Asteroid target selection for the new Rosetta mission baseline

Barucci, Maria Antonietta; Fulchignoni, M.; Fornasier, S.; Dotto, E.; Vernazza, Pierre; Birlan, Mirel; Binzel, Richard P.; Carvano, J. M.; Merlin, F.; Barbieri, C.; Belskaya, I. N.

doi:10.1051/0004-6361:20041505

Cited by 88 publications

(109 citation statements)

References 21 publications

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“…The carbonaceous-chondrite analogy and the affinity for C-type remains incompatible with the high IRAS albedo value reconfirmed by Mueller et al (2006) from thermalinfrared spectrophotometric measurements and thermal modeling (p V = 0.208 ± 0.025). Interestingly, Lazzarin et al (2004) found in the 0.38−0.95 µm a rather flat spectrum unlike those obtained by Bus (1999), Carvano et al (2003), and Barucci et al (2005) and two main absorption bands around 0.43 µm and 0.51 µm, features not reported before. Variegation of spectral features with rotational phase and sub-Earth coordinates was then proposed as an explanation for these contradictory results.…”

Section: Introductioncontrasting

confidence: 58%

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Near infra-red spectroscopy of the asteroid 21 Lutetia

Nedelcu

Birlan²,

Vernazza³

et al. 2007

A&A

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Aims. In the framework of the ground-based science campaign dedicated to the encounter with the Rosetta spacecraft, the mineralogy of the asteroid (21) Lutetia was investigated. Methods. Near-infrared (NIR) spectra of the asteroid in the 0.8−2.5 µm spectral range were obtained with SpeX/IRTF in remote observing mode from Meudon, France in March and April 2006. We analysed these data together with previously acquired spectra -March 2003, August 2004. I-band relative photometric data obtained on 20 January 2006 using the 105 cm telescope from Pic du Midi, France has been used to build the ephemeris for physical observations. A χ 2 test using meteorite spectra from the RELAB database was performed in order to find the best fit of complete visible + infrared (VNIR) spectra of Lutetia. Results. The new spectra reveal no absorption features. We find a clear spectral variation (slope), and a good correspondence between spectral variations and rotational phase. Two of the most different spectra correspond to two opposite sides of the asteroid (sub-Earth longitude difference around 180 • ). For the neutral spectra a carbonaceous chondrite spectrum yields the best fit, while for those with a slightly positive slope the enstatitic chondrite spectra are the best analog. Based on the chosen subset of the meteorite samples, our analysis suggests a primitive, chondritic nature for (21) Lutetia. Differences in spectra are interpreted in terms of the coexistence of several lithologies on the surface where the aqueous alteration played an important role.

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Section: Introductioncontrasting

confidence: 58%

“…The VNIR spectra were constructed by means of visible spectra obtained by Barucci et al (2005) using their overlapping region (0.82−0.95 µm). Our choice for the above V spectrum was based on its similarities with previously published ones (Bus 1999;Carvano et al 2003).…”

Section: Comparison With Laboratory Spectramentioning

confidence: 99%

Near infra-red spectroscopy of the asteroid 21 Lutetia

Nedelcu

Birlan²,

Vernazza³

et al. 2007

A&A

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“…Numerous researchers in the last few years (Barucci et al 2005(Barucci et al , 2008Lazzarin et al 2009;Perna et al 2010; see summary by Belskaya et al 2010) have argued that Lutetia shows certain spectral characteristics (e.g., in the thermal IR) that resemble several CO and CV meteorites, but not an iron meteorite. However, mineralogical interpretations of thermal IR spectra must be made cautiously because particle size, in addition to composition, can strongly affect the observed spectral features (Vernazza et al 2010).…”

Section: Discussionmentioning

confidence: 99%

Ultraviolet and visible photometry of asteroid (21) Lutetia using the Hubble Space Telescope

