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    1. http://www.stecf.org/goods/spectroscopy/CDFS_Mastercat/croom01.pdf
    ... absorbed QSOs have been invoked to explain the spectrum of the X-ray background radiation (e.g. Madau, Ghisellini & Fabian 1994 ...
    [ Текст ]  Ссылки http://www.stecf.org/goods/spectroscopy/CDFS_Mastercat/croom01.pdf -- 588.2 Кб -- 16.09.2004
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    2. http://www.stecf.org/goods/spectroscopy/CDFS_Mastercat/szokoly04.ps
    ... surveys indicate that the cosmic X-ray background (XRB) is largely due to accretion ... have now also resolved the majority (60-70%) of the very hard X-ray background ...
    [ Текст ]  Ссылки http://www.stecf.org/goods/spectroscopy/CDFS_Mastercat/szokoly04.ps -- 1186.7 Кб -- 16.09.2004
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    3. http://www.stecf.org/coordination/esa_eso/alma-herschel/report.pdf
    ... These are the objects responsible for the hard X-ray background and are crucial for a determination of the AGN bolometric luminosity, accretion rate and black hole mass. ...
    [ Текст ]  Ссылки http://www.stecf.org/coordination/esa_eso/alma-herschel/report.pdf -- 1000.5 Кб -- 04.09.2008
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    4. Structure Detection in Low Intensity X-Ray Images using the Wavelet Transform
    ... No background model is needed, and simulations with different background levels have shown the reliability and the robustness of the method. ...
    [ Сохраненная копия ]  Ссылки http://www.stecf.org/conferences/adass/adassVII/starckjl.html -- 16.2 Кб -- 12.06.2006
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    5. Fitting and Modeling of AXAF Data with the ASC Fitting Application
    ... hand, needs to construct the model by evaluating three model stacks, the source, background, and instrument model stacks, and then combining them appropriately (i.e., the background model is added to the source model, and the result is convolved with an ...
    [ Сохраненная копия ]  Ссылки http://www.stecf.org/conferences/adass/adassVII/does.html -- 12.1 Кб -- 12.06.2006
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    6. http://www.stecf.org/conferences/adass/adassVII/reprints/does.pdf
    ... hand, needs to construct the model by evaluating three model stacks, the source, background, and instrument model stacks, and then combining them appropriately (i.e., the background model is added to the source model, and the result is convolved with an ...
    [ Текст ]  Ссылки http://www.stecf.org/conferences/adass/adassVII/reprints/does.pdf -- 84.8 Кб -- 12.06.2006
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    7. http://www.stecf.org/conferences/adass/adassVII/reprints/starckjl.pdf
    ... must be performed without the last smoothed array for a background free restoration, and only from a subset of the wavelet ... virialisation first occurs and thus in this respect, should present an overall smooth distribution of the X-ray emitting gas ...
    [ Текст ]  Ссылки http://www.stecf.org/conferences/adass/adassVII/reprints/starckjl.pdf -- 63.4 Кб -- 12.06.2006
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    8. http://www.stecf.org/coordination/esa_eso/cosmology/report.pdf
    ... background (CMB) around 1 mm, for the study of primordial structure at the highest redshifts possible; optical and infrared ...
    [ Текст ]  Ссылки http://www.stecf.org/coordination/esa_eso/cosmology/report.pdf -- 1894.6 Кб -- 04.09.2008
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    9. http://www.stecf.org/coordination/esa_eso/extrasolar/report.pdf
    ... an orbit could provide effective shielding from high-energy ionising photons and cosmic rays from nearby supernovae, from the X-ray background by neutral hydrogen in the Galactic plane, and from temporary increases in the perturbed Oort comet impact rate ...
    [ Текст ]  Ссылки http://www.stecf.org/coordination/esa_eso/extrasolar/report.pdf -- 1083.5 Кб -- 04.09.2008
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    10. A Coronagraphic Search for Substellar Companions to Young Stars
    ... Ca H & K line emission, kinematics, X-ray emission, and rotational velocity ... Background objects could be stars or galaxies. ... Therefore, we expect less than 0.02 background stars within at H=22 for each star (D ...
    [ Сохраненная копия ]  Ссылки http://www.stecf.org/conferences/sardinia/node20.html -- 21.5 Кб -- 12.06.2006
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