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This article is an erratum for:

Volume 625, May 2019
Article Number C2
Number of page(s) 3
Section Planets and planetary systems
Published online 17 May 2019

Due to a bad correction of telluric lines some Na I absorptions detected towards some stars were not mentioned in the original paper. This corrigendum presents a proper telluric subtraction, carried out with MOLECFIT11 (Smette et al. 2015, Kausch et al. 2015).

Tables 3 and 4 from the original paper are rectified below with the corrected Na I absorptions shown in boldface text.

Figure 4 of the original paper showed an incorrect plot of the Na I D line features observed towards HD 138813. Figure 1 is the corrected version of the original paper’s Fig. 4.

Below we summarize the corrected Na I absorptions of each concerned star:

  • HD 9672: the Na I D absorption at 11.5 km s−1 coincides with the Ca II feature and the radial velocity of the ISM.

  • HD 131488: besides the already reported non-photospheric absorptions at ~5.3 km s−1, a Na I D2 feature at –13.9 km s−1 is detected. A similar feature is detected towards field stars and most likely has an interstellar medium origin.

  • HD 138813: two new non-photospheric features are detected in the Na I D lines (see Fig. 1). The approximately −22.2 km s−1 absorption is close to the Ca II K non-photospheric absorption and the G ISM cloud; thus, an interstellar origin is more plausible. A feature in emission at 0.1 km s−1 is detected in both Na I D lines at the radial velocity of the star; this feature is related to the star.

  • HD 156623: an emission Na I D feature is present at the radial velocity of the star. Figure 2 shows the emission feature in both Na I D lines.

  • HD 172555: two narrow non-photospheric absorptions are detected. One of them, at approximately −20.4 km s−1 is close to the G cloud, and therefore possibly of ISM origin. This feature was also reported by Kiefer et al. (2014). A weaker broad, variable feature might have been detected at ~15.3 km s−1. It does not coincide with the Ca II absorption, the radial velocity of the star or the G cloud velocity vector. If confirmed, it would have a circumstellar origin.

  • HD 181296: the absorption detected in Na I D2 coincides with the one observed in Ca II.

The only remarkable change in the results with respect to the original paper is the Na I emission towards HD 138813 and HD 156623.However, the analysis of those emissions are beyond the scope of the original paper, and we emphasize that the main conclusions are not affected.


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© ESO 2019

All Tables

Table 3

Radial velocities and equivalent widths (EWs) of the Ca II H&K and Na I D non-photospheric absorptions, radial velocities of the stars, and projected velocities of ISM clouds in the Colorado model.

Table 4

Summary of the non-photospheric absorption features of the observed cold gas-bearing debris disc stars.

All Figures

thumbnail Fig. 1

Figure corrected for HD 138813 Na I D2 (black solid line) and D1 (black dotted line) lines. The radial velocities of the star (red dashed line) and of the ISM (grey dashed line) are also shown. Three Na I features are present, including an emission line at the radial velocity of the star.

In the text
thumbnail Fig. 2

Figure for HD 156623 showing the emission feature at the radial velocity of the star in both Na I D lines. The D2 component is shown in solid line while D1 is plotted in dotted line. The radial velocities of the star (red dashed line) and of the ISM (grey dashed line) are also shown.

In the text

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