| Issue |
A&A
Volume 696, April 2025
|
|
|---|---|---|
| Article Number | C2 | |
| Number of page(s) | 3 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/202554249e | |
| Published online | 31 March 2025 | |
Charting circumstellar chemistry of carbon-rich asymptotic giant branch stars
I. ALMA 3 mm spectral surveys (Corrigendum)
1
Department of Space, Earth and Environment, Chalmers University of Technology,
412 96
Gothenburg, Sweden
2
Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory (OSO),
439 92
Onsala, Sweden
3
Joint ALMA Observatory (JAO),
Alonso de Córdova 3107, Vitacura 763-0355, Casilla 19001,
Santiago,
Chile
4
European Southern Observatory (ESO),
Alonso de Córdova 3107, Vitacura,
763-0355,
Santiago, Chile
5
NASA Goddard Space Flight Center,
8800 Greenbelt Road,
Greenbelt,
MD
20771, USA
6
Solar System Exploration Division, NASA Goddard Space Flight Center,
8800 Greenbelt Road,
Greenbelt,
MD
20771, USA
7
Department of Physics, Catholic University of America,
Washington,
DC
20064, USA
8
Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast,
University Road,
Belfast,
BT7 1NN,
UK
9
Gemini Observatory / NSF’s NOIRLab,
670 N. A’ohoku Place,
Hilo, Hawai’i,
96720,
USA
10
East Asian Observatory / James Clerk Maxwell Telescope,
660 N. A’ohoku Place,
Hilo,
HI
96720, USA
★ Corresponding author; ramlal.unnikrishnan@chalmers.se
Key words: stars: AGB and post-AGB / circumstellar matter / stars: mass-loss / stars: winds, outflows / submillimeter: stars / errata, addenda
It has come to our attention that an error occurred in the preparation of Table B.2. The listed rest frequencies were inadvertently shifted down by one row, starting from the entry for the CS (J = 5 − 4) transition. This occurred due to the accidental partial omission of a row listing the C33S (J = 5 − 4) line, with its frequency erroneously included in the row immediately below, alongside the CS (J = 5 − 4). This misalignment then propagated down through the rest of the table. We also had a typographical error in the same table, where the transition quantum numbers for the HC3N (J = 26 − 25) transition were mistakenly typed as J = 26 – 27. We include a corrected version of the table here. We note that this error was limited to the preparation of the table and does not, in any way, affect the analysis or results presented in the paper.
Appendix B Details of detected transitions
This appendix lists the detected emission lines along with their upper-level energies and integrated intensities for the three stars. Table B.2 includes the lines from the APEX surveys that were used in this work for abundance calculations.
Details of the lines from APEX observations used in the population diagrams.
© The Authors 2025
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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