The IUE spacecraft and instrumentation

Boggess, A.; Carr, F. A.; Evans, D. C.; Fischel, D.; Freeman, H. R.; Fuechsel, C. F.; Klinglesmith, Daniel A.; Krueger, V. L.; Longanecker, G. W.; Moore, James V.; Pyle, E. J.; Rebar, F. J.; Sizemore, K. O.; Sparks, W. M.; Underhill, Anne B.; Vitagliano, H. D.; West, D. K.; Macchetto, F.; Fitton, B.; Barker, Paul; Dunford, E.; Gondhalekar, P. M.; Hall, Jason E.; Harrison, V.A.W.; Oliver, Muellenhoff; Sandford, M. C. W.; Vaughan, P. A.; Ward, A. K.; Anderson, B.; Boksenberg, A.; Coleman, C. I.; Snijders, M. A. J.; Wilson, R.

doi:10.1038/275372a0

Cited by 239 publications

(94 citation statements)

References 11 publications

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“…By mining the IUE and the MAST archives, we have found UV spectra belonging to twenty old novae, the vast majority from IUE (Boggess et al 1978), complemented for some objects by data, generally unpublished, which was obtained with HST-GHRS, HST-STIS, HST-FOS. and FUSE.…”

Section: The Uv Data and Their Reductionmentioning

confidence: 99%

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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Section: The Uv Data and Their Reductionmentioning

confidence: 99%

An archive study of 18 old novae

Selvelli

Gilmozzi

2013

A&A

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“…Figure 4b shows the reddening of our sample, with a median reddening of A v,med = 0.13, in good agreement with expectations. As a check on the accuracy of derived reddening A v from sedFit, we use the sample of 21 OB stars in the Cep OB3 association with directly observed UV extinction curves from the International Ultraviolet Explorer (IUE, Boggess et al 1978) satellite observations (Massa & Conti 1981;Massa & Savage 1984). We fit the SEDs of 21 stars from photometry derived from the literature, in the same manner as §3.…”

Section: Tablementioning

confidence: 99%

A Catalog of Calibrator Stars for Next-Generation Optical Interferometers

Swihart

Garcia

Stassun

et al. 2016

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Benchmark stars with known angular diameters are key to calibrating interferometric observations. With the advent of optical interferometry, there is a need for suitably bright, well-vetted calibrator stars over a large portion of the sky. We present a catalog of uniformly computed angular diameters for 1523 stars in the northern hemisphere brighter than V = 6 and with declinations −15• < δ < 82• . The median angular stellar diameter is 0.527 mas. The list has been carefully cleansed of all known binary and multiple stellar systems. We derive the angular diameters for each of the stars by fitting spectral templates to the observed spectral energy distributions (SEDs) from literature fluxes. We compare these derived angular diameters against those measured by optical interferometry for 75 of the stars, as well as to 176 diameter estimates from previous calibrator catalogs, finding in general excellent agreement. The final catalog includes our goodness-of-fit metrics as well as an online atlas of our SED fits. The catalog presented here permits selection of the best calibrator stars for current and future visible-light interferometric observations.

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“…Indeed, most of the DAC observations leading to the concept of CIRs were carried out as part of the MEGA campaign (Massa et al 1995b) performed with the IUE satellite (Boggess et al 1978) and were not repeated afterwards. Long dedicated monitoring campaigns of the UV spectroscopic variability of the previously observed supergiant stars and the other supergiants hosted in the SgXBs are thus critically required.…”

Section: Discussionmentioning

confidence: 99%

The super-orbital modulation of supergiant high-mass X-ray binaries

Bozzo

Oskinova

Lobel

et al. 2017

A&A

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The long-term X-ray light curves of classical supergiant X-ray binaries and supergiant fast X-ray transients show relatively similar super-orbital modulations, which are still lacking a sound interpretation. We propose that these modulations are related to the presence of corotating interaction regions (CIRs) known to thread the winds of OB supergiants. To test this hypothesis, we couple the outcomes of three-dimensional (3D) hydrodynamic models for the formation of CIRs in stellar winds with a simplified recipe for the accretion onto a neutron star. The results show that the synthetic X-ray light curves are indeed modulated by the presence of the CIRs. The exact period and amplitude of these modulations depend on a number of parameters governing the hydrodynamic wind models and on the binary orbital configuration. To compare our model predictions with the observations, we apply the 3D wind structure previously shown to well explain the appearance of discrete absorption components in the UV time series of a prototypical B0.5I-type supergiant. Using the orbital parameters of IGRJ 16493-4348, which has the same B0.5I donor spectral type, the period and modulations in the simulated X-ray light curve are similar to the observed ones, thus providing support to our scenario. We propose that the presence of CIRs in donor star winds should be considered in future theoretical and simulation efforts of wind-fed X-ray binaries.

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The IUE spacecraft and instrumentation

Cited by 239 publications

References 11 publications

An archive study of 18 old novae

An archive study of 18 old novae

A Catalog of Calibrator Stars for Next-Generation Optical Interferometers

The super-orbital modulation of supergiant high-mass X-ray binaries

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