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 |
Goethite as an alternative origin of the 3.1 μm band on dark asteroids (Corrigendum)
1
Laboratoire de Planétologie de Grenoble (LPG/IPAG), Université J. Fourier, CNRS/INSU, UMR5109, OSUG, Université Joseph Fourier, 122 rue de la Piscine, 38041 Grenoble Cedex 9, France
e-mail: pierre.beck@obs.ujf-grenoble.fr
2
Institut des Sciences de la Terre (IsTerre), Université J. Fourier, CNRS/INSU, 1381 rue de la piscine, 38041 Grenoble Cedex, France
3
Space Research & Planetary Sciences Division, Physikalisches Institut-Universitaet Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
Key words: meteorites, meteors, meteoroids / minor planets, asteroids: general / minor planets, asteroids: individual: 24-themis / minor planets, asteroids: individual: 1-ceres / errata, addenda
An error occurred during the production process. Figure 1 was published twice. The corrected Figs. 1 and 4 are published below.
![]() |
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. |
![]() |
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
- Jones, T., Lebofsky, L., Lewis, J., & Marley, M. 1990, Icarus, 88, 172 [NASA ADS] [CrossRef] [Google Scholar]
- Milliken, R. E., & Rivkin, A. S. 2009, Nature Geoscience, 2, 258 [NASA ADS] [CrossRef] [Google Scholar]
- Rivkin, A. S., & Emery, J. P. 2010, Nature, 464, 1322 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
© ESO, 2011
All Figures
![]() |
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 |
![]() |
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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