PHEBUS: A double ultraviolet spectrometer to observe Mercury's exosphere

Chassefière, Éric; Maria, Jean-Luc; Goutail, Jean-Pierre; Quémerais, Éric; Leblanc, François; Okano, S.; Yoshikawa, Ichiro; Korablev, Oleg; Gnedykh, V. I.; Naletto, G.; Nicolosi, P.; Pelizzo, Maria Guglielmina; Correia, Jean-Jacques; Gallet, S.; Hourtoule, C.; Mine, Pierre-Olivier; Montaron, Christophe; Rouanet, Nicolas; Rigal, Jean-Baptiste; Muramaki, G.; Yoshioka, Kazuo; Kozlov, O. E.; Kottsov, V. A.; Moisseev, P.; Semena, N.; Bertaux, Jean-Loup; Capria, M. T.; Clarke, John; Cremonese, G.; Delcourt, Dominique; Doressoundiram, A.; Erard, S.; Gladstone, R.; Grandé, M.; Hunten, D. M.; Ip, W.-H.; Izmodenov, Vladislav; Jambon, Albert; Johnson, R. E.; Kallio, Esa; Killen, R. M.; Lallement, R.; Luhmann, J. G.; Mendillo, M.; Milillo, A.; Palme, H.; Potter, A. E.; Sasaki, Susumu; Slater, D. C.; Sprague, A. L.; Stern, A. S.; Yan, Nicolas

doi:10.1016/j.pss.2008.05.018

Cited by 45 publications

(30 citation statements)

References 33 publications

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“…Because the orbital period of the MPO space craft is about 2 hour, it is possible to know the spatial distribution of the atmospheric particle. Note that we have assumed the amount of argon in the atmosphere after Killen et al, 2002 19) , and the efficiencies of the other instrumental components (the entrance mirror and the grating) after Chassefiere et al, 2010 20) .…”

Section: Discussionmentioning

confidence: 99%

Optimization of the MCP Detector for the BepiColombo Mission

Yoshioka

Murakami

Yoshikawa

2009

Trans. JSASS Space Tech. Japan

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The BepiColombo is an international Mercury exploring mission which will be launched in 2014 and reach the planet in 2020. In this paper, we show the development status of the extreme ultraviolet (50-155 nm) detector for the mission. We have optimized the geometry of the micro channel plate that can achieve highest quantum detection efficiency. Furthermore, we have evaluated the quantum detection efficiencies of cesium iodide-coated micro channel plate which have been exposed to the air or dry nitrogen, in order to determine the treatment procedure to prevent performance degradation until the launch.

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Section: Discussionmentioning

confidence: 99%

Optimization of the MCP Detector for the BepiColombo Mission

Yoshioka

Murakami

Yoshikawa

2009

Trans. JSASS Space Tech. Japan

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“…The core scientific objectives of PHEBUS [1], are oriented toward a better understanding of the coupled surface-exosphere-magnetosphere system. The main measurement objectives are the following: -To detect new species, including metallic species (Si, Mg, Fe, …), atoms (C, N, S, …), molecules and radicals (H 2 O, H 2 , OH, CO), noble gases (Ar, Ne), ions (He + , Na + , Mg + , …), in addition to already detected species (Na, K, Ca, O, H, He).…”

Section: B Measurement Objectivesmentioning

confidence: 99%

Probing of Hermean Exosphere by ultraviolet spectroscopy: Instrument presentation, calibration philosophy and first lights results

Mariscal

Rouanet

Maria

et al. 2017

International Conference on Space Optics — ICSO 2010

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PHEBUS (Probing of Hermean Exosphere by Ultraviolet Spectroscopy) is a double spectrometer for the Extreme Ultraviolet range (55-155 nm) and the Far Ultraviolet range (145-315 nm) dedicated to the characterization of Mercury's exosphere composition and dynamics, and surface-exosphere connections. PHEBUS is part of the ESA BepiColombo cornerstone mission payload devoted to the study of Mercury. The BepiColombo mission consists of two spacecrafts: the Mercury Magnetospheric Orbiter (MMO) and the Mercury Planetary Orbiter (MPO) on which PHEBUS will be mounted. PHEBUS is a French-led instrument implemented in a cooperative scheme involving Japan (detectors), Russia (scanner) and Italy (ground calibration). Before launch, PHEBUS team want to perform a full absolute calibration on ground, in addition to calibrations which will be made in-flight, in order to know the instrument's response as precisely as possible. Instrument overview and calibration philosophy are introduced along with the first lights results observed by a first prototype.

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“…It is highly probable that other elements, such as C, N, S, OH, Al, and Fe are also present. The exosphere of Mercury will be further investigated by BepiColombo mission (Chassefière et al 2010;Yoshikawa et al 2010a). EXCEED will search for predicted species, C and N have emission lines in EUV, not previously detected, as well as new species.…”

Section: Third Target: Mercury and Saturnmentioning

confidence: 99%

“…It was based on our technological advances in the extreme ultraviolet (EUV) spectral range during the past two decades (e.g. Yoshikawa et al 1997Yoshikawa et al , 2001Yoshikawa et al , 2005Yoshikawa et al , 2010bYoshioka et al 2012;Chassefière et al 2010). We have enabled quantitative spectroscopy to provide detailed information on neutral and ionized gases of atmospheric and astrophysical interest.…”

Section: Introduction: Mission Backgroundmentioning

confidence: 99%

Extreme Ultraviolet Radiation Measurement for Planetary Atmospheres/Magnetospheres from the Earth-Orbiting Spacecraft (Extreme Ultraviolet Spectroscope for Exospheric Dynamics: EXCEED)

et al. 2014

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The Sprint-A satellite with the EUV spectrometer (Extreme Ultraviolet Spectroscope for Exospheric Dynamics: EXCEED) was launched in September 2013 by the Epsilon rocket. Now it is orbiting around the Earth (954.05 km × 1156.87 km orbit; the period is 104 minutes) and one has started a broad and varied observation program. With an effective area of more than 1 cm 2 and well-calibrated sensitivity in space, the EUV spectrometer will produce spectral images (520-1480 Å) of the atmospheres/magnetospheres of several planets (Mercury, Venus, Mars, Jupiter, and Saturn) from the Earth's orbit. At the first day of the observation, EUV emissions from the Io plasma torus (mainly sulfur ions) and aurora (H 2 Lyman and Werner bands) of Jupiter have been identified. Continuous 3-month measurement for Io's plasma torus and aurora is planned to witness the sporadic and sudden brightening events occurring on one or both regions. For Venus, the Fourth Positive (A 1 Π -X 1 Σ + ) system of CO and some yet known emissions of the atmosphere were identified even though the exposure was short (8-min). Long-term exposure from April to June (for approximately 2 months) will visualize the Venusian ionosphere and tail in the EUV spectral range. Saturn and Mars are the next targets.

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PHEBUS: A double ultraviolet spectrometer to observe Mercury's exosphere

Cited by 45 publications

References 33 publications

Optimization of the MCP Detector for the BepiColombo Mission

Optimization of the MCP Detector for the BepiColombo Mission

Probing of Hermean Exosphere by ultraviolet spectroscopy: Instrument presentation, calibration philosophy and first lights results

Extreme Ultraviolet Radiation Measurement for Planetary Atmospheres/Magnetospheres from the Earth-Orbiting Spacecraft (Extreme Ultraviolet Spectroscope for Exospheric Dynamics: EXCEED)

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