The Final Archive and Recalibration of the International Ultraviolet Explorer (IUE) Satellite

Nichols, Joy S.; Linsky, Jeffrey L.

doi:10.1086/117803

Cited by 125 publications

(99 citation statements)

References 14 publications

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“…We defined an average observed UV spectrum using the available highest S/N ratio spectra, namely LWP 27954 and LWP 30925 for the long wavelength region (1850-3350Å) and SWP 50606 and SWP 50609 for the short wavelength region (1150-2000Å), retrieved from the IUE Final Archive (Nichols & Linsky 1996).…”

Section: Physical Parametersmentioning

confidence: 99%

New physical elements of HR 7428 and its Hαbehaviour

Marino

Catalano

Frasca

et al. 2001

A&A

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Abstract. HR 7428 is a spectroscopic binary composed of a K2 II-III and a main-sequence A2 star. Thanks to a new set of radial velocity measurements from our and IUE spectroscopy we have improved the orbital period determination and the spectroscopic elements of both components. Combining optical photometry and UV low dispersion IUE spectra we have determined new stellar parameters through photospheric synthetic spectra using the NextGen models by Hauschildt et al. (1999aHauschildt et al. ( , 1999b. The hot secondary component parameters agree with those of a typical A2 V star while the radius of the primary cool star turns out to be 40 R , i.e. significantly smaller than a previous estimate of 62 R . The position of the hot and cool component on the H-R diagram is consistent with a normal evolution, without any mass exchange, of this binary system, whose age is in the range 100-200 Myrs. The system displays a filled-in Hα profile with significant variations both in depth and width along the orbital phase. In addition to the Hα chromospheric emission component, we have detected, at some phases, a broad extra-absorption and emission that we relate to an inter-system cloud.

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Section: Physical Parametersmentioning

confidence: 99%

New physical elements of HR 7428 and its Hαbehaviour

Marino

Catalano

Frasca

et al. 2001

A&A

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“…The log of images are given in Table 2. IUE obtained both low dispersion (6 Å resolution) and high dispersion (λ/δλ ∼ 10 000) spectra with the short-wavelength prime (SWP: 1150-2000 Å), longwavelenght prime (LWP: 1850-3400 Å), and long-wavelength redundant (LWR: 1850-3400 Å) cameras (Nichols & Linsky 1996). The spectra show emission lines originating in the chromosphere and transition region.…”

Section: Iue Data and Spectral Analysismentioning

confidence: 99%

“…29 and Oct. 5, 1984. In this study 54 IUE spectra of σ Gem observed between 1979 and 1986 and reduced by means of NEWSIPS were analysed and some of them were reviewed in detail together with the IUESIPS spectra analysed by Ayres et al (1984) and by Engvold et al (1988). The new calibration together with the new image processing techniques have been summarized by Nichols & Linsky (1996). They pointed out that the wavelength and absolute flux errors in the IUESIPS processing could be corrected by NEWSIPS progressing.…”

Section: Introductionmentioning

confidence: 99%

IUE-newsips spectra of σ Geminorum

Ekmekci

Karakuş

2002

A&A

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Abstract. The IUE spectra of σ Gem have been taken from the NASA IUE archive using IDL (Interactive Data Language). The spectra have been observed in 1979-1986 period. All the spectra analysed in the present study have NEWSIPS reductions and consist of 25 LWP, 8 LWR and 5 SWP images in high resolution, and 2 LWP and 14 SWP images in low dispersion. The emission lines, identified as activity indicators and originating in the chromosphere and transition region, are seen in the spectra. The emission line fluxes and equivalent widths are computed based on Gaussian profile fitting procedures to examine the existence of any line flux variation that depends on time or orbital phase. It was found that there is a flux variation with time and orbital phase that is in good agreement with the photometric light curve variation. By comparing the flux variation with simultaneous light curve variation, it can be shown that there is a relation between the ultraviolet flux variation and the spot activity of the system, as shown by Ayres et al. (1984) and Engvold et al. (1988) based on their IUE (with IUESIPS reduction) spectral analysis. Moreover, it was inferred that there is no ultraviolet excess in σ Gem by comparing the spectra of β Gem taken as a comparison star. The Mg II h and k radial velocity curves of σ Gem were in a good agreement with data obtained by Eker (1986) and Duemmler et al. (1997). The sinusoidal Mg II radial velocity curve solutions of the system give e = 0, P orb. = 19.607 ± 0.008 days, K = 34.86 ± 2.33 km s −1 , γ = 49.42 ± 1.87 km s −1 and T o = 2445972.53 ± 0.28. Since the ultraviolet flux data are not conveniently distributed and are insufficient to determine the activity cycle, the evaluation of the ultraviolet flux activity cycle was not successful.

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“…All raw data have been reduced by the NEW SPECTRAL IMAGE PROCESSING SYSTEM (ref. IUE NEWSIPS manual;Nichols & Linsky 1996). In Table 3 we collect the observe time, data format, exposure time, and so on.…”

Section: Observationsmentioning

confidence: 99%

A Two-Temperature Model for LBVs

Guo

Shan

2004

Proc. IAU

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Abstract. The continuum energy distributions of R127 and R110 in the outburst phase are fitted by use of a optically envelope model. Both stars show two peaks in the continuum energy distributions in which one lies in the short-wavelength range (near 1250Å) and the other in the optical band. We suggest that the fluxes in the UV and optical bands may have different origins: the UV flux comes from the central star and the optical flux comes from the expanded optically envelope. We construct such a model for LBVs with the use of two LTE atmosphere models with different temperatures, and find it to be in satisfactory agreement with the observed spectral energy distributions of R127 and R110.

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The Final Archive and Recalibration of the International Ultraviolet Explorer (IUE) Satellite

Cited by 125 publications

References 14 publications

New physical elements of HR 7428 and its Hαbehaviour

New physical elements of HR 7428 and its Hαbehaviour

IUE-newsips spectra of σ Geminorum

A Two-Temperature Model for LBVs

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