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Erratum
This article is an erratum for: [this article]

Issue
A&A
Volume 530, June 2011
Article Number C2
Number of page(s) 1
Section Planets and planetary systems
DOI https://doi.org/10.1051/0004-6361/201015851e
Published online 11 May 2011

An error occurred during the production process. Figure 1 was published twice. The corrected Figs. 1 and 4 are published below.

thumbnail Fig. 1

NIR spectra of a eucrite (Millbillillie) and a diogenite powder (Dhofar700) showing the absence of significant H2O- related 3-μm band upon heating to 80   °C and in a moderate vacuum (P = 10-3 mbar). Note the presence of a 3.1 μm band in the spectrum of Dhofar 700. From its shape and position, this feature may be caused by a small amount of goethite produced by terrestrial weathering. The small absorption at 3.4 μm is likely due to the presence of organic contamination.

Open with DEXTER

thumbnail Fig. 4

Different types of 3-μm band as observed on asteroids. 1-Ceres spectrum is from Milliken & Rivkin (2009), 2-Pallas spectrum is from Jones et al. (1990), and 24-Themis data are from Rivkin & Emery (2010). Spectra have been offset and rescaled for clarity.

Open with DEXTER

References


© ESO, 2011

All Figures

thumbnail Fig. 1

NIR spectra of a eucrite (Millbillillie) and a diogenite powder (Dhofar700) showing the absence of significant H2O- related 3-μm band upon heating to 80   °C and in a moderate vacuum (P = 10-3 mbar). Note the presence of a 3.1 μm band in the spectrum of Dhofar 700. From its shape and position, this feature may be caused by a small amount of goethite produced by terrestrial weathering. The small absorption at 3.4 μm is likely due to the presence of organic contamination.

Open with DEXTER
In the text
thumbnail Fig. 4

Different types of 3-μm band as observed on asteroids. 1-Ceres spectrum is from Milliken & Rivkin (2009), 2-Pallas spectrum is from Jones et al. (1990), and 24-Themis data are from Rivkin & Emery (2010). Spectra have been offset and rescaled for clarity.

Open with DEXTER
In the text

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