Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[clip,width=8cm]{9177f01.eps}\end{figure}$ Figure 1: Distribution of 40 863 observations selected from the SDSS-MOC3 (gray dots) in the space of first and second principal components. The black dots correspond to 371 observations of known Jupiter Trojans, but those surrounded by a circle have been discarded (see text).
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In the text

$\begin{figure} \par\includegraphics[clip,width=8cm]{9177f02.eps}\end{figure}$ Figure 2: Distribution of the parameter $\epsilon$ (see text) for the Sloan sample (gray histogram) and for the Spectroscopic sample (hatched histogram). Each histogram has been normalized such that its area is 1.
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In the text

$\begin{figure} \par\mbox{\includegraphics[clip,width=7cm]{9177f03a.eps} ~~~~ \includegraphics[clip,width=07cm]{9177f03b.eps} } \end{figure}$ Figure 3: a) Distribution of spectral slopes from the Sloan sample (349 observations, gray histogram) and from the Spectroscopic sample (138 observations, hatched histogram). Each histogram has been normalized such that its area is 1. The distribution of Sloan slopes shows a clear bimodality related to the presence of two taxonomic types: P-type (smaller slopes) and D-type (larger slopes). This bimodality is less evident, but still appreciable, in the distribution of Spectroscopic slopes. The peak of Spectroscopic slopes around 0 is mostly caused by the observations of the Eurybates family by Fornasier et al. (2007). b) Comparison between the Spectroscopic slopes and the Sloan slopes from observations of asteroids included in both samples.
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In the text

$\begin{figure} \par\mbox{\includegraphics[clip,width=07cm]{9177f04a.eps} ~~~~ \includegraphics[clip,width=07cm]{9177f04b.eps} } \end{figure}$ Figure 4: Left panel: asteroid families (big dots) identified in the L4 swarm, projected in the space of proper eccentricity and inclination. Background asteroids are represented by small dots. The cutoff level is 110 ${\rm m~ s^{-1}}$ . Right panel: the same, but for the L5 swarm. The cutoff level is 120 ${\rm m~ s^{-1}}$ .
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In the text

$\begin{figure} \par\mbox{\includegraphics[clip,width=07cm]{9177f05a.eps} ~~~~ \includegraphics[clip,width=07cm]{9177f05b.eps} } \end{figure}$ Figure 5: a) Distribution of spectral slopes of observations corresponding to family members. The gray histogram correspond to the Sloan slopes and the hatched histogram to the Spectroscopic slopes. b) Same as a), but for the observations corresponding to background asteroids. Each histogram has been normalized such that its area is 1.
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In the text

$\begin{figure} \par\mbox{\includegraphics[clip,width=6cm]{9177f06a.eps} ~~ \incl... ...]{9177f06b.eps} ~~ \includegraphics[clip,width=6cm]{9177f06c.eps} } \end{figure}$ Figure 6: a) Distribution of the Sloan slopes of family members only. The gray histogram corresponds to the L4 swarm and the outlined histogram to the L5 swarm. b) Same as a), but for the background asteroids only. c) Same as a), but for both family members and background asteroids together. Each histogram has been normalized such that its area is 1.
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In the text

$\begin{figure} \par\mbox{\includegraphics[clip,width=7cm]{9177f07a.eps} ~~~~ \includegraphics[clip,width=7cm]{9177f07b.eps} } \end{figure}$ Figure 7: a) Distribution of the Sloan slopes of family members as a function of proper inclination. Dots correspond to the L4 swarm and crosses to the L5 swarm. b) Same as a), but for the background asteroids. Note the significant lack of high-inclination background asteroids with small slopes (P-types).
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In the text

$\begin{figure} \par\mbox{\includegraphics[clip,width=7cm]{9177f08a.eps} ~~~~ \includegraphics[clip,width=7cm]{9177f08b.eps} } \end{figure}$ Figure 8: a) Distribution of Sloan slopes of family members as a function of absolute magnitude. Dots correspond to the L4 swarm and cross to the L5 swarm. b) Same as a), but for the background asteroids. Note the significant lack of large background asteroids with small slopes (P-types).
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In the text

$\begin{figure} \par\mbox{\includegraphics[clip,width=7cm]{9177f09a.eps} ~~~~ \includegraphics[clip,width=7cm]{9177f09b.eps} } \end{figure}$ Figure 9: Distribution of the Spectroscopic slopes of background asteroids as a function of proper inclination a) and absolute magnitude b). Dots correspond to the L4 swarm and cross to the L5 swarm.
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In the text

$\begin{figure} \par\includegraphics[clip,width=8.5cm]{9177f10.eps}\end{figure}$ Figure 10: Distribution of proper inclinations in terms of absolute magnitude for 913 known background Trojans. Dots correspond to the L4 swarm and cross to the L5 swarm. Note the relative lack of large asteroids with small inclinations.
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In the text

