Volume 559, November 2013
|Number of page(s)||1|
|Published online||18 November 2013|
Thermodynamic fluctuations in solar photospheric three-dimensional convection simulations and observations (Corrigendum)
Instituto de Astrofísica de Canarias (IAC), Calle Vía Láctea s/n, 38205 La Laguna,
2 Departamento de Astrofísica, Universidad de La Laguna (ULL), 38206, La Laguna, Tenerife, Spain
3 National Solar Observatory (NSO), 3010 Coronal Loop, 88349 Sunspot, New Mexico, USA
e-mail: firstname.lastname@example.org, email@example.com, firstname.lastname@example.org
4 Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
5 Kiepenheuer-Institut für Sonnenphysik (KIS), Schöneckstr. 6, 79104 Freiburg, Germany
Key words: Sun: photosphere / methods: data analysis / line: profiles / errata, addenda
We detected an error in the calculation of the stray-light contributions for the different observations which, however, does not affect any other result in the paper. To determine the stray-light contribution corresponding to the different spatial convolution kernels for the respective observations, a two-dimensional (2D) version of the kernel was constructed from the one-dimensional (1D) kernel given by Eq. (5) in Beck et al. (2013, hereafter BE13). By mistake, we normalized the full 1D kernel to unit area, i.e. , instead of normalizing . A second, conceptual mistake was to use the spatial sampling of the simulation’s spectra of 013 instead of re-sampling the values to the actual spatial sampling of the observations (cf. Table 1 in BE13). In addition, the values of the parameter a were given in pixels instead of arcseconds in both Fig. 3 and Table 2 of BE13. The corrected values of a and the stray-light estimates are given in Table 1 below to replace those in Table 2 of BE13. The scale of the y-axes in Fig. 3 of BE13 needs to be multiplied with 013 to obtain the corresponding values in arc-seconds (as given in Table 1 below), e.g., in the case of the SP, a = 0.16 pixel, as marked in the figure, which corresponds to 0.02′′.
As a consequence of the changed stray-light estimates, the following sentences in the text have to be modified:
Abstract: “The spatial degradation kernels yield a similargeneric spatial stray-light contamination of about 30% for allinstruments” should be replaced by “The spatial degradationkernels yield a generic spatial stray-light contamination between~20% and ~70%”.
p. 6, “where I(x′,y′,λ) are the synthetic spectra of the HD simulation at full resolution (HD-FR) and x and ydenote the pixel column and row inside the FOV, respectively” should be replaced by “where I(x′,y′,λ) are the synthetic spectra of the HD simulation at full resolution (HD-FR) after re-sampling them and the kernel to the spatial sampling of the respective observation, while x and y denote the pixel column and row inside the re-sampled FOV, respectively”.
p. 6, “All spectrograph data (SP, POLIS, TIP, Echelle) and the destretched GFPI data yield a value ≳30%, with little to no dependence on the spatial resolution” should be replaced by “All spatially under-sampled spectrograph data (SP, POLIS, TIP) yield similar values of about 20–30%, with little to no dependence on the spatial resolution”.
p. 6, “The only clear reduction of stray light is seen for the deconvolved GFPI spectra, where in the deconvolution process some inverse kernel was already applied” should be replaced by “A clear reduction of stray light by 20% is seen for the MOMFBD GFPI spectra relative to the destretched GFPI data, because in the deconvolution process some inverse kernel was already applied”.
Top row: “best” degradation kernel parameters a and FWHM(σ) for each instrument. Second row: average spatial stray-light level α corresponding to each of those “best” kernels.
We thank G. Scharmer for pointing out to us that the stray-light estimates did not match the kernel properties and the spatial sampling.
© ESO, 2013
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