Achromatic interfero-coronagraph with variable rotational shear: reducing of star leakage effect, white light nulling with lab prototype

Frolov, Pavel; Shashkova, I. A.; Bezymyannikova, Yuliya; Kiselev, Alexander V.; Tavrov, Alexander V.

doi:10.1117/1.jatis.2.1.011002

Cited by 11 publications

(11 citation statements)

References 13 publications

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“…PROCYON with a Lyman Alpha Imaging CAmera Cassegrain telescope has observed geocorona images [13]. Images are formed from exospheric atoms observed from up to more than 240,000 km, which is about 38 Earth radii.…”

Section: Uvspex Spectrograph Science Goalsmentioning

confidence: 99%

“…Planetary Orbiter (MPO) for the BepiColombo mission [44]. Among them, two flight tested components are the grating (CLASP mission [ 45 , 46 ]), and the photo-detector (BepiColombo/PHEBUS-FUV [47,48], PROCYON/LAICA [13]). Fig.…”

Section: Probing Of Herman Exosphere By Ultraviolet Spectroscopy (Phementioning

confidence: 99%

“…This optical concept is conventional and has been used in other space missions for UV spectroscopy, e.g., Extreme ultraviolet spectrosCope for ExosphEric Dynamics (EXCEED) onboard Hisaki [43] and Probing of Herman Exosphere by Ultraviolet Spectroscopy (PHEBUS) onboard Mercury Planetary Orbiter (MPO) for the BepiColombo mission [44]. Among them, two flight tested components are the grating (CLASP mission [ 45 , 46 ]), and the photo-detector (BepiColombo/PHEBUS-FUV [47,48], PROCYON/LAICA [13]).…”

Section: Uv Spectrograph Uvspexmentioning

confidence: 99%

“…The exospheres extend to more than ten times a planet's radius. Because of this extension, exospheres are detectable at stellar distances [13].…”

Section: Introductionmentioning

confidence: 98%

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Stellar imaging coronagraph and exoplanet coronal spectrometer: two additional instruments for exoplanet exploration onboard the WSO-UV 1.7-m orbital telescope

Tavrov

Kameda

Yudaev

et al. 2018

J. Astron. Telesc. Instrum. Syst.

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The World Space Observatory for Ultraviolet (WSO-UV) is an orbital optical telescope with a 1.7 mdiameter primary mirror currently under development. The WSO-UV is aimed to operate in the 115-310 nm UV spectral range. Its two major science instruments are UV spectrographs and a UV imaging field camera with filter wheels. The WSO-UV project is currently in the implementation phase, with a tentative launch date in 2023. As designed, the telescope field of view (FoV) in the focal plane is not fully occupied by instruments. Recently, two additional instruments devoted to exoplanets have been proposed for WSO-UV, which are the focus of this paper. UVSPEX, a UV-Spectrograph for Exoplanets, aims to determine atomic hydrogen and oxygen abundance in the exospheres of terrestrial exoplanets. The spectral range is 115-130 nm which enables simultaneous measurement of hydrogen and oxygen emission intensities during an exoplanet transit. Study of exosphere transit photometric curves can help differentiate among different types of rocky planets. The exospheric temperature of an Earth-like planet is much higher than that of a Venus-like planet, because of the low mixing ratio of the dominant coolant (CO2) in the upper atmosphere of the former, which causes a large difference in transit depth at the oxygen emission line. Thus, whether the terrestrial exoplanet is Earth-like, Venus-like, or other can be determined. SCEDI, a Stellar Coronagraph for Exoplanet Direct Imaging is aimed to directly detect the starlight reflected from exoplanets orbiting their parent stars or from the stellar vicinity including circumstellar discs, dust, and clumps. SCEDI will create an achromatic (optimized to 420-700 nm wavelength range), high-contrast stellocentric coronagraphic image of a circumstellar vicinity. The two instruments: UVSPEX and SCEDI, share common power and control modules. The present communication outlines the science goals of both proposed instruments and explains some of their engineering features.

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Section: Uvspex Spectrograph Science Goalsmentioning

confidence: 99%

Section: Probing Of Herman Exosphere By Ultraviolet Spectroscopy (Phementioning

confidence: 99%

Section: Uv Spectrograph Uvspexmentioning

confidence: 99%

“…The exospheres extend to more than ten times a planet's radius. Because of this extension, exospheres are detectable at stellar distances [13].…”

Section: Introductionmentioning

confidence: 98%

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Stellar imaging coronagraph and exoplanet coronal spectrometer: two additional instruments for exoplanet exploration onboard the WSO-UV 1.7-m orbital telescope

Tavrov

Kameda

Yudaev

et al. 2018

J. Astron. Telesc. Instrum. Syst.

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“…This effect limits the destructive interference contrast to 5 orders of magnitude in terms of starlight suppression. To overcome this effect, an interfero-coronagraph with a variable rotational shear smaller than 180 • , abbreviated as ARC in [11][12][13], offers a possibility to adjust an arbitrary pupil rotation angle to achieve an optimal coronagraphic contrast considering the observing configuration. With a two-meter telescope class, the 10 • -shear interferometer offers the stellar leakage (due to the finite size of the stellar disk) for a Sun-like star at 10 pc almost below 8 orders of magnitude for a 5 λ/D working angle of companion separation.…”

Section: Introductionmentioning

confidence: 99%

Wavefront Sensing by a Common-Path Interferometer for Wavefront Correction in Phase and Amplitude by a Liquid Crystal Spatial Light Modulator Aiming the Exoplanet Direct Imaging

et al. 2023

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We implemented the common-path achromatic interfero-coronagraph both for the wavefront sensing and the on-axis image component suppression, aiming for the stellar coronagraphy. A common-path achromatic interfero-coronagraph has its optical scheme based on a nulling rotational-shear interferometer. The angle of rotational shear can be chosen at a small angular extent of about 10 deg. Such a small angular shear maintains the coronagraphic contrast degradation known as the stellar leakage effect, caused by a finite stellar size. We study the phase and amplitude wavefront control by a liquid crystal spatial light modulator of reflection type which is used as the pixilated active adaptive optics unit. Therefore, adaptive optics perform a wavefront-correcting input toward a stellar interfero-coronagraph aiming at the direct exoplanet imaging. Presented here are both the numeric evaluations and the lab experiment stand to prove the declared functionality output.

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Future Exoplanet Research: High-Contrast Imaging Techniques

Baudoz

2017

Handbook of Exoplanets

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Achromatic interfero-coronagraph with variable rotational shear: reducing of star leakage effect, white light nulling with lab prototype

Cited by 11 publications

References 13 publications

Stellar imaging coronagraph and exoplanet coronal spectrometer: two additional instruments for exoplanet exploration onboard the WSO-UV 1.7-m orbital telescope

Stellar imaging coronagraph and exoplanet coronal spectrometer: two additional instruments for exoplanet exploration onboard the WSO-UV 1.7-m orbital telescope

Wavefront Sensing by a Common-Path Interferometer for Wavefront Correction in Phase and Amplitude by a Liquid Crystal Spatial Light Modulator Aiming the Exoplanet Direct Imaging

Future Exoplanet Research: High-Contrast Imaging Techniques

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