Study of the X-ray activity of Sagittarius A* during the 2011 XMM-Newton campaign (Corrigendum)

Enmanuelle Mossoux; Nicolas Grosso; Frédéric H. Vincent; Delphine Porquet

doi:10.1051/0004-6361/201424682e

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Erratum

This article is an erratum for:
[https://doi.org/10.1051/0004-6361/201424682]

Issue		A&A Volume 580, August 2015


Article Number		C2
Number of page(s)		1
Section		Galactic structure, stellar clusters and populations
DOI		https://doi.org/10.1051/0004-6361/201424682e
Published online		30 July 2015

A&A 580, C2 (2015)

Study of the X-ray activity of Sagittarius A* during the 2011 XMM-Newton campaign (Corrigendum)

Enmanuelle Mossoux¹, Nicolas Grosso¹, Frédéric H. Vincent² and Delphine Porquet¹

¹ Observatoire Astronomique de Strasbourg, Université de Strasbourg, CNRS, UMR 7550, 11 rue de l’Université, 67000 Strasbourg, France
e-mail: enmanuelle.mossoux@astro.unistra.fr
² Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warszawa, Poland

Key words: Galaxy: center / X-rays: individuals: Sgr A* / radiation mechanisms: general / errata, addenda

Erratum for: A&A 573, A46 (2015), DOI: 10.1051/0004-6361/201424682

The weight equation in Sect. 3.1 of Mossoux et al. (2015) unfortunately features a typo. The correct equation should read: $w = \frac{C R_{src + bkg}}{C R_{src + bkg} - C R_{bkg}}$ $\begin{equation} w=\frac{CR_{\mathrm{src+bkg}}}{CR_{\mathrm{src+bkg}}-CR_{\mathrm{bkg}}} \end{equation}$ (1)with CR_{src + bkg} the count rate of the Bayesian block of the source+background event list and CR_bkg the count rate of the corresponding Bayesian block of the background that is surface-corrected. As introduced in the first preprint version of the proceeding of Scargle et al. (2013), this weight equation adjusts the Voronoi time-interval in order to subtract the average background. The results presented in Mossoux et al. (2015) remain unchanged since they were all obtained following the recipe of Scargle et al. (2013) and using the correct equation for the Voronoi time-interval weighting.

Therefore, the “alternative” photon-weighting recently tested by Worpel & Schwope (2015) in their Sect. 4.6 (w ≡ 1 − CR_bkg/CR_{src + bkg}) is actually equivalent to the recipe of Scargle et al. (2013) that we used in Mossoux et al. (2015) since the photon-weighting is equal to the inverse of the Voronoi time-interval weighting. Indeed, the “alternative” photon-weighting of Worpel & Schwope (2015) is identical to those used in Eq. (1) of Mossoux et al. (2015) to compute smoothed light-curve.

References

Mossoux, E., Grosso, N., Vincent, F. H., & Porquet, D. 2015, A&A, 573, A46 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Scargle, J. D., Norris, J. P., Jackson, B., & Chiang, J. 2013, 2012 Fermi Symp. Proc. − eConf C121028 [arXiv:1304.2818v1] [Google Scholar]
Worpel, H., & Schwope, A. D. 2015, A&A, 578, A80 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]

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[1] Mossoux, E., Grosso, N., Vincent, F. H., & Porquet, D. 2015, A&A, 573, A46 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]

[2] Scargle, J. D., Norris, J. P., Jackson, B., & Chiang, J. 2013, 2012 Fermi Symp. Proc. − eConf C121028 [arXiv:1304.2818v1] [Google Scholar]

[3] Worpel, H., & Schwope, A. D. 2015, A&A, 578, A80 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]