Observations of Phobos and Deimos with SpeX at NASA infrared telescope facility

Takir, D.; Matsuoka, Moe; Waiters, A.; Kaluna, H. M.; Usui, Tomohiro

doi:10.1016/j.icarus.2021.114691

Cited by 6 publications

(6 citation statements)

References 46 publications

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“…These findings were partially confirmed by recent observations published by Takir et al ( 2022 ), who confirm the strong similarity between Deimos spectrum and the Phobos red unit one, suggesting a similarity to D-type asteroids. They ho we ver detect a 3-μm band with a depth of 4 -5 per cent on Deimos spectrum can be attributed to hydrated minerals in the bulk composition, to OH implanted from solar wind (Nakauchi et al 2021 ) or even to delivery of hydrated exogenic material (McCord et al 2012 ).…”

Section: Spectroscopic Obser V Ations Of Phobos and Deimossupporting

confidence: 85%

“…They ho we ver detect a 3-μm band with a depth of 4 -5 per cent on Deimos spectrum can be attributed to hydrated minerals in the bulk composition, to OH implanted from solar wind (Nakauchi et al 2021 ) or even to delivery of hydrated exogenic material (McCord et al 2012 ). Surprisingly no indication of mafic composition arises from their observations (Takir et al 2022 ). Authors also report surface heterogeneities on Phobos, with a significant slope variation at shorter wavelengths possibly linked with different regolith's composition, and/or space weathering degree (Takir et al 2022 ).…”

Section: Spectroscopic Obser V Ations Of Phobos and Deimosmentioning

confidence: 85%

“…Surprisingly no indication of mafic composition arises from their observations (Takir et al 2022 ). Authors also report surface heterogeneities on Phobos, with a significant slope variation at shorter wavelengths possibly linked with different regolith's composition, and/or space weathering degree (Takir et al 2022 ). Observations in the range of 1 -13 μm for Deimos and 3 -13 μm for Phobos revealed higher than expected temperatures but consistent with previous observations while, within the errors, there was little evidence for spectral features indicative of surface composition (Lynch et al 2007 ).…”

Section: Spectroscopic Obser V Ations Of Phobos and Deimosmentioning

confidence: 94%

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Phobos and Deimos surface composition: search for spectroscopic analogues

Poggiali

Matsuoka

Barucci

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Phobos and Deimos, the two satellites of Mars were largely studied in the past using ground-based telescope and spacecraft data, although most of the data were obtained by opportunity observations performed by Mars dedicated orbiters. Despite the data available so far, the main composition of the two moons is not yet fully understood. The possible presence of hydrated minerals along with mafic minerals olivine and pyroxene seems to be the most plausible interpretation, but more investigations are needed. MIRS spectrometer onboard the future JAXA MMX sample return mission will help to unveil the open question on the composition of Phobos and Deimos. In this work we review past spectroscopic observations of the Martian moons, both from ground observatories and spacecraft dataset, aiming at better understanding the constraints in interpreting the Mars satellites composition and at identifying the best spectroscopic analogs. We also present new laboratory measurements on mineral mixing and meteorites to match the satellites spectral behaviour. New measurements were acquired at INAF-Astrophysical Observatory of Arcetri and IPAG laboratories at room conditions exploring different geometries and the results obtained set new constraints for future laboratory measurements. Our preliminary results confirm that the surface of Phobos and Deimos can be associated with samples characterized by an higher presence of dark components (e.g. amorphous carbon) or minerals produced by space weathering (e.g. Fe0 and FeS-bearing materials). Presence of dark component could be also totally responsible for the reduced hydrated band observed on the moons without invoking dehydration or OH-implantation on anhydrous surface.

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Section: Spectroscopic Obser V Ations Of Phobos and Deimossupporting

confidence: 85%

Section: Spectroscopic Obser V Ations Of Phobos and Deimosmentioning

confidence: 85%

Section: Spectroscopic Obser V Ations Of Phobos and Deimosmentioning

confidence: 94%

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Phobos and Deimos surface composition: search for spectroscopic analogues

Poggiali

Matsuoka

Barucci

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“… 10 This means that minerals like pyroxene and olivine should be visible in the spectrum of the formed moons, but this does not seem to be the case; no absorption features indicative of pyroxene and olivine were detected on both Deimos and Phobos. 84 , 91 It was pointed out since the Viking missions that even a bulk density of 2.0 ± 0.6 g cm −3 would have ruled out any basaltic composition. 92 …”

Section: Igneous Processes In Small Satellites Of the Solar Systemmentioning

confidence: 99%

Igneous processes in the small bodies of the Solar System II: Small satellites and dwarf planets

Leone,

Tanaka

2024

iScience

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“…Several in situ and ground-based observations have shown that Phobos and Deimos -the two martian moons -are small bodies respectively of about 27 and 15 km, highly processed, cratered, with a red and flat near-infrared spectrum (Murchie & Erard 1996;Murchie 1999;Rivkin et al 2002;Fraeman et al 2012Fraeman et al , 2014Pajola et al 2012Pajola et al , 2018Takir et al 2022). These peculiar characteristics for a moon in the Solar System led to suppose that Phobos and Deimos could be D-type asteroids captured from the main asteroid belt (Rivkin et al 2002;Fraeman et al 2014).…”

Section: Contextmentioning

confidence: 99%

Development of a new Phobos spectral simulant: spectral properties from visible to the mid-infrared range

Wargnier

Poggiali

Doressoundiram

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Phobos is the target of Martian Moons eXploration (MMX) the next sample return mission of the Japanese space agency (JAXA). The mission will investigate the origin of Phobos and Deimos – the two martian moons, using a suite of dedicated instruments. Infrared analysis of the surface composition will be performed by the MIRS spectrometer onboard MMX. Within the scientific studies performed in preparation of the mission, we developed a new laboratory spectral simulant that well reproduces the red and featureless spectrum of Phobos. Our results show that a visible and near-infrared simulant can be developed using dark opaque materials such as anthracite and coal to reduce the reflectance and absorption features. To investigate the reliability of our proposed simulant in terms of composition and mineralogy we discussed the similarities and differences in the mid-infrared (MIR) range between our laboratory simulant and some past observations acquired on Phobos. Spectra with different observation geometries were also acquired for our simulant which gives information about grain size and textures of the surface. The simulant developed in our study presents a better match for the Phobos spectrum in the visible and near-infrared compared to the previously proposed simulants.

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Observations of Phobos and Deimos with SpeX at NASA infrared telescope facility

Cited by 6 publications

References 46 publications

Phobos and Deimos surface composition: search for spectroscopic analogues

Phobos and Deimos surface composition: search for spectroscopic analogues

Igneous processes in the small bodies of the Solar System II: Small satellites and dwarf planets

Development of a new Phobos spectral simulant: spectral properties from visible to the mid-infrared range

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