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\IBVShead{5648}{8 September 2005}

\IBVStitletl{Erratum:}{ ``A High-Resolution Spectrum of the T\lowercase{r}ES-1 Parent Star''}

\IBVSauth{Strassmeier, Klaus G.$^1$; Rice, John B.$^2$}

\IBVSinst{Astrophysical Institute Potsdam, Germany. e-mail: kstrassmeier@aip.de}
\IBVSinst{Brandon University, Dept. of Physics \& Astronomy,
Canada. e-mail: rice@brandonU.ca}


\SIMBADobjAlias{GSC 02652-01324}{NAME TrES-1 Parent Star} 
\IBVSabs{We present a high-resolution (R=120,000) spectrum  of the lithium}
\IBVSabs{region of the parent star of the newly-discovered transiting planet}
\IBVSabs{TrES-1 (GSC02652-01324, K0V, V=11.8mag). No lithium seems to be}
\IBVSabs{present at the surface of TrES-1.}


\begintext

In a previous IBVS note (Strassmeier \& Rice 2004; IBVS 5566; Oct.
2004) we presented a single high-resolution ($R$=120,000) spectrum
of the parent star of the TrES-1 planet in a 10nm wide wavelength
region centered at the lithium region at 671nm. Our intentions
were to determine the lithium abundance of the host star and to
obtain an accurate value of its rotational line broadening. As a
by product, we found an iron abundance of --0.6dex compared to the
most recent solar value. In the meantime, Sozzetti et al. (2004)
also published a high-resolution spectrum of TrES-1
($R\approx$60,000) but obtained a solar abundance of
[Fe/H]$\approx$0.00, in agreement with an earlier note in Alonso
et al. (2005) but in strong disagreement with our value.

Due to a data-reduction error during the combination of our five
individual TrES-1 spectra, our combined spectrum appeared with
spectral lines too shallow by 50\% and left its analysis faulty.
After a complete re-reduction of the individual and the combined
\hbox{TrES-1} spectra, this error did not appear again and its line
depths were produced correctly. We have then repeated the analysis
described in our previous note and confirm our earlier
non-detection of the lithium line at 670.8nm and the $v\sin i$
value of 2.8$\pm$0.2 (rms) km\,s$^{-1}$. The best fit to the Fe\,{\sc i}
670.356-nm line (Fig.~2 in the previous note) was now achieved
with an iron abundance of 7.46$\pm$0.04 though (on the $\log
n$(H)=12.00 scale), in very good agreement with the
[Fe/H]=0.00$\pm$0.09 value put forward by Sozzetti et al. (2004).
Fig.~1 shows a new plot of the lithium region that gives the
correct line depth of our TrES-1 spectrum. This figure replaces
the one in IBVS 5566. Fig.~2 in IBVS 5566 is obsolete.

\IBVSfig{9cm}{5648-f1.eps}{$R$=120,000 spectrum of the lithium
region of the TrES-1 parent star (top). The other spectra are
comparisons and arbitrarily shifted. Middle spectrum: the
K0V-standard star 70~Oph(A) obtained with the same equipment.
Lower spectrum: a $R$=600,000 spectrum of the Sun. }
\IBVSfigKey{5648-f1.eps}{GSC 02652-01324}{spectrum}

We apologize for any inconveniences and confusions this may have
caused.


\IBVSTnam{TrES-1, GSC02652-01324}

\IBVSTcoo{19\hr 04\mm 09\fsec8}{+36\deg 37\arcm 58\arcs}{2000}

\IBVSTobs{3.6m Canada-France-Hawaii telescope (CFHT), Gecko spectrograph}

\IBVSTdet{EEV2 CCD 2048$\times$4600, 13.5$\mu$m pixels, --113\deg C
cooled. }

\IBVSTdateobs{2004.08.31; UT}

\references

Alonso R., Brown T. M., Torres G. et al., 2004, {\it ApJ}, {\bf 613}, L153

Sozzetti A., Yong D., Torres G. et al., 2004, {\it ApJ}, {\bf 616}, L167

Strassmeier K. G., Rice J. B., 2004, {\it IBVS}, 5566

\endreferences


\end{document}
