The co-existence of hot and cold gas in debris discs (Corrigendum)

I. Rebollido; C. Eiroa; B. Montesinos; J. Maldonado; E. Villaver; O. Absil; A. Bayo; H. Canovas; A. Carmona; Ch. Chen; S. Ertel; A. Garufi; Th. Henning; D. P. Iglesias; R. Launhardt; R. Liseau; G. Meeus; A. Moór; A. Mora; J. Olofsson; G. Rauw; P. Riviere-Marichalar

doi:10.1051/0004-6361/201732329e

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Volume 625 (May 2019)

A&A, 625 (2019) C2

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Erratum

This article is an erratum for: [this article]

Issue		A&A Volume 625, May 2019


Article Number		C2
Number of page(s)		3
Section		Planets and planetary systems
DOI		https://doi.org/10.1051/0004-6361/201732329e
Published online		17 May 2019

A&A 625, C2 (2019)

The co-existence of hot and cold gas in debris discs (Corrigendum)

I. Rebollido¹, C. Eiroa¹, B. Montesinos², J. Maldonado³, E. Villaver¹, O. Absil⁴, A. Bayo⁵^,6, H. Canovas¹^,7, A. Carmona⁸, Ch. Chen⁹, S. Ertel¹⁰, A. Garufi¹, Th. Henning¹¹, D. P. Iglesias⁵^,6, R. Launhardt¹¹, R. Liseau¹², G. Meeus¹, A. Moór¹³, A. Mora¹⁴, J. Olofsson⁵^,6, G. Rauw⁴ and P. Riviere-Marichalar¹⁵

¹ Departamento Física Teórica, Universidad Autónoma de Madrid, Cantoblanco, 28049 Madrid, Spain
e-mail: isabel.rebollido@uam.es
² Centro de Astrobiología (CAB, CSIC-INTA), ESAC Campus, Camino Bajo del Castillo s/n, Villanueva de la Cañada, 28692 Madrid, Spain
³ INAF, Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
⁴ STAR Institute, Université de Liège, F.R.S.-FNRS, 19c Allée du Six Août, 4000 Liège, Belgium
⁵ Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Casilla, 5030 Valparaíso, Chile
⁶ Núcleo Milenio de Formación Planetaria-NPF, Universidad de Valparaíso, Av. Gran Bretaña, 1111 Valparaíso, Chile
⁷ European Space Astronomy Centre (ESA), PO Box 78, Villanueva de la Cañada, 28691 Madrid, Spain
⁸ Université de Toulouse, UPS-OMP, IRAP, 31400 Toulouse, France
⁹ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21212, USA
¹⁰ Steward Observatory, Department of Astronomy, University of Arizona, Tucson, AZ 85721, USA
¹¹ Max-Planck-Institut für Astronomie (MPIA), Königstuhl 17, 69117 Heidelberg, Germany
¹² Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden
¹³ Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, PO Box 67, 1525 Budapest, Hungary
¹⁴ Aurora Technology B.V. for ESA, ESA-ESAC, Villanueva de la Cañada, 28691 Madrid, Spain
¹⁵ Instituto de Ciencia de Materiales de Madrid (CSIC), Calle Sor Juana Inés de la Cruz 3, 28049 Cantoblanco, Madrid, Spain

Key words: stars: general / planetary systems / comets: general / ISM: clouds / circumstellar matter / errata, addenda

Erratum to: A&A, 614, A3 (2018), https://doi.org/10.1051/0004-6361/201732329

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.

References

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¹

https://www.eso.org/sci/software/pipelines/skytools/molecfit

© 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.

In the text

Table 4

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

In the text

All Figures

	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.
Open with DEXTER
In the text

	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.
Open with DEXTER
In the text

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