$\begin{figure} \par\mbox{\includegraphics[clip,width=7cm]{9177f11a.eps} ~~~~ \includegraphics[clip,width=7cm]{9177f11b.eps} } \end{figure}$ Figure 11: Left panel: dendogram of the Menelaus clan, indicating the main families identified. The dashed horizontal line is the cutoff used in this study. Right panel: distribution in the space of proper elements of the Menelaus family (gray circles) as detected at $d_{{\rm cut}}=110$ ${\rm m~ s^{-1}}$ , and of the Eurybates family (black circles) as detected at $d_{{\rm cut}}=70$ ${\rm m~ s^{-1}}$ . The size of each circle is proportional to the asteroid size.
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In the text

$\begin{figure} \mbox{\includegraphics[clip,width=5.5cm]{9177f12a.eps} ~~ \includ... ... } \par\medskip \par\includegraphics[clip,width=5.5cm]{9177f12g.eps}\end{figure}$ Figure 12: Distribution of spectral slopes against absolute magnitude for seven families of the Menelaus clan. Full circles correspond to Sloan slopes. Triangles correspond to Spectroscopic slopes. The vertical dotted lines define the slope transition, within $\pm$ $0.8\times10^{-5}~{\rm \AA}^{-1}$ , between the different taxonomic classes indicated above the plots.
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In the text

$\begin{figure} \mbox{\includegraphics[clip,width=5.5cm]{9177f13a.eps} ~~ \includ... ...9177f13c.eps} ~~ \includegraphics[clip,width=5.5cm]{9177f13d.eps} } \end{figure}$ Figure 13: Same as Fig. 12, but for four families in the L4 swarm.
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In the text

$\begin{figure} \par\mbox{\includegraphics[clip,width=5.5cm]{9177f14a.eps} ~~ \in... ...9177f14b.eps} ~~ \includegraphics[clip,width=5.5cm]{9177f14c.eps} } \end{figure}$ Figure 14: Same as Fig. 12, but for three high-inclination families in the L4 swarm.
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In the text

$\begin{figure} \par\includegraphics[clip,width=8.5cm]{9177f15.eps}\end{figure}$ Figure 15: Distribution in the space of proper elements of the Anchises clan as detected at $d_{{\rm cut}}=130$ ${\rm m~ s^{-1}}$ . It is constituted by five families: Panthoos, Polydoros, Sergestus, Agelaos and 1999 RV165. (1173) Anchises is incorporated into the Agelaos family at $d_{{\rm cut}}>135$ ${\rm m~ s^{-1}}$ . The size of each circle is proportional to the asteroid size.
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In the text

$\begin{figure} \par\mbox{\includegraphics[clip,width=5.5cm]{9177f16a.eps} ~~ \in... ...9177f16b.eps} ~~ \includegraphics[clip,width=5.5cm]{9177f16c.eps} } \end{figure}$ Figure 16: Distribution of spectral slopes against absolute magnitude for three families of the Anchises clan: a) Panthoos, b) Polydoros + Sergestus, and c) Agelaos + Anchises. Full circles correspond to Sloan slopes. Triangles correspond to Spectroscopic slopes. The vertical dotted lines define the slope transition, within $\pm$ $0.8\times10^{-5}~{\rm \AA}^{-1}$ , between the different taxonomic classes indicated above the plots.
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In the text

$\begin{figure} \mbox{\includegraphics[clip,width=5.5cm]{9177f17a.eps} ~~ \includ... ...9177f17d.eps} ~~ \includegraphics[clip,width=5.5cm]{9177f17e.eps} } \end{figure}$ Figure 17: Same as Fig. 16, but for five different families in the L5 swarm.
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In the text

