High‐resolution FUV spectroscopy of the terrestrial day airglow with the Far Ultraviolet Spectroscopic Explorer

Feldman, P. D.; Sahnow, David J.; Kruk, J. W.; Murphy, E. M.; Moos, H. W.

doi:10.1029/2000ja000356

Cited by 110 publications

(91 citation statements)

References 24 publications

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“…We have included both the night and day time data for VV 114 due to the small percentage of night time data available for that target. Feldman et al (2001). Though the night airglow spectrum is very noisy the two spectra show the wealth of geo-coronal emission features that impact data analysis in these wavelength regions.…”

Section: Discussionmentioning

confidence: 99%

Observations of Starburst Galaxies With Far-Ultraviolet Spectrographic Explorer: Galactic Feedback in the Local Universe

Grimes

Heckman

Aloisi

et al. 2009

ApJS

166

200

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We have analyzed FUSE (905-1187Å) spectra of a sample of 16 local starburst galaxies. These galaxies cover almost three orders of magnitude in starformation rates and over two orders of magnitude in stellar mass. Absorption features from the stars and interstellar medium are observed in all the spectra. The strongest interstellar absorption features are generally blue-shifted by ∼ 50 to 300 km s −1 , implying the almost ubiquitous presence of starburst-driven galactic winds in this sample. The outflow velocites increase with both the star formation rate and the star formation rate per unit stellar mass, consistent with a galactic wind driven by the population of massive stars. We find outflowing coronal-phase gas (T ∼ 10 5.5 K) detected via the O VI absorption-line in nearly every galaxy. The O VI absorption-line profile is optically-thin, is generally weak near the galaxy systemic velocity, and has a higher mean outflow velocity than seen in the lower ionization lines. The relationship between the line width and column density for the O VI absorbing gas is in good agreement with expectations for radiatively cooling and outflowing gas. Such gas will be created in the interaction of the hot out-rushing wind seen in X-ray emission and cool dense ambient material. O VI emission is not generally detected in our sample, suggesting that radiative cooling by the coronal gas is not dynamically significant in draining energy from galactic winds. We find that the measured outflow velocities in the HI and HII phases of the interstellar gas in a given galaxy increase with the strength (equivalent width) of the absorption feature and not with the -2 -ionization potential of the species. The strong lines often have profiles consisting of a broad and optically-thick component centered near the galaxy systemic velocity and weaker but highly blue-shifted absorption. This suggests that the outflowing gas with high velocity has a lower column density than the more quiescent gas, and can only be readily detected in the strongest absorption lines. From direct observations below the Lyman edge in the galaxy rest-frame, we find no evidence of Lyman continuum radiation escaping from any of the galaxies in the sample. Moreover, the small escape fraction of light in the center of the strong C II absorption feature confirms the high opacity below the Lyman limit in the neutral ISM. The absolute fraction of escaping Lyman continuum photons is typically <1%. This sample provides a unique window on the global properties of local star-forming galaxies as observed in the far-UV and also provides a useful comparison sample for understanding spectra of high redshift star-forming galaxies.

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Section: Discussionmentioning

confidence: 99%

Observations of Starburst Galaxies With Far-Ultraviolet Spectrographic Explorer: Galactic Feedback in the Local Universe

Grimes

Heckman

Aloisi

et al. 2009

ApJS

166

200

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“…These authors provide FUSE spectra of the earth's illuminated disk. In the wavelength region in which the C iii(λ1176 Å) line occurs, the day-time airglow spectra (Feldman et al 2001) show no enhancements. Around 976.5 Å there is a known O i airglow emission line that is also visible in the FUSE airglow spectra.…”

Section: Solar C Iii(λ1176 å)/ C Iii(λ977 å) Line Ratiomentioning

confidence: 99%

“…For the investigation of airglow contamination we made use of the analysis by Feldman et al (2001). These authors provide FUSE spectra of the earth's illuminated disk.…”

