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Erratum: "A 33 GHz Survey of Local Major Mergers: Estimating the Sizes of the Energetically Dominant Regions from High-resolution Measurements of the Radio Continuum" (2017, ApJ, 843, 117)

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Published 2017 November 2 • © 2017. The American Astronomical Society. All rights reserved.
, , Citation L. Barcos-Muñoz et al 2017 ApJ 849 74 DOI 10.3847/1538-4357/aa9330

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Author e-mails

loreto.barcos@alma.cl

Author affiliations

1 Joint ALMA Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile; loreto.barcos@alma.cl

2 National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA

3 Department of Astronomy, University of Virginia, 530 McCormick Road, Charlottesville, VA 22904, USA

4 Astronomy Department, The Ohio State University, 140 W 18th Street, Columbus, OH 43210, USA

5 Instituto de Astrofísica, Facultad de Física, Pontificia universidad Católica de Chile, Casilla 306, Santiago, Chile

6 Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile

7 Department of Astronomy and Center for Cosmology & Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA

8 Spitzer Science Center, California Institute of Technology, MC 220-6, 1200 East California Boulevard, Pasadena, CA 91125, USA

9 Núcleo de Astronomía de la Facultad de Ingeniería, Universidad Diego Portales, Av. Ejército Libertador 441, Santiago, Chile

10 Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology, Pasadena, CA 91125, USA

11 New Mexico Institute of Mining and Technology, 801 Leroy Place, Socorro, NM 87801, USA

12 National Radio Astronomy Observatory, P.O. Box O, 1003 Lopezville Road, Socorro, NM 87801, USA

13 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96816, USA

14 Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany

15 Spitzer Science Center, MS 314-6, California Institute of Technology, Pasadena, CA 91125, USA

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Dates

  1. Received 2017 October 12
  2. Accepted 2017 October 12
  3. Published

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0004-637X/849/1/74

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Due to an error at the publisher, Figure 1 was published without the second page of panels. The complete version of Figure 1 appears here. IOP Publishing sincerely regrets this error.

Figure 1.

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Figure 1.

Figure 1. Contour and color maps of ∼33 GHz continuum emission of each galaxy in our sample. The contours are spaced by a factor of two in intensity, with the outermost contour set to 5 times the rms noise in the map. The beam for each map appears as a boxed black ellipse in the bottom left corner. The scale bar for each map appears in the bottom right corner. The white crosses indicate the location of compact sources whose properties were derived from Gaussian fits (see Section 3.4 of the original article). The red contour encloses 50% of the total flux density at 33 GHz; we use the area inside this contour, A50, as a characteristic size for the energetically dominant part of the galaxy. Most of the emission in our sample is compact, with only a few systems showing considerable extended emission (e.g., VV 340a) and others showing a combination of compact and extended emission (e.g., UGC 08387).

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10.3847/1538-4357/aa9330