All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{2820f01.ps} \end{figure}$ Figure 1: A typical spectrum, here for object #32. The abscissa is wavelength in angstroms, and the ordinate is flux in erg s^-1 cm^-2 Å^-1, after division by an appropriate factor of $1.8\times 10^{-13}$ . The spectrum is dominated by CN and C₂ features, and H $\alpha$ is in emission. The strong absorption band near 7600-7700 Å is telluric O₂. All other spectra are available in the electronic Appendix.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.6cm,clip]{2820f02.ps} \end{figure}$ Figure 2: The reduced proper motion H = J + 5 log $_{10}(\mu )$ plotted as a function of the R-J color index. Open circles are known dwarf carbon stars. Filled squares represent the 16 C stars of our sample for which USNO-B1 provides a non-zero proper motion (see text).
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7.7cm,clip]{2820f03a.ps} \includegraphics[angle=-90,width=7.7cm,clip]{2820f03b.ps} } \end{figure}$ Figure 3: Plots in galactocentric XYZ of the observed AGB C halo stars, with those found in this paper indicated by a cross. Left panel: the C stars trace the Sgr Stream seen nearly edge-on, with a very distant C star to the South, and several C stars off the plane in the North. Right panel: the Sun is at X = +8.5 kpc, Z=0 to the right of the origin, and the Sgr dwarf galaxy centre is indicated by a filled square at X = 14.7 kpc Z = -5.8 kpc to the left of the origin. In the right panel, the scarcity of objects near the horizontal axis is due to the difficulty of finding very distant C stars close to the Galactic plane (see text).
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7.7cm,clip]{2820f04a.ps} \includegraphics[angle=-90,width=7.7cm,clip]{2820f04b.ps} } \end{figure}$ Figure 4: Same plots in XYZ of the model of the Sgr Stream, from the N-body simulations of Law et al. (2004). This simulation corresponds to the case of a spheroidal Galactic potential.
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In the text

$\begin{figure}\par\includegraphics[angle=-90,width=16cm,clip]{2820ob31.ps} \incl... ...20ob33.ps} \includegraphics[angle=-90,width=16cm,clip]{2820ob34.ps} \end{figure}$ Figure A.1: Spectra of objects 31, 32, 33, & 34. In all these graphs, fluxes in ordinates are in erg s^-1 cm^-2 Å^-1. Fluxes were divided by factors $0.7\times 10^{-14}$ , $1.8\times 10^{-13}$ , $0.5 \times 10^{-13}$ , and $0.25 \times 10^{-13}$ for objects 31, 32, 33, and 34, respectively.

In the text

$\begin{figure}\par\includegraphics[angle=-90,width=16cm,clip]{2820ob35.ps} \incl... ...b37.ps} \includegraphics[angle=-90,width=16cm,clip]{2820ob38.ps}\par\end{figure}$ Figure A.2: Spectra of objects 35, 36, 37, and 38. In all these graphs, fluxes in ordinates are in erg s^-1 cm^-2 Å^-1. Fluxes were divided by factors $0.18\times 10^{-14}$ , $5.5\times 10^{-15}$ , $0.22\times 10^{-14}$ , and $0.25\times 10^{-14}$ for objects 35, 36, 37, and 38, respectively.

In the text

$\begin{figure}\par\includegraphics[angle=-90,width=16cm,clip]{2820ob39.ps} \incl... ...b41.ps} \includegraphics[angle=-90,width=16cm,clip]{2820ob42.ps}\par\end{figure}$ Figure A.3: Spectra of objects 39, 40, 41, and 42. In all these graphs, fluxes in ordinates are in erg s^-1 cm^-2 Å^-1. Fluxes were divided by factors $0.95\times 10^{-14}$ , $3.5 \times 10^{-15}$ , $0.9\times 10^{-14}$ , & $0.4 \times 10^{-14}$ for objects 39, 40, 41, and 42, respectively.

In the text

$\begin{figure}\par\includegraphics[angle=-90,width=16cm,clip]{2820ob43.ps} \incl... ...b45.ps} \includegraphics[angle=-90,width=16cm,clip]{2820ob46.ps}\par\end{figure}$ Figure A.4: Spectra of objects 43, 44, 45, and 46. In all these graphs, fluxes in ordinates are in erg s^-1 cm^-2 Å^-1. Fluxes were divided by factors $0.22\times 10^{-14}$ , $0.017\times 10^{-14}$ , $4.5\times 10^{-15}$ , and $3.5\times 10^{-14}$ for objects 43, 44, 45, and 46, respectively.

In the text

$\begin{figure}\par\includegraphics[angle=-90,width=16cm,clip]{2820ob47.ps} \incl... ...20ob49.ps} \includegraphics[angle=-90,width=16cm,clip]{2820ob50.ps} \end{figure}$ Figure A.5: Spectra of objects 47, 48, 49, and 50. In all these graphs, fluxes in ordinates are in erg s^-1 cm^-2 Å^-1. Fluxes were divided by factors $0.15\times 10^{-14}$ , $2.6\times 10^{-15}$ , $3.3 \times 10^{-14}$ , and $0.75\times 10^{-14}$ for objects 47, 48, 49, and 50, respectively.

In the text

$\begin{figure}\par\includegraphics[angle=-90,width=16cm,clip]{2820ob51.ps} \incl... ...b53.ps} \includegraphics[angle=-90,width=16cm,clip]{2820ob54.ps}\par\end{figure}$ Figure A.6: Spectra of objects 51, 52, 53, and 54. In all these graphs, fluxes in ordinates are in erg s^-1 cm^-2 Å^-1. Fluxes were divided by factors $0.6 \times 10^{-14}$ , $2.7 \times 10^{-14}$ , $5.5 \times 10^{-14}$ , and $0.72 \times 10^{-15}$ for objects 51, 52, 53, and 54, respectively.

In the text

$\begin{figure}\par\includegraphics[angle=-90,width=16cm,clip]{2820ob55.ps} \end{figure}$ Figure A.7: Spectrum of object 55. The flux in ordinates is in erg s^-1 cm^-2 Å^-1, after dividing by a factor of $2.2\times 10^{-14}$ .

In the text

$\begin{figure}\par\includegraphics[angle=-90,width=16cm,clip]{2820ob56.ps} \incl... ...20ob57.ps} \includegraphics[angle=-90,width=16cm,clip]{2820ob58.ps} \end{figure}$ Figure A.8: Spectra of objects 56, 57, and 58. In all these graphs, fluxes in ordinates are in erg s^-1 cm^-2 Å^-1. Fluxes were divided by factors $0.21\times 10^{-14}$ , $0.52\times 10^{-14}$ , and $3.7\times 10^{-15}$ for objects 56, 57, and 58, respectively.

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.6cm,clip]{2820f02.ps} \end{figure}$	Figure 2: The reduced proper motion H = J + 5 log $_{10}(\mu )$ plotted as a function of the R-J color index. Open circles are known dwarf carbon stars. Filled squares represent the 16 C stars of our sample for which USNO-B1 provides a non-zero proper motion (see text).
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$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=7.7cm,clip]{2820f04a.ps} \includegraphics[angle=-90,width=7.7cm,clip]{2820f04b.ps} } \end{figure}$	Figure 4: Same plots in XYZ of the model of the Sgr Stream, from the N-body simulations of Law et al. (2004). This simulation corresponds to the case of a spheroidal Galactic potential.
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