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J/ApJ/652/1554      Iron in hot DA white dwarfs              (Vennes+, 2006)

Iron in hot DA white dwarfs. Vennes S., Chayer P., Dupuis J., Lanz T. <Astrophys. J., 652, 1554-1562 (2006)> =2006ApJ...652.1554V
ADC_Keywords: Stars, white dwarf ; Effective temperatures ; X-ray sources ; Ultraviolet Keywords: stars: abundances - stars: atmospheres - white dwarfs Abstract: We present a study of the iron abundance pattern in hot, hydrogen-rich (DA) white dwarfs. The study is based on new and archival far-ultraviolet spectroscopy of a sample of white dwarfs in the temperature range 30000K≤Teff≤64000K. The spectra obtained with the Far Ultraviolet Spectroscopic Explorer, along with spectra obtained with the Hubble Space Telescope Imaging Spectrograph and the International Ultraviolet Explorer, sample FeIII-FeVI absorption lines, enabling a detailed iron abundance analysis over a wider range of effective temperatures than previously afforded. Description: The FUSE observations were made using the 30"x30" low-resolution slit (LWRS), resulting in 100% throughput and ensuring complete spectral coverage (900Å≤λ≤180Å) with a spectroscopic resolving power R=lambda/δλ=20000+/2000. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table4.dat 37 104 Soft X-ray to EUV count rate ratios
See also: IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1999) IX/29 : ROSAT All-Sky Survey Faint Source Catalog (Voges+ 2000) Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [1RXS] 6- 21 A16 --- 1RXS ROSAT Name (JHHMMSS.s+DDMMSS) 23- 27 F5.2 --- CRRatio Count-rate ratio, C(PSPC)/C(100Å) 29- 32 F4.2 --- e_CRRatio rms uncertainty on CRRatio 34- 37 F4.1 10+3K Teff Effective temperature
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 29-Jul-2008
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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