The D-CIXS X-ray spectrometer on the SMART-1 mission to the Moon—First results

Grandé, M.; Kellett, B. J.; Howe, C.; Perry, C. H.; Swinyard, Bruce; Dunkin, S. K.; Huovelin, J.; Alha, L.; d’Uston, L.; Maurice, S.; Gasnault, O.; Couturier-Doux, S.; Barabash, S.; Joy, K. H.; Crawford, Ian; Lawrence, D. J.; Fernandes, V. A.; Casanova, I.; Wieczorek, M. A.; Thomas, N.; Mall, U.; Foing, B.; Hughes, David W.; Alleyne, H.; Russell, S. S.; Grady, M. M.; Lundin, R.; Baker, D. M. H.; Murray, C. D.; Guest, J. E.; Christou, Apostolos

doi:10.1016/j.pss.2006.08.004

Cited by 43 publications

(15 citation statements)

References 12 publications

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“…Major elemental mapping in planets can be carried out with concurrent observation of X-rays from the Sun and the planet, as was proven in the Apollo 15 and 16 missions (e.g., Adler and Trombka, 1977). This method has also been used in planetary missions such as the Near-Earth Asteroid Rendezvous-Shoemaker (Trombka et al, 2000;Nittler et al, 2001), Hayabusa , and SMART-1 (Kellett et al, 2006;Grande et al, 2007).…”

Section: Introductionmentioning

confidence: 99%

Laboratory experiments of particle size effect in X-ray fluorescence and implications to remote X-ray spectrometry of lunar regolith surface

et al. 2008

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We performed laboratory experiments to investigate the effect of particle size in X-ray fluorescence (XRF) with respect to interpreting remote X-ray spectrometry. To simulate microscopic roughness of the uppermost surface of lunar regolith, we used powdery specimens of crashed rocks ranging 25 to 500 μm in size and flat rock plates for comparison. Our results show that XRF intensities from powdery specimens decrease relative to those from flat plates by up to 50%, especially for larger particle size and at increasing source-to-surface-to-detector angle (phase angle). Corrections should be required for elemental analysis by XRF spectrometry in the SELENE "Kaguya" and other planetary orbiter missions.

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Section: Introductionmentioning

confidence: 99%

Laboratory experiments of particle size effect in X-ray fluorescence and implications to remote X-ray spectrometry of lunar regolith surface

et al. 2008

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“…The detector plane of the instrument consists of twenty four e2v technologies CCD54 swept-charge devices (SCDs). Such devices were first flown in the Demonstration of a Compact Imaging X-ray Spectrometer (D-CIXS) instrument onboard SMART-1 [4,5]. The detector plane in each case provides a total X-ray collection area of 26.4 cm 2 .…”

Section: Introductionmentioning

confidence: 99%

Radiation study of swept-charge devices for the Chandrayaan-1 X-ray Spectrometer (C1XS) instrument

et al. 2008

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The Chandrayaan-1 X-ray Spectrometer (C1XS) will be launched as part of the Indian Space Research Organisation (ISRO) Chandrayaan-1 payload in September 2008, arriving at the Moon within 7 days to begin a two year mission in lunar orbit conducting mineralogical surface mapping over the range of 1 -10 keV. The detector plane of the instrument consists of twenty four e2v technologies CCD54 swept-charge devices (SCDs). Such devices were first flown in the Demonstration of a Compact Imaging X-ray Spectrometer (D-CIXS) instrument onboard SMART-1 [4,5]. The detector plane in each case provides a total X-ray collection area of 26.4 cm 2 . The SCD is capable of providing near Fano-limited spectroscopy at -10 o C, and at -20 o C, near the Chandrayaan-1 mission average temperature, it achieves a total system noise of 6.2 electrons r.m.s. and a FWHM of 134 eV at Mn-Kα. This paper presents a brief overview of the C1XS mission and a detailed study of the effects of proton irradiation on SCD operational performance.

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“…The D-CIXS's initial observation over Mare Crisium and nearby highland area took place during occurrence of M-class solar flare (Kellett et al, 2006). The spectra obtained during this period are reported to indicate the first unambiguous detection of Calcium from the lunar surface (Grande et al, 2007).…”

Section: Introductionmentioning

confidence: 85%

“…More recently the European Space Agency's SMART-1 mission carried the Demonstration of a Compact Imaging X-ray Spectrometer (D-CIXS), which also performed x-ray spectroscopic remote observation of lunar surface (Grande et al, 2007). The D-CIXS instrument uses swept charge device (SCD) array as a main detector (Grande, 2001).…”

Section: Introductionmentioning

confidence: 99%

Instrumentation and performance evaluation of the XRS on SELENE orbiter

et al. 2008

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The x-ray fluorescence spectrometer (XRS) on board Japanese lunar polar orbiter SELENE (Kaguya) will provide global distribution of major elemental composition on the lunar surface in energy range of characteristic K-α x-ray line emission for Mg, Al, Si, Ca, Ti, and Fe. These measurements will contribute to research of lunar origin and its evolution. The XRS shows a good energy resolution within 200 eV at 5.9 keV relying on charge coupled device (CCD) as photon energy dispersive detector. Total collective area of 100 cm 2 for main detector facing the lunar surface is composed of 16 CCD chips. Instrumentation of the XRS and its performance evaluated in laboratory are presented.

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The D-CIXS X-ray spectrometer on the SMART-1 mission to the Moon—First results

Cited by 43 publications

References 12 publications

Laboratory experiments of particle size effect in X-ray fluorescence and implications to remote X-ray spectrometry of lunar regolith surface

Laboratory experiments of particle size effect in X-ray fluorescence and implications to remote X-ray spectrometry of lunar regolith surface

Radiation study of swept-charge devices for the Chandrayaan-1 X-ray Spectrometer (C1XS) instrument

Instrumentation and performance evaluation of the XRS on SELENE orbiter

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