| 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 | |
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.