Hydration state of the Martian surface as seen by Mars Express OMEGA: 2. H2O content of the surface

By Ralph E. Milliken, J. F. Mustard, François Poulet, D. Jouglet, J. Bibring, B. Gondet, Yves Langevin. 2007

133 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/b34c9dc4739eaf7740c771e8971be72e2bdcc3a0

How researchers see this paper

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In Aerospace Engineering

1. François Poulet
2. Yves Langevin
3. Francois Forget
4. B. Gondet
5. F. Montmessin
6. J. Bibring
7. R. Wordsworth

In Astronomy and Astrophysics

1. J. Bibring
2. Francois Forget
3. Yves Langevin
4. B. Gondet
5. F. Montmessin
6. François Poulet
7. R. Wordsworth
8. Ehouarn Millour

Citations in the corpus

• Observations of the south seasonal cap of Mars during recession in 2004–2006 by the OMEGA visible/near‐infrared imaging spectrometer on board Mars Express (2007, background): “Furthermore, spectral identifications are made more complex by the low S/N (Figure 4) and the deep hydration band at 3 mm which is observed for all surface materials as well as in aerosols [Jouglet et al., 2007; Milliken et al., 2007 ].”
• The Sedimentary Rock Record of Mars: Distribution, Origins, and Global Stratigraphy (2012, unknown): “For reference, typical dusty regions on Mars exhibit 2 to 4 wt. % H2O, as seen by OMEGA (Milliken et al. 2007).”