Stellar structures, molecular gas, and star formation across the PHANGS sample of nearby galaxies (Corrigendum)

M. Querejeta; E. Schinnerer; S. Meidt; J. Sun; A. K. Leroy; E. Emsellem; R. S. Klessen; J. C. Muñoz-Mateos; H. Salo; E. Laurikainen; I. Bešlić; G. A. Blanc; M. Chevance; D. A. Dale; C. Eibensteiner; C. Faesi; A. García-Rodríguez; S. C. O. Glover; K. Grasha; J. Henshaw; C. Herrera; A. Hughes; K. Kreckel; J. M. D. Kruijssen; D. Liu; E. J. Murphy; H.-A. Pan; J. Pety; A. Razza; E. Rosolowsky; T. Saito; A. Schruba; A. Usero; E. J. Watkins; T. G. Williams

doi:10.1051/0004-6361/202557599e

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Erratum

This article is an erratum for:
[https://doi.org/10.1051/0004-6361/202140695]

Issue		A&A Volume 703, November 2025


Article Number		C1
Number of page(s)		2
Section		Extragalactic astronomy
DOI		https://doi.org/10.1051/0004-6361/202557599e
Published online		31 October 2025

A&A 703, C1 (2025)

Stellar structures, molecular gas, and star formation across the PHANGS sample of nearby galaxies (Corrigendum)

M. Querejeta¹^⋆, E. Schinnerer², S. Meidt³, J. Sun⁴, A. K. Leroy⁴, E. Emsellem⁵^,6, R. S. Klessen⁷^,8, J. C. Muñoz-Mateos², H. Salo⁹, E. Laurikainen⁹, I. Bešlić¹⁰, G. A. Blanc¹¹^,12, M. Chevance¹³, D. A. Dale¹⁴, C. Eibensteiner¹⁰, C. Faesi¹⁵, A. García-Rodríguez¹, S. C. O. Glover⁷, K. Grasha¹⁶, J. Henshaw², C. Herrera¹⁷, A. Hughes¹⁸^,19, K. Kreckel¹³, J. M. D. Kruijssen¹³, D. Liu², E. J. Murphy²⁰, H.-A. Pan², J. Pety¹⁷^,21, A. Razza¹², E. Rosolowsky²², T. Saito², A. Schruba²³, A. Usero¹, E. J. Watkins¹⁸ and T. G. Williams²

¹ Observatorio Astronómico Nacional (IGN), C/ Alfonso XII 3, E-28014 Madrid, Spain
² Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany
³ Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, B-9000 Gent, Belgium
⁴ Department of Astronomy, The Ohio State University, 140 West 18th Ave, Columbus, OH 43210, USA
⁵ European Southern Observatory, Karl-Schwarzschild-Straße 2, D-85748 Garching, Germany
⁶ Univ Lyon, Univ Lyon1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, F-69230 Saint-Genis-Laval, France
⁷ Universität Heidelberg, Zentrum für Astronomie, Albert-Ueberle-Straße 2, D-69120 Heidelberg, Germany
⁸ Universität Heidelberg, Interdisziplinäres Zentrum für Wissenschaftliches Rechnen, INF 205, D-69120 Heidelberg, Germany
⁹ Space Physics and Astronomy Research Unit, University of Oulu, Pentti Kaiteran katu 1, FI-90014, Finland
¹⁰ Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, D-53121 Bonn, Germany
¹¹ The Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA, 91101, USA
¹² Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
¹³ Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Mönchhofstraße 12-14, D-69120 Heidelberg, Germany
¹⁴ Department of Physics & Astronomy, University of Wyoming, Laramie, WY, 82071, USA
¹⁵ Department of Astronomy, University of Massachusetts, Amherst, 710 North Pleasant St., Amherst, MA, 01003, USA
¹⁶ Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia
¹⁷ IRAM, 300 rue de la Piscine, F-38406 Saint Martin d’Hères, France
¹⁸ CNRS, IRAP, 9 Av. du Colonel Roche, BP 44346, F-31028 Toulouse Cedex 4, France
¹⁹ Université de Toulouse, UPS-OMP, IRAP, F-31028 Toulouse Cedex 4, France
²⁰ NRAO, 520 Edgemont Road, Charlottesville, VA, 22903, USA
²¹ Sorbonne Université, Observatoire de Paris, Université PSL, CNRS, LERMA, F-75005 Paris, France
²² University of Alberta, 4-183 CCIS, Edmonton, Alberta, Canada
²³ Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße 1, D-85748 Garching, Germany

^⋆ Corresponding author: m.querejeta@oan.es

Key words: errata, addenda / galaxies: ISM / galaxies: star formation / galaxies: structure

Erratum for: A&A, 656, A133 (2021), https://doi.org/10.1051/0004-6361/202140695

We have identified an inconsistency between the bisector fits to the Kennicutt-Schmidt relation plotted in Fig. 7 (and Appendix A) and the fit parameters listed in Table 4. The fits from the table relied on a different masking scheme for the CO(2–1) emission line maps (‘broad’ masks as opposed to ‘flat’ masks), which affects the x-axis of the Kennicutt-Schmidt relation (Σ_mol). This alternative masking scheme reflects differences in the treatment of non-detections. This inconsistency does not affect any of the other results and conclusions presented in the paper.

The correct version of Table 4, which matches the fits plotted in Fig. 7, is provided below (Table 1). For completeness, we include as Fig. 1 an updated version of Fig. A.1, which consistently shows the fits from Table 4 using the same masking scheme for different α_CO recipes.

Table 1.

Bisector fits to the molecular Kennicutt–Schmidt relation for the different α_CO prescriptions.

Fig. 1.

Molecular Kennicutt–Schmidt relation for kpc-scale measurements in PHANGS–ALMA using alternative prescriptions for the α_CO conversion factor, as indicated in the top-left of each panel. The straight lines represent the best bisector fit to the data for the different environments, as indicated by the different colours. The numerical results of the bisector fits are listed in Table 1.

We thank Romane Cologni for pointing out this issue.

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.

This article is published in open access under the Subscribe to Open model. Subscribe to A&A to support open access publication.

All Tables

Table 1.

Bisector fits to the molecular Kennicutt–Schmidt relation for the different α_CO prescriptions.

In the text

All Figures

	Fig. 1. Molecular Kennicutt–Schmidt relation for kpc-scale measurements in PHANGS–ALMA using alternative prescriptions for the α_CO conversion factor, as indicated in the top-left of each panel. The straight lines represent the best bisector fit to the data for the different environments, as indicated by the different colours. The numerical results of the bisector fits are listed in Table 1.
In the text

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