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J/A+A/347/69       Abundances of halo early-type stars        (Rolleston+, 1999)

Early-type stars in the Galactic halo from the Palomar-Green Survey. II: A sample of distant, apparently young Population I stars Rolleston W.R.J., Hambly N.C., Keenan F.P., Dufton P.L., Saffer R.A. <Astron. Astrophys. 347, 69 (1999)> =1999A&A...347...69R (SIMBAD/NED BibCode)
ADC_Keywords: Stars, early-type ; Equivalent widths ; Abundances Keywords: stars: abundances - stars: atmospheres - stars: early-type - stars: kinematics Abstract: We present echelle (R∼40,000) spectroscopic observations for a sample of apparently normal, high Galactic latitude, early-type stars drawn from the Palomar-Green Survey. The metal-line spectra show evidence for rotational velocity broadening with values of vsini≤300km/s. In conjunction with Kurucz model atmospheres, we derive stellar photospheric abundances that are consistent with a Population I chemical composition; differential abundances with respect to Galactic disk Population I stars indicate no abundance differences outside the estimated errors. From a comparison of the derived atmospheric parameters with recent theoretical evolutionary models, we derive distance and age estimates for individual stars. Using kinematical considerations, we conclude that all these objects are `runaway' stars, formed in the Galactic disk and subsequently ejected, possibly by supernovae explosions or dynamical interactions. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 08 58 21.0 +29 12 12 PG 0855+294 09 37 04.0 +14 18 24 PG 0934+145 09 58 14.4 +28 52 26 PG 0955+291 12 07 57.4 +22 31 47 PG 1205+228 22 21 59.1 +09 37 31 PG 2219+094 22 32 08.5 +10 14 25 PG 2229+099 23 48 22.4 +24 23 06 PG 2345+241 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table4.dat 74 17 Equivalent width for the non-diffuse helium and metal lines (PG 0855+294 to PG 2219+094) table5.dat 38 61 Equivalent width for the non-diffuse helium and metal lines (PG 2229+099 and PG 2345+241)
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 7 F7.2 0.1nm Line Wavelength of spectral line 10- 15 A6 --- Species Ionization stage of element 18- 20 I3 0.1pm EW0855 ? Equivalent width for PG 0855+294 22- 26 F5.2 --- A0855 ? LTE abundances for PG 0855+294 in 12+log(X/H) 30- 32 I3 0.1pm EW0934 ? Equivalent width for PG 0934+145 34- 38 F5.2 --- A0934 ? LTE abundances for PG 0934+145 in 12+log(X/H) 42- 44 I3 0.1pm EW0955 ? Equivalent width for PG 0955+291 46- 50 F5.2 --- A0955 ? LTE abundances for PG 0955+291 in 12+log(X/H) 54- 56 I3 0.1pm EW1205 ? Equivalent width for PG 1205+228 58- 62 F5.2 --- A1205 ? LTE abundances for PG 1205+228 in 12+log(X/H) 66- 68 I3 0.1pm EW2219 ? Equivalent width for PG 2219+094 70- 74 F5.2 --- A2219 ? LTE abundances for PG 2219+094 in 12+log(X/H)
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 7 F7.2 0.1nm Line Wavelength of spectral line 10- 15 A6 --- Species Ionization stage of element 18- 20 I3 0.1pm EW2229 ? Equivalent width for PG 2229+099 22- 26 F5.2 --- A2229 ? LTE abundances for PG 2229+099 in 12+log(X/H) 30- 32 I3 0.1pm EW2345 ? Equivalent width for PG 2345+241 34- 38 F5.2 --- A2345 ? LTE abundances for PG 2345+241 in 12+log(X/H)
Acknowledgements: Robert Rolleston References: Hambly et al., Paper I. 1997ApJS..111..419H
(End) Patricia Bauer [CDS] 29-Apr-1999
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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