Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany

Due to a computational error in the bolometric correction the $L_{\rm x}/L_{\rm bol}$ ratios given in Table 2 of the paper are wrong. The same applies to upper limits to $L_{\rm x}/L_{\rm bol}$ for X-ray undetected members of the Tucanae association (Table 3 in the original paper).

Generally, the values given in the paper are too large. As far as the detections are concerned, in all (but three cases) the error is within a factor of 2, i.e. within the uncertainties produced by the count rate error, the uncertainty in the count rate to luminosity conversion, and the X-ray variability. For two of the RASS detections, namely HIP1910 and HIP107345, the change in $L_{\rm bol}$ after the correction is significantly higher than that.

Table 1: Corrected values for $\log{(L_{\rm x}/L_{\rm bol})}$ of RASS detected candidate members of the Tucanae association.
Designation $\log{(L_{\rm x}/L_{\rm bol})}$

RASS detected probable Tuc Members

HIP1481 -4.14

HIP1910 -3.40

HIP2729 -3.20

HIP92680 -3.50

HIP93815 -4.10

HIP99803 -4.49

HIP105388 -3.35

HIP105404 -3.16

HIP107345 -3.33

HIP107947 -4.03

HIP108195 -4.91

PPM366328 -3.51

HIP116748 -3.37

RASS detected improbable Tuc Members

HIP103438 -4.81

**Table 1:** Corrected values for $\log{(L_{\rm x}/L_{\rm bol})}$ of RASS detected candidate members of the Tucanae association.
Designation	$\log{(L_{\rm x}/L_{\rm bol})}$
RASS detected probable Tuc Members
HIP1481	-4.14
HIP1910	-3.40
HIP2729	-3.20
HIP92680	-3.50
HIP93815	-4.10
HIP99803	-4.49
HIP105388	-3.35
HIP105404	-3.16
HIP107345	-3.33
HIP107947	-4.03
HIP108195	-4.91
PPM366328	-3.51
HIP116748	-3.37
RASS detected improbable Tuc Members
HIP103438	-4.81

Table 2: Corrected values for $\log{(L_{\rm x}/L_{\rm bol})}$ of candidate members of the Tucanae association which are not detected by the RASS.
Designation $\log{(L_{\rm x}/L_{\rm bol})}$

Non-detected probable Tuc Members

HIP1993 < -3.72

HIP2484 < -6.39

HIP2487 < -6.17

HIP2578 < -6.90

HIP95261 < -5.97

HIP95270 < -4.74

HIP100751 < -8.00

HIP104308 < -5.24

HIP118121 < -5.65

Non-detected improbable Tuc Members

HIP459 < -4.54

HIP1399 < -3.90

HIP93096 < -4.31

HIP94051 < -5.02

HIP94858 < -7.02

HIP94997 < -3.90

HIP95302 < -4.84

HIP97705 < -6.27

HIP101636 < -4.67

HIP101844 < -3.62

HIP104256 < -4.55

HIP107806 < -4.92

HIP109612 < -4.27

HIP114236 < -6.98

**Table 2:** Corrected values for $\log{(L_{\rm x}/L_{\rm bol})}$ of candidate members of the Tucanae association which are not detected by the RASS.
Designation	$\log{(L_{\rm x}/L_{\rm bol})}$
Non-detected probable Tuc Members
HIP1993	< -3.72
HIP2484	< -6.39
HIP2487	< -6.17
HIP2578	< -6.90
HIP95261	< -5.97
HIP95270	< -4.74
HIP100751	< -8.00
HIP104308	< -5.24
HIP118121	< -5.65
Non-detected improbable Tuc Members
HIP459	< -4.54
HIP1399	< -3.90
HIP93096	< -4.31
HIP94051	< -5.02
HIP94858	< -7.02
HIP94997	< -3.90
HIP95302	< -4.84
HIP97705	< -6.27
HIP101636	< -4.67
HIP101844	< -3.62
HIP104256	< -4.55
HIP107806	< -4.92
HIP109612	< -4.27
HIP114236	< -6.98

The new, correct values for all Tucanae stars (detected and undetected) are given in two tables below. As a consequence of these corrections the values plotted in Fig. 3

$\begin{figure} \par\includegraphics[width=8cm,clip]{Lrat_WLi.eps} \end{figure}$	Figure 1: Correlation between the X-ray to bolometric luminosity ratio and the equivalent width of lithium after correction of the $L_{\rm x}/L_{\rm bol}$ values.
Open with DEXTER

of the paper have changed. The figure below is the updated version of Fig. 3 from the paper. The correlation between the lithium equivalent width and $L_{\rm x}/L_{\rm bol}$ is preserved. But the saturation limit is now closer to the "canonical'' value for late-type stars of $\log{(L_{\rm x}/L_{\rm bol})} = -3$ .

We note that for HIP 118121, listed as a non-detected star in our Table 3 of the paper, there is a detection in the Faint Star Catalogue (FSC) at a distance of $\sim$ 15 $^{\prime\prime}$ . However, due to a nearby brighter source the count rate given for this source in the FSC (0.06cps) is not reliable, and the source appears to be extended. Our detection procedure has not detected this source because it has been designed to specialize on point sources.

X-ray emission from young stars in the Tucanae association