Section: Solar C Iii(λ1176 å)/ C Iii(λ977 å) Line Ratiomentioning

confidence: 99%

Search for indications of stellar mass ejections using FUV spectra

Leitzinger

Odert

Ribas

et al. 2011

A&A

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Aims. We search for highly energetic activity phenomena in a small sample of late-type main-sequence stars in the far ultraviolet (FUV) using data from the Far Ultraviolet Spectroscopic Explorer (FUSE). Methods. Because FUSE allows a simultaneous photometric and spectroscopic analysis, we are able to analyze variations in the light curves (flares) and possible, activity-related signatures (line asymmetries, enhancements, and shifts) in the spectra. Furthermore, the computation of the well-known density-sensitive line ratio C iii(λ1176 Å)/C iii(λ977 Å) is also possible, and allows the investigation of its dependence on stellar activity. Results. Three late-type main-sequence stars found in the FUSE archive (HD 36705, HD 197481, and Gl 388) show flares in their light curves. We find no obvious Doppler shifts in the brightest lines of these stars, but the O vi(λ1032 Å) transition region line of AD Leo shows a blue wing enhancement one spectrum after a flare event. This emission feature is shifted by ∼-84 km s −1 from the line core. We can exclude that the spectral feature was caused by a gas cloud co-rotating with the star and favor an interpretation of a mass ejection. In addition we find an increase of the C iii(λ1176 Å)/C iii(λ977 Å) line ratio during all detected flares. We compare this finding to the Sun using solar full-disk spectra from the Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED) and SOlar Radiation and Climate Experiment (SORCE) missions, and find that powerful flare events also show an increased C iii(λ1176 Å)/C iii(λ977 Å) line ratio but this result is of low statistical significance. Owing to a lack of perfectly temporally coinciding TIMED/SORCE spectra and a low temporal resolution (∼15 spectra per day) it is not possible to distinguish clearly if this increase is caused by the flares or by the related mass ejections.

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“…The disagreement between the predicted and observed Ly quasi-molecular H þ 2 lines in AM Her may suggest that the magnetic field plays a role in the formation of these lines. The continuum flux of AM Her below '970 8 is very weak and strongly contaminated by airglow emission (see Feldman et al [2001] for details on the identification of airglow lines). Similar to those in the STIS spectrum, a number of weak and sharp absorption features are detected, which we identify as interstellar metallic absorption lines (Sembach 1999) and H 2 molecular absorption bands (Jenkins & Peimbert 1997).…”

Section: Average Spectramentioning

confidence: 99%

FUSEandHSTSTIS Far‐Ultraviolet Observations of AM Herculis in an Extended Low State

Gänsicke

Long

Barstow

et al. 2006

ApJ

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We have obtained FUSE and HST STIS time-resolved spectroscopy of the Polar AM Herculis during a deep low state. The spectra are entirely dominated by the emission of the white dwarf. Both the far-ultraviolet ( FUV ) flux and the spectral shape vary substantially over the orbital period, with maximum flux occurring at the same phase as during the high state. The variations are due to the presence of a hot spot on the white dwarf, which we model quantitatively. The white dwarf parameters can be determined from a spectral fit to the faint-phase data, when the hot spot is self-eclipsed. Adopting the distance of 79 þ8 À6 pc determined by Thorstensen, we find an effective temperature of 19;800 AE 700 K and a mass of M WD ¼ 0:78 þ 0:12 À 0:17 M . The hot spot has a lower temperature than during the high state, $34,000-40,000 K, but covers a similar area, $10% of the white dwarf surface. Low-state FUSE and STIS spectra taken during four different epochs in [2002][2003] show no variation of the FUV flux level or spectral shape, implying that the white dwarf temperature and the hot spot temperature, size, and location do not depend on the amount of time the system has spent in the low state. Possible explanations are ongoing accretion at a low level or deep heating; both alternatives have some weaknesses, which we discuss. No photospheric metal absorption lines are detected in the FUSE and STIS spectra, suggesting that the average metal abundances in the white dwarf atmosphere are lower than $10 À3 times their solar values.

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High‐resolution FUV spectroscopy of the terrestrial day airglow with the Far Ultraviolet Spectroscopic Explorer

Cited by 110 publications

References 24 publications

Observations of Starburst Galaxies With Far-Ultraviolet Spectrographic Explorer: Galactic Feedback in the Local Universe

Observations of Starburst Galaxies With Far-Ultraviolet Spectrographic Explorer: Galactic Feedback in the Local Universe

Search for indications of stellar mass ejections using FUV spectra

FUSEandHSTSTIS Far‐Ultraviolet Observations of AM Herculis in an Extended Low State

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