$\begin{figure} \par\includegraphics[clip,width=8cm]{9177f01.eps}\end{figure}$	Figure 1: Distribution of 40 863 observations selected from the SDSS-MOC3 (gray dots) in the space of first and second principal components. The black dots correspond to 371 observations of known Jupiter Trojans, but those surrounded by a circle have been discarded (see text).
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$\begin{figure} \par\includegraphics[clip,width=8cm]{9177f02.eps}\end{figure}$	Figure 2: Distribution of the parameter $\epsilon$ (see text) for the Sloan sample (gray histogram) and for the Spectroscopic sample (hatched histogram). Each histogram has been normalized such that its area is 1.
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$\begin{figure} \par\mbox{\includegraphics[clip,width=07cm]{9177f04a.eps} ~~~~ \includegraphics[clip,width=07cm]{9177f04b.eps} } \end{figure}$	Figure 4: Left panel: asteroid families (big dots) identified in the L4 swarm, projected in the space of proper eccentricity and inclination. Background asteroids are represented by small dots. The cutoff level is 110 ${\rm m~ s^{-1}}$ . Right panel: the same, but for the L5 swarm. The cutoff level is 120 ${\rm m~ s^{-1}}$ .
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$\begin{figure} \par\mbox{\includegraphics[clip,width=07cm]{9177f05a.eps} ~~~~ \includegraphics[clip,width=07cm]{9177f05b.eps} } \end{figure}$	Figure 5: a) Distribution of spectral slopes of observations corresponding to family members. The gray histogram correspond to the Sloan slopes and the hatched histogram to the Spectroscopic slopes. b) Same as a), but for the observations corresponding to background asteroids. Each histogram has been normalized such that its area is 1.
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$\begin{figure} \par\mbox{\includegraphics[clip,width=6cm]{9177f06a.eps} ~~ \incl... ...]{9177f06b.eps} ~~ \includegraphics[clip,width=6cm]{9177f06c.eps} } \end{figure}$	Figure 6: a) Distribution of the Sloan slopes of family members only. The gray histogram corresponds to the L4 swarm and the outlined histogram to the L5 swarm. b) Same as a), but for the background asteroids only. c) Same as a), but for both family members and background asteroids together. Each histogram has been normalized such that its area is 1.
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$\begin{figure} \par\mbox{\includegraphics[clip,width=7cm]{9177f07a.eps} ~~~~ \includegraphics[clip,width=7cm]{9177f07b.eps} } \end{figure}$	Figure 7: a) Distribution of the Sloan slopes of family members as a function of proper inclination. Dots correspond to the L4 swarm and crosses to the L5 swarm. b) Same as a), but for the background asteroids. Note the significant lack of high-inclination background asteroids with small slopes (P-types).
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$\begin{figure} \par\mbox{\includegraphics[clip,width=7cm]{9177f08a.eps} ~~~~ \includegraphics[clip,width=7cm]{9177f08b.eps} } \end{figure}$	Figure 8: a) Distribution of Sloan slopes of family members as a function of absolute magnitude. Dots correspond to the L4 swarm and cross to the L5 swarm. b) Same as a), but for the background asteroids. Note the significant lack of large background asteroids with small slopes (P-types).
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$\begin{figure} \par\mbox{\includegraphics[clip,width=7cm]{9177f09a.eps} ~~~~ \includegraphics[clip,width=7cm]{9177f09b.eps} } \end{figure}$	Figure 9: Distribution of the Spectroscopic slopes of background asteroids as a function of proper inclination a) and absolute magnitude b). Dots correspond to the L4 swarm and cross to the L5 swarm.
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$\begin{figure} \par\includegraphics[clip,width=8.5cm]{9177f10.eps}\end{figure}$	Figure 10: Distribution of proper inclinations in terms of absolute magnitude for 913 known background Trojans. Dots correspond to the L4 swarm and cross to the L5 swarm. Note the relative lack of large asteroids with small inclinations.
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$\begin{figure} \mbox{\includegraphics[clip,width=5.5cm]{9177f12a.eps} ~~ \includ... ... } \par\medskip \par\includegraphics[clip,width=5.5cm]{9177f12g.eps}\end{figure}$	Figure 12: Distribution of spectral slopes against absolute magnitude for seven families of the Menelaus clan. Full circles correspond to Sloan slopes. Triangles correspond to Spectroscopic slopes. The vertical dotted lines define the slope transition, within $\pm$ $0.8\times10^{-5}~{\rm \AA}^{-1}$ , between the different taxonomic classes indicated above the plots.
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$\begin{figure} \mbox{\includegraphics[clip,width=5.5cm]{9177f13a.eps} ~~ \includ... ...9177f13c.eps} ~~ \includegraphics[clip,width=5.5cm]{9177f13d.eps} } \end{figure}$	Figure 13: Same as Fig. 12, but for four families in the L4 swarm.
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$\begin{figure} \par\mbox{\includegraphics[clip,width=5.5cm]{9177f14a.eps} ~~ \in... ...9177f14b.eps} ~~ \includegraphics[clip,width=5.5cm]{9177f14c.eps} } \end{figure}$	Figure 14: Same as Fig. 12, but for three high-inclination families in the L4 swarm.
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$\begin{figure} \par\includegraphics[clip,width=8.5cm]{9177f15.eps}\end{figure}$	Figure 15: Distribution in the space of proper elements of the Anchises clan as detected at $d_{{\rm cut}}=130$ ${\rm m~ s^{-1}}$ . It is constituted by five families: Panthoos, Polydoros, Sergestus, Agelaos and 1999 RV165. (1173) Anchises is incorporated into the Agelaos family at $d_{{\rm cut}}>135$ ${\rm m~ s^{-1}}$ . The size of each circle is proportional to the asteroid size.
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$\begin{figure} \mbox{\includegraphics[clip,width=5.5cm]{9177f17a.eps} ~~ \includ... ...9177f17d.eps} ~~ \includegraphics[clip,width=5.5cm]{9177f17e.eps} } \end{figure}$	Figure 17: Same as Fig. 16, but for five different families in the L5 swarm.
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