Spectroscopic observations of Jupiter Trojans

Bendjoya, Philippe; Cellino, A.; Martino, M. Di; Saba, L.

doi:10.1016/j.icarus.2003.12.004

Cited by 34 publications

(64 citation statements)

References 13 publications

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“…Three of our targets (4035, 6545 and 11351) were already observed by Dotto et al (2006): for 6545 and 11351 there is a good consistency between our spectra and those already published. 4035 was observed also by Bendjoya et al (2004): all the spectra are featureless, but Bendjoya et al (2004) obtain a slope of 8.8 %/10 3Å , comparable to the one here presented, while Dotto et al (2006) found a higher value (see Table 5). This could be interpreted as due to the different rotational phases seen in the three observations, and could indicate some inhomogeneities on the surface of 4035.…”

Section: Wd [Figure 6]supporting

confidence: 87%

“…Our spectrum has a higher S/N ratio than the spectrum by Bendjoya et al (2004), and it is perfectly matched by our measured color indices that confirm the spectral slope. This difference cannot be caused by the slightly different spectral ranges used to measure the slope, but could possibly be due to heterogeneous surface composition.…”

Section: åsupporting

confidence: 82%

“…7). 5511 Cloanthus was observed also by Bendjoya et al (2004), who found a slope of 13.0±0.1 %/10 3Å in the 5000-7500Å wavelength range, while we measure a value of 10.84±0.15 %/10…”

Section: [Figure 4]supporting

confidence: 74%

“…We performed the taxonomic classification of this enlarged sample, on the basis of the Dahlgren and Lagerkvist (1995) scheme, by analyzing spectral slopes computed in the range 5500-8000Å. Different authors, of course, considered different spectral ranges for their own slope gradient evaluations: Jewitt & Luu (1990) and Fitzimmons et al (1994) use the 4000-7400Å and Bendjoya et al (2004, Table 2) used a slightly different ranges around 5200-7500Å. Since all the cited papers show spectra with linear featureless trends, the different wavelength ranges used for the spectral gradient computation by Bendjoya et al (2004) and Jewitt & Luu (1990) are not expected to influence the obtained slopes.…”

Section: Size Vs Spectral Slope Distribution: Individual Familiesmentioning

confidence: 99%

“…Several observations of Trojans in the near infrared region (0.8-2.5 µm) have failed to clearly detect any absorption features indicative of water ice (Barucci et al, 1994;Dumas et al, 1998;Emery & Brown, 2003Dotto et al, 2006). Also in the visible range Trojan spectra appear featureless (Jewitt & Luu, 1990;Fornasier et al, 2004a, Bendjoya et al, 2004Dotto et al, 2006). Up to now only 2 objects (1988 BY1 and1870 Glaukos) show the possible presence of faint bands (Jewitt & Luu, 1990).…”

Section: Introductionmentioning

confidence: 98%

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Visible spectroscopic and photometric survey of Jupiter Trojans: Final results on dynamical families☆

Fornasier

Dotto

Hainaut

et al. 2007

Icarus

103

158

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We present the results of a visible spectroscopic and photometric survey of Jupiter Trojans belonging to different dynamical families. The survey was carried out at the 3.5m New Technology Telescope (NTT) of the European Southern Observatory (La Silla, Chile) in April 2003, May 2004 and January 2005. We obtained data on 47 objects, 23 belonging to the L5 swarm and 24 to the L4 one. These data together with those already published by Fornasier et al. (2004a) and Dotto et al. (2006), acquired since November 2002, constitute a total sample of visible spectra for 80 objects. The survey allows us to investigate six families (Aneas, Anchises, Misenus, Phereclos, Sarpedon, Panthoos) in the L5 cloud and four L4 families (Eurybates, Menelaus, 1986 WD and 1986 TS6). The sample that we measured is dominated by D-type asteroids, with the exception of the Eurybates family in the L4 swarm, where there is a dominance of C-and P-type asteroids. All the spectra that we obtained are featureless with the exception of some Eurybates members, where a drop-off of the reflectance is detected shortward of 5200Å. Similar features are seen in main belt C-type asteroids and commonly attributed to the intervalence charge transfer transition in oxidized iron. Our sample comprises fainter and smaller Trojans as compared to the literature's data and allows us to investigate the properties of objects with estimated diameter smaller than 40-50 km. The analysis of the spectral slopes and colors versus the estimated diameters shows that the blue and red objects have indistinguishable size distribution, so any relationship between size and spectral slopes has been found. To fully investigate the Trojans population, we include in our analysis 62 spectra of Trojans available in literature, resulting in a total sample of 142 objects. Although the mean spectral behavior of L4 and L5 Trojans is indistinguishable within the uncertainties, we find that the L4 population is more heterogeneous and that it has a higher abundance of bluish objects as compared to the L5 swarm. Finally, we perform a statistical investigation of the Trojans's spectra property distributions as a function of their orbital and physical parameters, and in comparison with other classes of minor bodies in the outer Solar System. Trojans at lower inclination appear significantly bluer than those at higher inclination, but this effect is strongly driven by the Eurybates family. The mean colors of the Trojans are similar to those of short period comets and neutral Centaurs, but their color distributions are different.

