Star formation efficiency along the radio jet in Centaurus A (Corrigendum)
1 LERMA, Observatoire de Paris, CNRS UMR 8112, 61 avenue de l’Observatoire, 75014 Paris, France
e-mail: quentin.salome@obspm.fr
2 Collège de France, 11 place Marcelin Berthelot, 75005 Paris, France
3 CSIRO Astronomy & Space Science, PO Box 76, Epping, NSW 1710, Australia
4 Department of Physics & Electronics, Rhodes University, PO Box 94, 6140 Grahamstown, South Africa
Key words: methods: data analysis / galaxies: individual: Centaurus A / galaxies: evolution / galaxies: interactions / galaxies: star formation / errata, addenda
In Sect. 2.5, we did not take into account the CO(2−1)/CO(1−0) ratio to derive the mass of the clumps observed by ALMA. This corresponds to an error of a factor of about two, compared with that obtained when using the ratio of 0.55 given by Charmandaris et al. (2000). With such a factor, the total molecular gas mass of the clumps is MHS ~ 1.6 × 105 M⊙. We provide a new version of Table 2, which shows the corrected values of the molecular gas mass for the clumps.
CO(2−1) emission line properties for each clump (central velocity, FWHM, and molecular gas mass estimated with a standard and fixed conversion factor with no metallicity correction).
© ESO, 2016
All Tables
CO(2−1) emission line properties for each clump (central velocity, FWHM, and molecular gas mass estimated with a standard and fixed conversion factor with no metallicity correction).