Volume 613, May 2018
|Number of page(s)||1|
|Published online||31 May 2018|
Subarcsecond international LOFAR radio images of Arp 220 at 150 MHz
A kpc-scale star forming disk surrounding nuclei with shocked outflows (Corrigendum)
Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory,
2 Department of Astronomy, University of Virginia, 530 McCormick Road, Charlottesville, VA 22904, USA
3 The Netherlands Institute for Radio Astronomy (ASTRON), PO Box 2, 7990 AA Dwingeloo, The Netherlands
4 Now at: Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia
5 Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Manchester M13 9PL, UK
6 Instituto de Astrofísica de Andalucía (IAA, CSIC), Glorieta de las Astronomía, s/n, 18008 Granada, Spain
7 Departamento de Física Teorica, Facultad de Ciencias, Universidad de Zaragoza, Spain
8 Department of Astronomy, University of Wisconsin-Madison, WI 53706, USA
9 Department of Physics, University of Wisconsin-Madison, WI 53706, USA
10 Center for Magnetic Self-Organization in Laboratory and Astrophysical Plasmas, University of Wisconsin-Madison, WI 53706, USA
11 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
12 Now at: Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
13 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
Accepted: 20 November 2017
Key words: ISM: structure / techniques: high angular resolution / galaxies: individual: Arp 220 / galaxies: starburst / errata, addenda
In Sect. 3.2.1 of Varenius et al. (2016), Eq. (2) was missing an exponent. The correct equation is (1)
as given by Kim & Trippe (2014). Although written incorrectly in the text, we emphasize that the correct equation was used to generate Figs. 5b–d.
The peak surface brightness values published in Table 3 and Fig. 7 for convolved images were given as twice the true values. A factor of two was missing when converting from convolved units of Jy beam−1 into Jy arcsec−2. The correct values are given here in Table 1 and Fig. 1. We note that since both measured and simulated values were scaled by the same factor, the ratio of 60% referred to in Sect. 4.3.1 was correct, although the model surface brightness quoted at 150 MHz (after convolving to 0.′′7 × 0.′′5) should be corrected to 90 mJy arcsec−2. We emphasize that the error in these peak surface brightness values does not affect the modeling or conclusions in the paper as these were based on integrated flux densities or peak values in units of Jy beam−1.
© ESO 2018
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