A new fitting-function to describe the time evolution of a galaxy’s gravitational potential (Corrigendum)

Hans J. T. Buist; Amina Helmi

doi:10.1051/0004-6361/201323059e

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A&A, 589 (2016) C3

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Erratum

This article is an erratum for:
[https://doi.org/10.1051/0004-6361/201323059]

Issue		A&A Volume 589, May 2016


Article Number		C3
Number of page(s)		1
Section		Extragalactic astronomy
DOI		https://doi.org/10.1051/0004-6361/201323059e
Published online		12 April 2016

A&A 589, C3 (2016)

A new fitting-function to describe the time evolution of a galaxy’s gravitational potential (Corrigendum)

Hans J. T. Buist and Amina Helmi

Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands
e-mail: buist@astro.rug.nl

Key words: galaxies: evolution / dark matter / errata, addenda

Erratum for: A&A 563, A110 (2014), DOI: 10.1051/0004-6361/201323059

Fig. 1

Like Fig. 4 of Buist & Helmi (2014) but with the corrected values for the growth rate a_g.

The quoted values of the growth rate a_g for the Aquarius haloes in Fig. 4 of Buist & Helmi (2014) are too small by a factor log (10) ≈ 2. This growth rate stems from fitting the evolution of the scale mass M_s(t) and scale radius r_s(t) with a model where they grow as an exponential in redshift z $\begin{matrix} M_{s} (z) & \propto \exp {- 2 a_{g} z^{}}, \\ r_{s} (z) & \propto \exp {- 2 (a_{g} / γ^{)} z}, \end{matrix}$ $\begin{eqnarray} M_\text{s}(z) &&\propto \exp{\left\{-2 a_{\rm g} z\right\}} , \\ r_\text{s}(z) &&\propto \exp{\left\{-2 \left( a_{\rm g}/\gamma \right) z \right\}}, \end{eqnarray}$ such that M_s(t) and r_s(t) are related by a power law with coefficient γ. The quoted values of γ in the figure are correct. The curves shown in the figure are not affected, nor are any other figures in the article. A corrected version of Fig. 4 is shown in Fig. 1.

In the discussion of the results from the Milky-Way like Aquarius dark matter haloes we mentioned that the similarly defined growth rate a_c of M_vir(t) (see Wechsler et al. 2002) was in the range 0.1 to 0.2 for these haloes, which was below the 68% scatter of the median given by Wechsler et al. in their Fig. 8. With the correction above, we now find a_c in the range ≈0.2 to 0.4, which is still mostly below the median but within the 68% scatter.

The authors would like to thank Raphaël Errani for pointing out this error.

References

Buist, H. J. T., & Helmi, A. 2014, A&A, 563, A110 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Wechsler, R. H., Bullock, J. S., Primack, J. R., Kravtsov, A. V., & Dekel, A. 2002, ApJ, 568, 52 [NASA ADS] [CrossRef] [Google Scholar]

© ESO, 2016

All Figures

	Fig. 1 Like Fig. 4 of Buist & Helmi (2014) but with the corrected values for the growth rate a_g.
In the text

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[1] Buist, H. J. T., & Helmi, A. 2014, A&A, 563, A110 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]

[2] Wechsler, R. H., Bullock, J. S., Primack, J. R., Kravtsov, A. V., & Dekel, A. 2002, ApJ, 568, 52 [NASA ADS] [CrossRef] [Google Scholar]