The imaging and slitless spectroscopy instrument for surveys (ISSIS) for the world space observatory-ultraviolet (WSO-UV)

Castro, Ana Inés Gómez de; Maíz, Jesús; Rodríguez, P.; Gómez, Maite; Larruquert, Juan I.; Méndez, José A.; Belenguer, T.; Rodrigo-Gudiel, Víctor; López-Martínez, F.; Sestito, P.

doi:10.1007/s10509-011-0695-9

Cited by 17 publications

(3 citation statements)

References 9 publications

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“…The main directions and stages of development of methods of UV spectroscopy are presented in Panchuk et al (2006) in more detail. Recent progress in UV imaging is presented in Gómez de Castro et al (2011).…”

Section: Uv Experiments and Observatories: Past And Presentmentioning

confidence: 99%

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World space observatory-ultraviolet among UV missions of the coming years

Шустов

Sachkov

Castro

et al. 2011

Astrophys Space Sci

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Continuous access to the UV domain has been considered of importance to astrophysicists and planetary scientists since the mid-sixties. However, the future of UV missions for the post-HST era is believed by a significant part of astronomical community to be less encouraging. We argue that key science problems of the coming years will require further development of UV observational technologies. Among these hot astrophysical issues are: the search for missing baryons, revealing the nature of astronomical engines, properties of atmospheres of exoplanets as well as of the planets of the Solar System etc. We give a brief review of UV-missions both in the past and in the future. We conclude that UV astronomy has a great future but the epoch of very large and efficient space UV facilities seems to be a prospect for the next decades. As to the current state of the UV instrumentation we think that this decade will be dominated by the HST and coming World Space ObservatoryUltraviolet (WSO-UV) with a 1.7 m UV-telescope onboard. The international WSO-UV mission is briefly described. It will allow high resolution/high sensitivity imaging and B. Shustov · M. Sachkov ( )

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Section: Uv Experiments and Observatories: Past And Presentmentioning

confidence: 99%

“…The set of cameras (under responsibility of Spain) was named Imaging and Slitless Spectroscopy Instrument for Surveys (ISSIS). It is described in detail in Gómez de Castro et al (2011). Here we briefly recall the major features of the Instrument.…”

Section: Wso-uv Science Instrumentsmentioning

confidence: 99%

World space observatory-ultraviolet among UV missions of the coming years

Шустов

Sachkov

Castro

et al. 2011

Astrophys Space Sci

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“…LSS can be used for quick studies of BMS wind signatures, and even terminal velocity determinations. The Imaging and Slitless Spectrograph Instrument for Surveys (ISSIS) can also be used in spectroscopic mode for this purpose, but with lower resolution (R ∼ 500; Gómez de Castro et al 2011). For a detailed quantitative analysis, the enhanced resolution of HIRDES-VUVES observations will be required.…”

Section: The Prolific 900-1800 å Spectral Regionmentioning

confidence: 99%

WSO and the winds of massive stars: the gate to the metal-poor Local Universe

García

Herrero

Najarro

2011

Astrophys Space Sci

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The spectrographs on-board the World Space Observatory (WSO) will provide access to the 1020-1800 Å wavelength range with unprecedented sensitivity. Previous observatories operating in the 1150-2000 Å range (such as IUE and HST-STIS) have proved extremely useful to study the winds of OB type stars, which leave their most prominent imprints in the far ultraviolet range. The addition of the λ < 1200 Å wavelengths is critical as it contains important diagnostic lines for mass loss and shocks in the wind, as found by FUSE-based analyses.WSO will enable quantitative spectroscopic analyses of blue massive stars in the Local Group beyond the Magellanic Clouds. The results will lead to the characterization of their winds as a function of metallicity, and shed new light on current urging questions regarding radiation driven winds. Metallicity and the winds of blue massive stars Radiation driven winds, key agents of evolutionThe role of massive stars in our understanding of galacticscale processes and the Universe is often understated. Massive stars craft the interstellar medium, dominate the spectral energy distribution of star-forming galaxies and are related to very energetic and disruptive processes like supernovae and possibly long gamma-ray bursts.Blue massive stars (BMS) experience radiation-driven outflows of matter, or winds. They are propelled by the absorption of photons in the numerous ultraviolet transitions of metallic ions (see for instance the review of Kudritzki and Puls 2000). The stellar wind is the main interface of pre-supernova massive stars with the interstellar medium because of its injection of mechanical and radiative energy, and chemically enriched material. The wind is also a principal agent of the evolution of the massive star itself. Because of the wind mass removal the rate and efficiency of the central nuclear reactions change, altering the duration of the evolutionary stages and ultimately deciding the fate of the star (the SN explosion, the stellar yields, and the remnant: Matteucci 2008;Woosley et al. 2002;Maeder and Meynet 2003).Radiation driven winds are included in the codes that model the atmospheres of blue massive stars (Puls et al. 2005;Pauldrach et al. 2001;Hillier and Miller 1998) and their evolution (Maeder and Meynet 2000), and subsequently in models of galactic chemical evolution (see recent review by Recchi 2009, 2010). The inclusion of stellar winds has a significant impact on the stellar parameters derived from spectroscopic analyses (Herrero et al. 2002;Repolust et al. 2004), which in turn provide constraints for massive star evolution models.

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WSO‐UV project for high‐resolution spectroscopy and imaging

et al. 2014

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During the last three decades, astronomers have had practically continuous access to the 100-300 nm spectral range that is unreachable with ground-based instruments but where astrophysical processes can be efficiently studied with unprecedented capability since the resonance lines of the most abundant atoms and ions at temperatures between 3 000 and 300 000 K are in the UV. The successful International Ultraviolet Explorer (IUE) observatory, Russian ASTRON mission and successor instruments such as the COS and STIS spectrographs on-board the Hubble Space Telescope (HST) demonstrate the major impact that observations in the UV wavelength range have had on modern astronomy. The access to space-based observatories is very limited. For the next decade, for the post-HST era, the World Space Observatory UltraViolet (WSO-UV) will be the only large telescope class mission for UV observations, both spectroscopic and imaging. By its potential, the WSO-UV mission is similar to the HST, though it exceeds the HST/STIS in sensitivity by a factor 5-10, but all the observing time will be available for UV astronomy. In this paper, we briefly outline the WSO-UV mission model, instrumentation description, science management plan as well as some of the key science issues that WSO-UV will address during its lifetime.

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The imaging and slitless spectroscopy instrument for surveys (ISSIS) for the world space observatory-ultraviolet (WSO-UV)

Cited by 17 publications

References 9 publications

World space observatory-ultraviolet among UV missions of the coming years

World space observatory-ultraviolet among UV missions of the coming years

WSO and the winds of massive stars: the gate to the metal-poor Local Universe

WSO‐UV project for high‐resolution spectroscopy and imaging

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