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Section: Wd [Figure 6]supporting

confidence: 87%

Section: åsupporting

confidence: 82%

“…7). 5511 Cloanthus was observed also by Bendjoya et al (2004), who found a slope of 13.0±0.1 %/10 3Å in the 5000-7500Å wavelength range, while we measure a value of 10.84±0.15 %/10…”

Section: [Figure 4]supporting

confidence: 74%

Section: Size Vs Spectral Slope Distribution: Individual Familiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

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Visible spectroscopic and photometric survey of Jupiter Trojans: Final results on dynamical families☆

Fornasier

Dotto

Hainaut

et al. 2007

Icarus

103

158

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Exploring the Bimodal Solar System via Sample Return from the Main Asteroid Belt: The Case for Revisiting Ceres

Burbine

Greenwood

2020

Space Sci Rev

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Sample return from a main-belt asteroid has not yet been attempted, but appears technologically feasible. While the cost implications are significant, the scientific case for such a mission appears overwhelming. As suggested by the “Grand Tack” model, the structure of the main belt was likely forged during the earliest stages of Solar System evolution in response to migration of the giant planets. Returning samples from the main belt has the potential to test such planet migration models and the related geochemical and isotopic concept of a bimodal Solar System. Isotopic studies demonstrate distinct compositional differences between samples believed to be derived from the outer Solar System (CC or carbonaceous chondrite group) and those that are thought to be derived from the inner Solar System (NC or non-carbonaceous group). These two groups are separated on relevant isotopic variation diagrams by a clear compositional gap. The interface between these two regions appears to be broadly coincident with the present location of the asteroid belt, which contains material derived from both groups. The Hayabusa mission to near-Earth asteroid (NEA) (25143) Itokawa has shown what can be learned from a sample-return mission to an asteroid, even with a very small amount of sample. One scenario for main-belt sample return involves a spacecraft launching a projectile that strikes an object and flying through the debris cloud, which would potentially allow multiple bodies to be sampled if a number of projectiles are used on different asteroids. Another scenario is the more traditional method of landing on an asteroid to obtain the sample. A significant range of main-belt asteroids are available as targets for a sample-return mission and such a mission would represent a first step in mineralogically and isotopically mapping the asteroid belt. We argue that a sample-return mission to the asteroid belt does not necessarily have to return material from both the NC and CC groups to viably test the bimodal Solar System paradigm, as material from the NC group is already abundantly available for study. Instead, there is overwhelming evidence that we have a very incomplete suite of CC-related samples. Based on our analysis, we advocate a dedicated sample-return mission to the dwarf planet (1) Ceres as the best means of further exploring inherent Solar System variation. Ceres is an ice-rich world that may be a displaced trans-Neptunian object. We almost certainly do not have any meteorites that closely resemble material that would be brought back from Ceres. The rich heritage of data acquired by the Dawn mission makes a sample-return mission from Ceres logistically feasible at a realistic cost. No other potential main-belt target is capable of providing as much insight into the early Solar System as Ceres. Such a mission should be given the highest priority by the international scientific community.

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Surface Compositions of Trojan Asteroids

Emery,

Binzel,

Britt

et al. 2024

Space Sci Rev

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The Jupiter Trojan asteroids are a key population for understanding the chemical and dynamical evolution of the Solar System. Surface compositions of Trojans, in turn, provide crucial information for reconstructing their histories. NASA’s Lucy mission will soon complete the first spacecraft reconnaissance of this population. This review summarizes the current state of knowledge of Trojan surface compositions and looks ahead to expected advances in that knowledge from Lucy. Surface compositions of Trojans remain uncertain due to a relative lack of diagnostic absorption features, though dedicated observations have begun to provide some clues to compositions. Trojans have uniformly low albedos, with a population average of ∼5.3%, and red spectral slopes at ultraviolet, visible, and near-infrared wavelengths. A bimodality of spectral slopes has been detected and confirmed across all these wavelengths, and the ratio of “less-red” to “red” Trojans increases with decreasing size. A broad absorption at ∼3.1 μm in some less-red Trojans may indicate the presence of N-H bearing material. Mid-infrared emissivity spectra reveal the presence of fine-grained anhydrous silicates on the surfaces. The meteorite collection contains no identifiable analogs to Trojan asteroids. Among small body populations, some Main Belt asteroids, comets, irregular satellites, and Centaurs provide reasonable spectral matches, supporting some genetic relationships among some members of these groups. The cause of the observed spectral properties remains uncertain, but recent suggestions include a combination of volatile ice sublimation and space weathering or a combination of impact gardening and space weathering. The Lucy mission will provide detailed compositional analysis of (3548) Eurybates, (15094) Polymele, (11351) Leucus, (21900) Orus, and (617) Patroclus-Menoetius, a suite of targets that sample the diversity among the Trojan population along several dimensions. With these flybys, the Lucy mission is poised to resolve many of the outstanding questions regarding Trojan surface compositions, thereby revealing how the Trojans formed and evolved and providing a clearer view of Solar System history.

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Spectroscopic observations of Jupiter Trojans

Cited by 34 publications

References 13 publications

Visible spectroscopic and photometric survey of Jupiter Trojans: Final results on dynamical families☆

Visible spectroscopic and photometric survey of Jupiter Trojans: Final results on dynamical families☆

Exploring the Bimodal Solar System via Sample Return from the Main Asteroid Belt: The Case for Revisiting Ceres

Surface Compositions of Trojan Asteroids

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