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Erratum
This article is an erratum for:
[https://doi.org/10.1051/0004-6361/201015851]


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.

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.

References

  1. Jones, T., Lebofsky, L., Lewis, J., & Marley, M. 1990, Icarus, 88, 172 [NASA ADS] [CrossRef] [Google Scholar]
  2. Milliken, R. E., & Rivkin, A. S. 2009, Nature Geoscience, 2, 258 [NASA ADS] [CrossRef] [Google Scholar]
  3. Rivkin, A. S., & Emery, J. P. 2010, Nature, 464, 1322 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]

© 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.

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.

In the text

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