Volume 603, July 2017
|Number of page(s)||1|
|Published online||24 July 2017|
Testing core creation in hydrodynamical simulations using the HI kinematics of field dwarfs (Corrigendum)
1 Kapteyn Astronomical Institute, University of Groningen, Landleven 12, 9747 AD Groningen, The Netherlands
e-mail: firstname.lastname@example.org; email@example.com
2 Research School of Astronomy & Astrophysics, Australian National University, Canberra, ACT 2611, Australia
Key words: galaxies: kinematics and dynamics / dark matter / galaxies: dwarf / galaxies: halos / radio lines: galaxies / errata, addenda
In the published version of this article, items of an enumerated list in Sect. 4.1 have mistakenly been replaced by bullet points. Headings of Sect. 4.1 should read as follow: “i) Cosmologically representative dwarf sample. ii) No large observational systematics in the measurement of HI kinematics. iii) Observed HI kinematics accurately reflect the true circular velocity profile”.
Consequently, the last sentence of Sect. 3.2 should be read as follows: “We therefore always apply corrections for pressure support to the measured Vout, HI values for our sample of observed dwarfs (see item iii in Sect. 4.1 for details on pressure-support corrections, and for a discussion of the important remaining caveats associated with our comparison between observed and simulated kinematics)”.
In addition, the last paragraph of Sect. 5 should be read as follows: “We would like to stress that the results we present in Fig. 1 are only valid under a set of implicit assumptions. The first isthat our sample of dwarfs with spatially resolved HI kinematics is representative of the overall population of field dwarfs. This may not be the case since our sample has been compiled from the literature and lacks a common set of selection criteria (item i in Sect. 4.1). Second, we assume that no large observational systematics affect the kinematic measurements of our sample of HI dwarfs. The main worry in this context is the possibility of a systematic overestimation of galactic inclinations (item ii in Sect. 4.1). Third, the comparison between halo RCs and measured HI velocities assumes that the HI kinematics reflect (up to corrections) the true underlying halo potential. This may not be the case if, for example, the HI velocity field is very complex or if the HI disk is very thick (item iii in Sect. 4.1). Assumptions i and ii can be tested in the near future with the data provided by next-generation HI interferometric surveys. On the other hand, assumption iii may be very difficult to test in practice since the true underlying potential in which a dwarf galaxy is embedded is not an observable quantity.”.
© ESO, 2017
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