A New Measurement of the Average Far‐Ultraviolet Extinction Curve

Sasseen, T. P.; Hurwitz, M.; Dixon, W. V.; Airieau, S.

doi:10.1086/337955

Cited by 37 publications

(38 citation statements)

References 33 publications

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“…Reducing the value of m increases the width, as can be seen in Figure 1. The photoabsorption cross sections also show increased extinction toward higher energies (10 eV and beyond), in good agreement with observations (Sassen et al 2002).…”

Section: The Uv Bumpsupporting

confidence: 89%

Fullerenes and Buckyonions in the Interstellar Medium

Iglesias‐Groth

2004

ApJ

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We show that photoabsorption by fullerenes and buckyonions (multishell fullerenes) explain the shape, width, and peak energy of the most prominent feature of interstellar absorption, the UV bump at 2175 . The predicted A optical and near-infrared transitions for these molecules also offer a potential explanation for the long-standing problem of the identity of the diffuse interstellar bands. The implied ubiquitous distribution of fullerenes may also account for the anomalous galactic microwave emission detected by cosmic microwave background experiments. Comparing theoretical cross sections and astronomical data, we estimate a density of fullerenes in the diffuse interstellar medium of 0.1-0.2 parts per million, consistent with the findings in meteorites. Fullerenebased molecules appear to be a major carbon reservoir in the interstellar medium.

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Section: The Uv Bumpsupporting

confidence: 89%

Fullerenes and Buckyonions in the Interstellar Medium

Iglesias‐Groth

2004

ApJ

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“…Also, Sasseen et al (2002) find that in the far-UV region the extinction curve is consistent with an extrapolation of the standard SM curve.…”

Section: The Reddening Correctionsupporting

confidence: 68%

An archive study of 18 old novae

Selvelli

Gilmozzi

2013

A&A

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Aims. We present an overview of the UV spectral properties of old novae as a class. The data and results of this paper, together with data from the outburst phases, will be utilized in a follow-up study to determine statistical properties and to investigate correlations among the physical parameters of the quiescent and eruptive phases. Methods. All the available IUE, HST, and FUSE archive data for 18 old novae were used to derive accurate and homogeneous estimates of the reddening from the 2175 Å extinction bump and to determine the intrinsic spectral energy distribution corresponding to the utilization of both existing extinction curves. We also measured all the emission and absorption lines. Results. We have found good agreement between spectra taken at different epochs and by different instruments, a clear indication of the near constancy of the SED on timescales of several years. With the possible exception of GK Per, the dereddened UV continua are represented well by a single-curve power-law distribution F λ ∝ λ −α , with α in the range 0.32-2.55 for one curve and 0.35-2.88 for the other one. The extrapolation of the various UV power laws to the optical range yields values that are in good agreement with the V magnitudes. We interpret this result as evidence that the SED is dominated by the accretion disk in the UV and optical spectral regions. A detailed study of the emission spectrum has led to measuring and identifying more than one hundred features and to detecting several lines that are rather uncommon in other CVs and whose identification is uncertain.

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“…The low N(H tot ) seen by FUSE and STIS is consistent with the Chandra detection of essentially unabsorbed X-ray emission toward HD 104237 . The O vi 1032 8 profiles, corrected for foreground extinction with the FUV extinction curve of Sasseen et al (2002), registered to a common wavelength scale using the foreground H 2 absorption and scaled to a nominal distance of 100 pc, are shown in Figure 9.…”

Section: Fusementioning

confidence: 99%

The Environment of the Optically Brightest Herbig Ae Star, HD 104237

Grady

Woodgate

Torres

et al. 2004

ApJ

129

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We investigate the environment of the nearest Herbig Ae star, HD 104237, with a multiwavelength combination of optical coronagraphic, near-IR, and mid-IR imaging supported by optical, UV, and far-ultraviolet spectroscopy. We confirm the presence of T Tauri stars associated with the Herbig Ae star HD 104237, noted by Feigelson et al. We find that two of the stars within 15 00 of HD 104237 have IR excesses, potentially indicating the presence of circumstellar disks, in addition to the Herbig Ae star itself. We derive a new spectral type of A7.5Ve-A8Ve for HD 104237 and find log (L=L ) ¼ 1:39. With these data, HD 104237 has an age of t % 5 Myr, in agreement with the estimates for the other members of the association. HD 104237 is still actively accreting, with a conspicuous UV/far-UV excess seen down to 1040 8, and is driving a bipolar microjet termed HH 669. This makes it the second, older Herbig Ae star now known to have a microjet. The presence of the microjet enables us to constrain the circumstellar disk to r 0B6 (70 AU) with an inclination angle of i ¼ 18 þ14 À11 from pole-on. The absence of a spatially extended continuum and fluorescent H 2 emission near Ly is in agreement with the prediction of shadowed disk models for the IR spectral energy distribution. With the high spatial density of disks in this group of stars, proximity, and minimal reddening, HD 104237 and its companions should serve as ideal laboratories for probing the comparative evolution of planetary systems.

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A New Measurement of the Average Far‐Ultraviolet Extinction Curve

Cited by 37 publications

References 33 publications

Fullerenes and Buckyonions in the Interstellar Medium

Fullerenes and Buckyonions in the Interstellar Medium

An archive study of 18 old novae

The Environment of the Optically Brightest Herbig Ae Star, HD 104237

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