![\begin{figure}
\par\includegraphics[width=8.8cm,clip]{Gh251_f1.eps}\end{figure}](/articles/aa/full/2004/40/aagh251/img15.gif) |
Figure 1:
HARPS radial-velocity measurements of  Ara as a function
of time. The filled line represents the best fit to the data, obtained
with the sum of a Keplerian function and a linear trend, representing the effect
of the long period companions to the system. The residuals of the fit, with
an rms of only 0.9 m s-1, are shown in the lower panel. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=8.5cm,clip]{Gh251_f2.eps}\end{figure}](/articles/aa/full/2004/40/aagh251/img16.gif) |
Figure 2:
Phase-folded radial-velocity measurements of Ara after subtraction of
the linear trend shown in the upper panel of Fig. 1. In both panels the
error bars represent the rms around the weighted average of the individual measurements
for a given night. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=8.25cm,clip]{Gh251_f3.eps}\end{figure}](/articles/aa/full/2004/40/aagh251/img18.gif) |
Figure 3:
Radial velocity measurements of Ara
obtained during the past 6 years with the CORALIE (dots) and HARPS spectrographs
(open triangles), and by Jones et al. (2002) (open circles). The curve represents
the best 2-body Keplerian fit to the data.
In the lower panel we present the rms around the fit. For the longer period
Keplerian fit, the eccentricity was fixed to a value of 0.2. |
| Open with DEXTER | |
In the text