 38 F5.2 [Sun] [X/H]23 ? Abundance ([X/H]) for PMMR23 41- 45 F5.1 0.1pm EW27 ? Equivalent width of the line for star PMMR27 46 A1 --- n_EW27 [*] Note (1) 48- 52 F5.2 [Sun] [X/H]27 ? Abundance ([X/H]) for PMMR27 55- 59 F5.1 0.1pm EW48 ? Equivalent width of the line for star PMMR48 60 A1 --- n_EW48 [*] Note (1) 62- 66 F5.2 [Sun] [X/H]48 ? Abundance ([X/H]) for PMMR48 69- 73 F5.1 0.1pm EW102 ? Equivalent width of the line for star PMMR102 74 A1 --- n_EW102 [*] Note (1) 76- 80 F5.2 [Sun] [X/H]102 ? Abundance ([X/H]) for PMMR102 83- 87 F5.1 0.1pm EW144 ? Equivalent width of the line for star PMMR144 88 A1 --- n_EW144 [*] Note (1) 90- 94 F5.2 [Sun] [X/H]144 ? Abundance ([X/H]) for PMMR144 97-101 F5.1 0.1pm EW145 ? Equivalent width of the line for star PMMR145 102 A1 --- n_EW145 [*] Note (1) 104-108 F5.2 [Sun] [X/H]145 ? Abundance ([X/H]) for PMMR145
Note (1): Asterisks means that the corresponding abundance was determined by fitting the line profile rather than using this equivalent width, due to a severe blend or to the hyperfine structure of the line.

(End) Patricia Bauer [CDS] 27-Sep-1996
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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