Overview of an extensive multi-wavelength study of GX 339−4 during the 2010 outburst (Corrigendum)

M. Cadolle Bel; J. Rodriguez; P. D’Avanzo; D. M. Russell; J. Tomsick; S. Corbel; F. W. Lewis; F. Rahoui; M. Buxton; P. Goldoni; E. Kuulkers

doi:doi:10.1051/0004-6361/201117684e

Free access

This article is an erratum for: [this article]

Issue		A&A Volume 544, August 2012


Article Number		C2
Number of page(s)		1
Section		Stellar structure and evolution
DOI		http://dx.doi.org/10.1051/0004-6361/201117684e
Published online		07 August 2012

A&A 544, C2 (2012)

Overview of an extensive multi-wavelength study of GX 339−4 during the 2010 outburst (Corrigendum)

M. Cadolle Bel¹, J. Rodriguez², P. D’Avanzo³, D. M. Russell⁴, J. Tomsick⁵, S. Corbel², F. W. Lewis⁶, F. Rahoui⁷, M. Buxton⁸, P. Goldoni⁹ and E. Kuulkers¹

¹ ESAC, ISOC, Villañueva de la Cañada, Madrid, Spain
e-mail: Marion.Cadolle@sciops.esa.int
² Laboratoire AIM, UMR 7158, CEA/DSM – CNRS – Université Paris Diderot, IRFU/SAp, Gif-sur-Yvette, France
³ INAF, Osservatorio Astronomico di Brera, 23807 Merate, Italy
⁴ University of Amsterdam (Anton Pannekoek Institute), The Netherlands
⁵ SSL/California University, Berkeley, USA
⁶ Faulkes Telescope Project, University of Glamorgan, Wales, UK
⁷ Astronomy Department, Harvard University & Harvard-Smithsonian Center for Astrophysics, Cambridge, USA
⁸ Astronomy Department, Yale University, USA
⁹ Laboratoire APC, UMR 7164, CEA/DSM – CNRS – Université Paris Diderot, IRFU/SAp, Paris, France

Key words: black hole physics / stars: individual: GX 339 / 4 / X-rays: binaries / gamma rays: general / infrared: general / errata, addenda

Erratum of: A&A 534, A119 (2011), DOI: 10.1051/0004-6361/201117684

By mistake, three flux density values of UVOT were erroneously reported in Fig. 7 (uw1 on MJD = 55 260.21, uw2 on MJD = 55 281.78 and on MJD = 55 297.96). The correct figure is reported here (Fig. 1). None of the conclusions of our paper are affected by this change, given that only the data points of the spectral energy distribution (SED) obtained on MJD = 55 303.30 were modeled. The authors thank Dr. Z. Yan for pointing out the inconsistency, and we apologize for any confusion this may have caused.

Fig. 1

Compiled SEDs with UVOT, REM, SMARTS (M. Buxton et al. 2012, AJ, 143, 130) and FTS data at distinct MJD: MJD = 55 260.21 (UVOT/uw1, u and REM/V, R, I, J, H, K); MJD = 55 281.78 (UVOT/uw2 and FTS/V, R, i′); MJD = 55 297.96 (UVOT/uw2, FTS/R, i′ and SMARTS/V, H) and MJD = 55 303.30 (UVOT/uw2, um2, uw1, u, b, v, SMARTS/V, I, J, H and REM/R). The error bar is so large that the fluxes of uw1, um2 and uw2 are comparable (within the errors).

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© ESO, 2012

All Figures

	Fig. 1 Compiled SEDs with UVOT, REM, SMARTS (M. Buxton et al. 2012, AJ, 143, 130) and FTS data at distinct MJD: MJD = 55 260.21 (UVOT/uw1, u and REM/V, R, I, J, H, K); MJD = 55 281.78 (UVOT/uw2 and FTS/V, R, i′); MJD = 55 297.96 (UVOT/uw2, FTS/R, i′ and SMARTS/V, H) and MJD = 55 303.30 (UVOT/uw2, um2, uw1, u, b, v, SMARTS/V, I, J, H and REM/R). The error bar is so large that the fluxes of uw1, um2 and uw2 are comparable (within the errors).
Open with DEXTER
In the text

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