WSO–UV Project: New Touches

Шустов, Б. М.; Sachkov, Mikhail; Sichevsky, S. G.; Arkhangelsky, R. N.; Beitia-Antero, Leire; Бисикало, Д. В.; Богачев, С. А.; Buslaeva, A. I.; Vallejo, Juan Carlos; Castro, Ana Inés Gómez de; Grigorovich, S.; Iosipenko, S. V.; Kanev, E.; Canet, Ada; Korablev, Oleg; Kuzin, Sergey; Moisheev, A. A.; Cazalla, I. Prada; Tavrov, A. V.; Marcos, R. de la Fuente; Shakhanov, A. E.; Shmagin, V.; Shostak, S. V.; Shugarov, A. S.; Gestoso, F. J. Yañez

doi:10.1134/s0038094621070194

Cited by 11 publications

(2 citation statements)

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“…For more than 40 yr, the astronomical community used UV spectroscopy as a tool with great value through missions and instruments such as IUE (Macchetto & Penston 1978), theHopkins UV Telescope (Davidsen & Fountain 1985), EUVE (Malina et al 1982), HST-STIS (Kimble et al 1997), FUSE (Sahnow et al 2000), and HST-COS (Green et al 2011). With only a few spectral high-resolution UV satellite missions flying until 2023, however, several future UV satellite projects have already been scheduled (SPARC; Jewell et al 2018), are under construction (WSO-UV; Shustov et al 2021), and/or are scheduled to successfully leave their conceptional phase soon (POLLUX; Muslimov et al 2018). The idea of understanding the chemical evolution of the galaxy through a broad multispectral observation (Lebouteiller et al 2019) requires the knowledge of numerous molecular fingerprints, from simple to complex molecular species, for their unambiguous identification and interpretation.…”

Section: Introductionmentioning

confidence: 99%

Vibrationally Resolved Absorption and Fluorescence Cross Sections of Adamantane in the Far-ultraviolet Spectral Range on an Absolute Scale

Marder

Breier

Oliveira

et al. 2023

ApJS

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High-resolution absorption, dispersed fluorescence emission, and photoionization cross sections are presented for gas-phase adamantane excited by synchrotron radiation in the exciting-photon energy range of 6–30 eV. Relative and absolute absorption cross sections of so-far unmatched resolution of down to 0.27 cm−1 line width in the region from 6.4–28 eV are shown along with newly discovered vibronic substructures around the HOMO–LUMO transition. Absorption line positions are provided with very high accuracy and listed in tabular form to be used as spectral fingerprints for the detection of adamantane in interstellar media, where its column density may be determined via the absolute cross sections. The fluorescence emission lies in the ultraviolet range from 190–250 nm and is excited starting at the HOMO–LUMO transition at 6.49 eV, which corresponds to the highest fluorescence emission energy. Hitherto unreported fluorescence in the same spectral range and relative photoionization cross sections in the exciting-photon energy range up to 30 eV are also presented along with lifetime measurements for differentiation of the involved electronic states.

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Section: Introductionmentioning

confidence: 99%

Vibrationally Resolved Absorption and Fluorescence Cross Sections of Adamantane in the Far-ultraviolet Spectral Range on an Absolute Scale

Marder

Breier

Oliveira

et al. 2023

ApJS

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“…The Spektr-UF (Spectrum-UV, World Space Observatory-Ultraviolet, WSO-UV) observatory is designed to study the Universe in 115 nm to 310 nm ultraviolet (UV) wavelengths. A 170 cm aperture space telescope has two main science instruments-spectrographs and field cameras [1][2][3].…”

Section: Introductionmentioning

confidence: 99%

Spektr–UF Mission Spectrograph Space Qualified CCD Detector Subsystem

Shugarov,

Sachkov

2023

Photonics

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Spektr–UF (World Space Observatory Ultraviolet, WSO-UV) is a Russian-led international collaboration aiming to develop a large space-borne 1.7 m Ritchey–Chretién telescope with science instruments to study the Universe in ultraviolet wavelengths. The WSO-UV spectrograph (WUVS) consists of three channels: two high-resolution channels (R = 50,000) with spectral ranges of 115–176 nm and 174–310 nm, and a low-resolution (R = 1000) channel with a spectral range of 115–305 nm. Each of the three channels has an almost identical custom detector consisting of a CCD inside a vacuum enclosure, and drive electronics. The main challenges of the WUVS detectors are to achieve high quantum efficiency in the FUV-NUV range, to provide low readout noise (3 e− at 50 kHz) and low dark current (<12 e−/pixel/hour), to operate with integral exposures of up to 10 h and to provide good photometric accuracy. A custom vacuum enclosure and three variants of a custom CCD272-64 sensor with different UV AR coatings optimised for each WUVS channel were designed. The enclosure prevents contamination and maintains the CCD at the operating temperature of −100 ∘C, while the temperature of the WUVS optical bench is +20 ∘C. A camera electronics box (CEB) that houses the CCD drive electronics was developed. Digital correlated double sampling technology allows for extremely low readout noise and flexible frequency for normal and binned pixel readout modes. This paper presents the WUVS detector design drivers, methods for extending the service life of the CCD sensors working with low signals in a space radiation environment and the key calculated parameters and results of the engineering qualification model qualification campaign.

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