    Spectra for $\delta$ Eri were obtained using the SARG spectrograph \citep{1997SPIE.2871.1204G} mounted on the Italian TNG at La Palma, Spain, in a service-mode observing run in 2008 (PI Heiter). Given the brightness of the target (and additional abudance tests planned), the highest resolving power achievable ($R\,=\,164\,000$) was chosen. Using two different grisms, spectra with the nominal wavelength coverage of $3600-5140$\,\AA\ and red $4960-10110$\,\AA, respectively, were obtained. The exposure times were adjusted to reach a signal-to-noise ratio (S/N) of order 400, which resulted in 260 s exposure for the red and 650 s for the blue grism mode.
    
Data reduction was performed using REDUCE \citep{2002A&A...385.1095P}. REDUCE uses a cluster-analysis method for order tracing, employing the flat-field spectrum as it has no absorption lines and high signal. REDUCE determines cluster groups according to a signal-level criterion and fits them with third-order polynomials. In contrast to many other data-reduction packages, no assumption is made about the cross-dispersion profile: it is recovered from the observations. To check the true quality of our data, we estimated the signal-to-noise (S/N) ratio in the centre of each order for the spectral regions of interest. The resulting S/N values are somewhat lower than expected. For the optical region of interest (5550 - 6750 \AA), the S/N is found to be in the range of $200-400$, but in the IR it only reaches 70-90. On top of that, the resolving power is not as high as claimed and degrades towards the red, as measured on arc-lamp calibration frames. In order 110 ($\lambda_c = 5550$\,\AA) we found $R\,=\,120\,000-130\,000$ decreasing to $R\,=\,85\,000-90\,000$ in order 66 ($\lambda_c = 9280$\,\AA). Consulting the TNG staff, we learned that the spectrograph was slightly defocused during the time of observation. Fringing further limits the S/N of the near-IR data. We nonetheless deem the data quality to be sufficient for our scientific goals.

%{\bf Add results from 2009 data}

Various attempts were made to deal with the near-IR fringing in a satisfactory way. The use of a telluric standard star of early spectral type observed during the same night proved difficult, as its spectrum contain strong Paschen lines in the Gaia-RVS spectral region. In the end, the best results were obtained by standard flat-field division. On Fig. 1 you can see a small fragments of $\delta$ Eri spectra in the optical and IR regions.

   \begin{figure}[t]
   \centering
   \includegraphics[angle=90,width=\columnwidth]{Fig1.ps}
   \caption{The upper panel shows a fragment of $\delta$ Eri spectrum obtained in the optical region and the lower one shows a part of the RVS spectrum zoomed onto the two Ca II lines (8498 \AA\ and 8542.1 \AA\ respectively).}
   \end{figure}
   