UV detectors for spectrographs of WSO-UV project

Shugarov, A. S.; Саванов, И. С.; Sachkov, Mikhail; Jerram, Paul; Moody, Ian; Pool, P.; Turner, P.R.; Pittock, R.; Kuzin, Sergey; Waltham, Nick

doi:10.1007/s10509-014-1911-1

Cited by 39 publications

(12 citation statements)

References 9 publications

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“…Because of this technical change, the WUVS exposure time calculator is not yet available. See Shugarov et al (2014) for detailed information about the WSO-UV CCD detectors.…”

Section: Wso-uv Spectrographsmentioning

confidence: 99%

Major prospects of exoplanet astronomy with the World Space Observatory–UltraViolet mission

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et al. 2014

Astrophys Space Sci

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The success of the International Ultraviolet Explorer (IUE) first and then of the STIS and COS spectrographs on-board the Hubble Space Telescope (HST) demonstrate the impact that observations at UV wavelengths had and are having on modern astronomy. Several discoveries in the exoplanet field have been done at UV wavelengths. Nevertheless, the amount of data collected in this band is still limited both in terms of observed targets and time spent on each of them. For the next decade, the post-HST era, the only large (2-m class) space telescope capable of UV observations will be the World Space Observatory-UltraViolet (WSO-UV). In its characteristics, the WSO-UV mission is similar to that of HST, but all observing time will be dedicated to UV astronomy. In this work, we briefly outline the major prospects of the WSO-UV mission in terms of exoplanet studies. To the limits of the data and tools currently available, here we also compare the quality of key exoplanet data obtained in the far-UV and near-UV with HST (STIS and COS) to that expected to obtain with WSO-UV.

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“…Because of this technical change, the WUVS exposure time calculator is not yet available. See Shugarov et al (2014) for detailed information about the WSO-UV CCD detectors.…”

Section: Wso-uv Spectrographsmentioning

confidence: 99%

Major prospects of exoplanet astronomy with the World Space Observatory–UltraViolet mission

Fossati

Бисикало

Lämmer

et al. 2014

Astrophys Space Sci

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“…It is expected that the effective area of the VUVPS in the far ultraviolet will be comparable to the HST instruments, and exceed their effective area in the near UV. We believe this can be achieved thanks to substantial progress in the efficiencies of CCD detectors [23] and the high quality of the UV coatings of the reflecting elements [21]. Note that this high efficiency of the spectographs (channels) can be reached in spite of the fact that the surface area of the T-170M telescope is roughly half the corresponding surface area of the HST.…”

Section: Spektr-uv (World Spacementioning

confidence: 99%

Scientific problems addressed by the Spektr-UV space project (world space Observatory—Ultraviolet)

et al. 2016

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Abstract-The article presents a review of scientific problems and methods of ultraviolet astronomy, focusing on perspective scientific problems (directions) whose solution requires UV space observatories. These include reionization and the history of star formation in the Universe, searches for dark baryonic matter, physical and chemical processes in the interstellar medium and protoplanetary disks, the physics of accretion and outflows in astrophysical objects, from Active Galactic Nuclei to close binary stars, stellar activity (for both low-mass and high-mass stars), and processes occurring in the atmospheres of both planets in the solar system and exoplanets. Technological progress in UV astronomy achieved in recent years is also considered. The well advanced, international, Russian-led Spektr-UV (World Space Observatory-Ultraviolet) project is described in more detail. This project is directed at creating a major space observatory operational in the ultraviolet (115-310 nm). This observatory will provide an effective, and possibly the only, powerful means of observing in this spectral range over the next ten years, and will be an powerful tool for resolving many topical scientific problems.

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“…The main changes with respect to the previous design (Reutlinger et al 2011) have been: (1) the cross disperser in the UVES spectrograph is now similar to the VUVES spectrograph (based on the cross disperser combined with a UV camera mirror) and (2) segmented toroidal gratings are implemented in the LSS design. CCDs were chosen as detectors for all 3 channels (see Shugarov et al 2014) for more details about the The optical elements of WUVS are being produced by the National Research University of Information Technologies, Mechanics and Optics (ITMO) (see Fig. 6).…”

Section: Wuvs Designmentioning

confidence: 99%