Weaver¹,

Feldman²,

Merline³

et al. 2010

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Context. The asteroid (21) Lutetia is the target of a planned close encounter by the Rosetta spacecraft in July 2010. To prepare for that flyby, Lutetia has been extensively observed by a variety of astronomical facilities. Aims. We used the Hubble Space Telescope (HST) to determine the albedo of Lutetia over a wide wavelength range, extending from ∼1500 Å to ∼7000 Å. Methods. Using data from a variety of HST filters and a ground-based visible light spectrum, we employed synthetic photometry techniques to derive absolute fluxes for Lutetia. New results from ground-based measurements of Lutetia's size and shape were used to convert the absolute fluxes into albedos. Results. We present our best model for the spectral energy distribution of Lutetia over the wavelength range 1200−8000 Å. There appears to be a steep drop in the albedo (by a factor of ∼2) for wavelengths shorter than ∼3000 Å. Nevertheless, the far ultraviolet albedo of Lutetia (∼10%) is considerably larger than that of typical C-chondrite material (∼4%). The geometric albedo at 5500 Å is 16.5 ± 1%. Conclusions. Lutetia's reflectivity is not consistent with a metal-dominated surface at infrared or radar wavelengths, and its albedo at all wavelengths (UV-visibile-IR-radar) is larger than observed for typical primitive, chondritic material. We derive a relatively high FUV albedo of ∼10%, a result that will be tested by observations with the Alice spectrograph during the Rosetta flyby of Lutetia in July 2010.

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“…However, several weak features (e.g., around 0.9 µm) have been identified and used to discriminate sub-classes Ockert-Bell et al 2010;Fornasier et al 2011). Proposed meteorite analogs for X, Xc, Xe, and Xk asteroids virtually cover the entire meteorite collection: the anhydrous CV/CO carbonaceous chondrites (Barucci et al 2005(Barucci et al , 2012, enstatite chondrites and aubrites (Vernazza et al 2009b(Vernazza et al , 2011bOckert-Bell et al 2010), mesosiderites (Vernazza et al 2009b), stony-iron (Ockert-Bell et al 2010), and iron meteorites (Fornasier et al 2011). The mineralogy represented in the X-complex is therefore probably more diverse than in the S-and C-complexes, due to the limits of the taxonomy based on spectral features only.…”

Section: Linking Small Bodies With Meteoritesmentioning

confidence: 99%

Density of asteroids

Carry

2012

Planetary and Space Science

506

444

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The small bodies of our solar system are the remnants of the early stages of planetary formation. A considerable amount of information regarding the processes that occurred during the accretion of the early planetesimals is still present among this population. A review of our current knowledge of the density of small bodies is presented here. Density is indeed a fundamental property for the understanding of their composition and internal structure. Intrinsic physical properties of small bodies are sought by searching for relationships between the dynamical and taxonomic classes, size, and density. Mass and volume estimates for 287 small bodies (asteroids, comets, and transneptunian objects) are collected from the literature. The accuracy and biases affecting the methods used to estimate these quantities are discussed and best-estimates are strictly selected. Bulk densities are subsequently computed and compared with meteorite density, allowing to estimate the macroporosity (i.e., amount of voids) within these bodies. Dwarf-planets apparently have no macroporosity, while smaller bodies (<400 km) can have large voids. This trend is apparently correlated with size: C and S-complex asteroids tends to have larger density with increasing diameter. The average density of each Bus-DeMeo taxonomic classes is computed (DeMeo et al., 2009, Icarus 202). S-complex asteroids are more dense on average than those in the C-complex that in turn have a larger macroporosity, although both complexes partly overlap. Within the C-complex asteroids, B-types stand out in albedo, reflectance spectra, and density, indicating a unique composition and structure. Asteroids in the Xcomplex span a wide range of densities, suggesting that many compositions are included in the complex. Comets and TNOs have high macroporosity and low density, supporting the current models of internal structures made of icy aggregates. Although the number of density estimates sky-rocketed during last decade from a handful to 287, only a third of the estimates are more precise than 20%. Several lines of investigation to refine this statistic are contemplated, including observations of multiple systems, 3-D shape modeling, and orbital analysis from Gaia astrometry.Keywords: Minor planets, Mass, Volume, Density, Porosity Small bodies as remnants of planetesimalsThe small bodies of our solar System are the left-overs of the building blocks that accreted to form the planets, some 4.6 Gyr ago. They represent the most direct witnesses of the conditions that reigned in the proto-planetary nebula (Bottke et al. 2002a). Indeed, terrestrial planets have thermally evolved and in some cases suffered erosion (e.g., plate tectonic, volcanism) erasing evidence of their primitive composition. For most small bodies, however, their small diameter limited the amount of radiogenic nuclides in their interior, and thus the amount of energy for internal heating. The evolution of small bodies is therefore mainly exogenous, through eons of collisions, external heating, and bombardm...

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Asteroid target selection for the new Rosetta mission baseline

Cited by 88 publications

References 21 publications

Near infra-red spectroscopy of the asteroid 21 Lutetia

Near infra-red spectroscopy of the asteroid 21 Lutetia

Ultraviolet and visible photometry of asteroid (21) Lutetia using the Hubble Space Telescope

Density of asteroids

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