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Appendix A: Radial velocity results

RV results for all CES Long Camera survey stars are displayed for comparison in the same time frame (JD 2 448 800 to JD 2 451 000), and with the y-axis adjusted according to the individual velocity dispersion.

$\begin{figure} {\psfig{figure=MS2400f25_1.eps,width=8.2cm,angle=270} }\vspace*{2... ...ace*{2mm} {\psfig{figure=MS2400f25_4.eps,width=8.2cm,angle=270} } \end{figure}$

Figure A.1: Radial velocity results for $\zeta$ Tuc, $\beta$ Hyi, HR 209 and $\nu$ Phe.

$\begin{figure} { \psfig{figure=MS2400f26_1.eps,width=8.2cm,angle=270} }\vspace*{... ...ace*{2mm} {\psfig{figure=MS2400f26_4.eps,width=8.2cm,angle=270} } \end{figure}$

Figure A.2: Radial velocity results for HR 448, HR 506, $\tau$ Cet and $\kappa$ For.

$\begin{figure} { \psfig{figure=MS2400f27_1.eps,width=8.2cm,angle=270} }\vspace*{... ...ce*{2mm} { \psfig{figure=MS2400f27_4.eps,width=8.2cm,angle=270} } \end{figure}$

Figure A.3: Radial velocity results for HR 753, $\iota$ Hor, $\alpha$ For and $\zeta ^{1}$ Ret.

$\begin{figure} { \psfig{figure=MS2400f28_1.eps,width=8.2cm,angle=270} }\vspace*{... ...e*{2mm} { \psfig{figure=MS2400f28_4.eps,width=8.2cm,angle=270} } \end{figure}$

Figure A.4: Radial velocity results for $\zeta ^{2}$ Ret, $\epsilon$ Eri, $\delta$ Eri and $\alpha$ Men.

$\begin{figure} { \psfig{figure=MS2400f29_1.eps,width=8.1cm,angle=270} }\vspace*{... ...e*{2mm} { \psfig{figure=MS2400f29_4.eps,width=8.1cm,angle=270} } \end{figure}$

Figure A.5: Radial velocity results for HR 2400, HR 2667, HR 3259 and HR 3677.

$\begin{figure} { \psfig{figure=MS2400f30_1.eps,width=8.1cm,angle=270} } \vspace*... ...ce*{2mm} { \psfig{figure=MS2400f30_4.eps,width=8.1cm,angle=270} } \end{figure}$

Figure A.6: Radial velocity results for HR 4523, HR 4979, $\alpha$ Cen A and $\alpha$ Cen B.

$\begin{figure} {\psfig{figure=MS2400f31_1.eps,width=8cm,angle=270} }\vspace*{2mm... ...space*{2mm} {\psfig{figure=MS2400f31_4.eps,width=8cm,angle=270} } \end{figure}$

Figure A.7: Radial velocity results for HR 5568, HR 6416, HR 6998 and HR 7373.

$\begin{figure} { \psfig{figure=MS2400f32_1.eps,width=8cm,angle=270} }\vspace*{2m... ...pace*{2mm} { \psfig{figure=MS2400f32_4.eps,width=8cm,angle=270} } \end{figure}$

Figure A.8: Radial velocity results for HR 7703, $\phi ^{2}$ Pav, HR 8323 and $\epsilon$ Ind.

$\begin{figure} { \psfig{figure=MS2400f33_1.eps,width=8cm,angle=270} }\vspace*{2m... ...pace*{2mm} { \psfig{figure=MS2400f33_4.eps,width=8cm,angle=270} } \end{figure}$

Figure A.9: Radial velocity results for HR 8501, HR 8883, Barnard's star and GJ 433.

$\begin{figure} {\psfig{figure=MS2400f34.eps,width=8.2cm,angle=270} } \end{figure}$

Figure A.10: Radial velocity results for Proxima Centauri.

Appendix B: Limits for planetary companions

The upper mass-limits for planets we can place according to the method described in Sect. 5 are shown here for the 28 examined CES survey stars (the limits for planets orbiting either $\alpha$ Cen A or B were presented in Endl et al. (2001a). Figures .11 to .17 display the $m\sin i$ values (in units of Jupiter masses) of detectable planetary signals as circles plotted vs. separation in AU. We can exclude all planets in circular orbits with masses above these limits. As described in Sect. 5 some stars have windows of non-detectability which are plotted as vertical lines. The $m\sin i = 1~{M}_{\rm Jup}$ border is shown for a better comparison as horizontal dotted line in each figure.

In the case of $\epsilon$ Eri the location of the long-period planetary companion from Hatzes et al. (2000) is also indicated (Fig. .13) by an asterisk. For Barnard's star (Fig. .17) we include the HST astrometric limits from Benedict et al. (1999).

$\begin{figure} {\psfig{figure=MS2400f35_1.eps,width=7.5cm,angle=270} }\vspace*{2... ...ce*{2mm} { \psfig{figure=MS2400f35_4.eps,width=7.5cm,angle=270} } \end{figure}$

Figure B.1: Planetary companion limits for $\zeta$ Tuc, $\beta$ Hyi, HR 209 and $\nu$ Phe.

$\begin{figure} { \psfig{figure=MS2400f36_1.eps,width=7.5cm,angle=270} }\vspace*{... ...ce*{2mm} { \psfig{figure=MS2400f36_4.eps,width=7.5cm,angle=270} } \end{figure}$

Figure B.2: Planetary companion limits for HR 448, HR 506, $\tau$ Cet and $\kappa$ For.

$\begin{figure} { \psfig{figure=MS2400f37_1.eps,width=7.5cm,angle=270} }\vspace*{... ...ce*{2mm} { \psfig{figure=MS2400f37_4.eps,width=7.5cm,angle=270} } \end{figure}$

Figure B.3: Planetary companion limits for $\alpha$ For, $\zeta ^{2}$ Ret, $\epsilon$ Eri and $\delta$ Eri.

$\begin{figure} { \psfig{figure=MS2400f38_1.eps,width=7.5cm,angle=270} }\vspace*{... ...ce*{2mm} { \psfig{figure=MS2400f38_4.eps,width=7.5cm,angle=270} } \end{figure}$

Figure B.4: Planetary companion limits for $\alpha$ Men, HR 2400, HR 2667 and HR 3259.

$\begin{figure} { \psfig{figure=MS2400f39_1.eps,width=7.5cm,angle=270} } \vspace*... ...ce*{2mm} { \psfig{figure=MS2400f39_4.eps,width=7.5cm,angle=270} } \end{figure}$

Figure B.5: Planetary companion limits for HR 3677, HR 4523, HR 4979 and HR 5568.

$\begin{figure} { \psfig{figure=MS2400f40_1.eps,width=7.5cm,angle=270} }\vspace*{... ...ce*{2mm} { \psfig{figure=MS2400f40_4.eps,width=7.5cm,angle=270} } \end{figure}$

Figure B.6: Planetary companion limits for HR 6416, HR 6998, HR 7703 and $\phi ^{2}$ Pav.

$\begin{figure} { \psfig{figure=MS2400f41_1.eps,width=7.5cm,angle=270} }\vspace*{... ...ce*{2mm} { \psfig{figure=MS2400f41_4.eps,width=7.5cm,angle=270} } \end{figure}$

Figure B.7: Planetary companion limits for $\epsilon$ Ind, HR 8501, HR 8883, and Barnard's star.

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