A High‐Dispersion Spectroscopic Survey of the Hot White Dwarfs: The
                    <i>IUE</i>
                    NEWSIPS SWP Echelle Data Set

Holberg, J. B.; Barstow, M. A.; Sion, E. M.

doi:10.1086/313161

Cited by 82 publications

(124 citation statements)

References 69 publications

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“…The lack of Fe VII lines in the K 1-16 FUSE data supports a result by Holberg et al (1998). They found no evidence of Fe VII lines in (much less meaningful) IUE spectra, contrary to earlier work by Feibelman & Bruhweiler (1990).…”

Section: K 1-16supporting

confidence: 71%

“…Numerous IUE high resolution spectra exist which can be co-added. Holberg et al (1998) find no evidence of the Fe VII lines reported by Feibelman & Bruhweiler (1990). We confirm this result and find that this is due to the high temperature.…”

Section: Ngc 246supporting

confidence: 60%

“…There are two Mg II lines nearby, at 1239.93Å and 1240.39Å. The redshift of the photospheric spectrum (+47.22 km s −1 from Holberg et al 1998, confirmed by our measurement of the C IV 1107.93Å line) and the blueshift of the ISM lines (−2.39 km s −1 ) conspire in a way that the interstellar Mg II 1239.93Å line almost coincides with the position of a possible stellar Fe VII line. The same problem arises in the case of KPD 0005+5106 (see below).…”

Section: Rx J 21171+3412mentioning

confidence: 99%

“…Right panel: models with T eff = 140 000 K/log g = 6.4 (dash-dotted), 150 000/6.5 (dashed) and 160 000/6.6 (solid), and solar iron abundance. A velocity shift of −48.07 km s −1 is taken into account according to Holberg et al (1998). The spectra are smoothed with 0.01Å Gaussians.…”

Section: Model Atmospheres and Synthetic Spectramentioning

confidence: 99%

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Iron abundance in hot hydrogen-deficient central stars and white dwarfs from FUSE, HST, and IUE spectroscopy

Miksa

Deetjen

Kruk³

et al. 2002

A&A

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Abstract. We present a first systematic investigation of the iron abundance in very hot (T eff ≥ 50 000 K) hydrogendeficient post-AGB stars. Our sample comprises 16 PG 1159 stars and four DO white dwarfs. We use recent FUSE observations as well as HST and IUE archival data to perform spectral analyses with line blanketed NLTE model atmospheres. Iron is not detected in any PG 1159 star. In most cases this is compatible with a solar iron abundance due to limited quality of HST and IUE data, although the tendency to an iron underabundance may be recognized. However, the absence of iron lines in excellent FUSE spectra suggests an underabundance by at least 1 dex in two objects (K 1-16, NGC 7094). A similar result has been reported recently in the [WC]-PG 1159 transition object Abell 78 . We discuss dust fractionation and s-process neutron-captures as possible origins. We also announce the first identification of sulfur in PG 1159 stars.

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Section: K 1-16supporting

confidence: 71%

Section: Ngc 246supporting

confidence: 60%

Section: Rx J 21171+3412mentioning

confidence: 99%

Section: Model Atmospheres and Synthetic Spectramentioning

confidence: 99%

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Iron abundance in hot hydrogen-deficient central stars and white dwarfs from FUSE, HST, and IUE spectroscopy

Miksa

Deetjen

Kruk³

et al. 2002

A&A

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“…-Strong detections of photospheric material in both IUE (e.g. Holberg et al 1998) Table 3, but the weaker (at ~50 km s -1 ) is seen only in C II. Photospheric C III, Si IV and S IV are detected at 13.8 km s -1 .…”

Section: Wd0455-282mentioning

confidence: 96%

O VI in the local interstellar medium

Barstow¹,

Boyce²,

Barstow³

et al. 2008

Space Astronomy

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We report the results of a search for O VI absorption in the spectra of 80 hot DA white dwarfs observed by the FUSE satellite. We have carried out a detailed analysis of the radial velocities of interstellar and (where present) stellar absorption lines for the entire sample of stars. In approximately 35% of cases (where photospheric material is detected), the velocity differences between the interstellar and photospheric components were beneath the resolution of the FUSE spectrographs. Therefore, in 65% of these stars the interstellar and photospheric contributions could be separated and the nature of the O VI component unambiguously determined. Furthermore, in other examples, where the spectra were of a high signal-to-noise, no photospheric material was found and any O VI detected was assumed to be interstellar. Building on the earlier work of Oegerle et al. (2005) and Savage & Lehner (2006), we have increased the number of detections of interstellar O VI and, for the first time, compared their locations with both the soft X-ray background emission and new detailed maps of the distribution of neutral gas within the local interstellar medium. We find no strong evidence to support a spatial correlation between O VI and SXRB emission. In all but a few cases, the interstellar O VI was located at or beyond the boundaries of the local cavity. Hence, any T ~ 300,000K gas responsible for the O VI absorption may reside at the interface between the cavity and surrounding medium or in that medium itself. Consequently, it appears that there is much less O VI-bearing gas than previously stated within the inner rarefied regions of the local interstellar cavity.

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Quasi-Molecular Lines in Lyman Wings of Cool DA White Dwarfs; Application to FUSE Observations of G 231–40

et al. 2003

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Abstract. We present new theoretical calculations of the total line profiles of Lyman α and Lyman β which include perturbations by both neutral hydrogen and protons and all possible quasi-molecular states of H2 and H + 2 . They are used to improve theoretical modeling of synthetic spectra for cool DA white dwarfs. We compare them with FUSE observation of G 231-40. The appearance of the line wings between Lyman α and Lyman β is shown to be sensitive to the relative abundance of hydrogen ions and neutral atoms, and thereby to provide a temperature diagnostic for stellar atmospheres and laboratory plasmas.

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A High‐Dispersion Spectroscopic Survey of the Hot White Dwarfs: The IUE NEWSIPS SWP Echelle Data Set

Cited by 82 publications

References 69 publications

Iron abundance in hot hydrogen-deficient central stars and white dwarfs from FUSE, HST, and IUE spectroscopy

Iron abundance in hot hydrogen-deficient central stars and white dwarfs from FUSE, HST, and IUE spectroscopy

O VI in the local interstellar medium

Quasi-Molecular Lines in Lyman Wings of Cool DA White Dwarfs; Application to FUSE Observations of G 231–40

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