Rapid-response mode VLT/UVES spectroscopy of GRB 060418 (Corrigendum) - Conclusive evidence for UV pumping from the time evolution of Fe II and Ni II excited- and metastable-level populations

P. M. Vreeswijk; C. Ledoux; A. Smette; S. L. Ellison; A. O. Jaunsen; M. I. Andersen; A. S. Fruchter; J. P. U. Fynbo; J. Hjorth; A. Kaufer; P. Møller; P. Petitjean; S. Savaglio; R. A. M. J.  Wijers

doi:10.1051/0004-6361/20066780e

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Erratum

This article is an erratum for:
[https://doi.org/10.1051/0004-6361/200811572]
[https://doi.org/10.1051/0004-6361:200810286]
[https://doi.org/10.1051/0004-6361:20066780]

Issue		A&A Volume 532, August 2011


Article Number		C3
Number of page(s)		1
Section		Extragalactic astronomy
DOI		https://doi.org/10.1051/0004-6361/20066780e
Published online		03 August 2011

A&A 532, C3 (2011)

Rapid-response mode VLT/UVES spectroscopy of GRB 060418 (Corrigendum)

Conclusive evidence for UV pumping from the time evolution of Fe II and Ni II excited- and metastable-level populations

P. M. Vreeswijk¹, C. Ledoux², A. Smette², S. L. Ellison³, A. O. Jaunsen⁴, M. I. Andersen⁵^,6, A. S. Fruchter⁷, J. P. U. Fynbo⁶, J. Hjorth⁶, A. Kaufer², P. Møller⁸, P. Petitjean⁹, S. Savaglio¹⁰ and R. A. M. J. Wijers¹¹

¹ Centre for Astrophysics and Cosmology, Science Institute, University of Iceland, Dunhagi 5, 107 Reykjavík, Iceland
e-mail: pmv@raunvis.hi.is
² European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Santiago 19, Chile
³ Department of Physics and Astronomy, University of Victoria, Victoria, BC, Canada
⁴ Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029 Blindern, 0315 Oslo, Norway
⁵ Space Science Center, Niels Bohr Institute, University of Copenhagen, 2100 Copenhagen, Denmark
⁶ Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, 2100 Copenhagen, Denmark
⁷ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
⁸ European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748, Garching bei München, Germany
⁹ Institut d’Astrophysique de Paris, UMR 7095 CNRS & Université Pierre et Marie Curie, 98bis boulevard Arago, 75014 Paris, France
¹⁰ Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, 85748 Garching bei München, Germany
¹¹ Astronomical Institute Anton Pannekoek and GRAPPA, Science Park 904, 1098 XH, Amsterdam, The Netherlands

Key words: Gamma rays: bursts / galaxies: abundances / galaxies: ISM / galaxies: distances and redshifts / quasars: absorption lines / errata, addenda

Erratum for: A&A 468, 83-96 (2007), DOI: 10.1051/0004-6361:20066780

Erratum for: A&A 491, 189-207 (2008), DOI: 10.1051/0004-6361:200810286

Erratum for: A&A 506, 661-675 (2009), DOI: 10.1051/0004-6361/200811572

We have recently realized that, in Eq. (1) in Vreeswijk et al. (2007), the flux F_ν(τ₀) should be divided by 4 π. The relation should therefore read as follows:

$\frac{d N_{u}}{d t} = N_{l} B_{lu} \frac{F_{ν} (τ_{0})}{4 π} - N_{u} [A_{ul} + B_{ul} \frac{F_{ν} (τ_{0})}{4 π}] \cdot$ $\begin{equation} \frac{{\rm d}N_{\rm u}}{{\rm d}t} = N_{\rm l} B_{\rm lu} \frac{F_{\nu}(\tau_0)}{4\,\pi} - N_{\rm u} \left[A_{\rm ul}+B_{\rm ul} \frac{F_{\nu}(\tau_0)}{4\,\pi}\right]\cdot \label{eq:dndt} \end{equation}$ (1)Using this relation, our excitation program is now fully consistent with the PopRatio code (Silva & Viegas 2002, see also Sect. 5.2) when neglecting collisional excitation, and in the optically thin regime as PopRatio assumes all transitions are optically thin. The consequence is that excitation is a factor of 4 π less effective than we had previously assumed, resulting in a decreased distance estimate by a factor of $\sqrt{4 π} ~ 3.5$ $\hbox{$\sqrt{4\,\pi}\sim3.5$}$ . Therefore, the distance of GRB 060418 to the neutral absorbing material – previously d = 1.7 ± 0.2 kpc – needs to be revised to d = 0.48 ± 0.06 kpc, under the same model assumptions. The main conclusion of the paper, that the neutral absorbing gas is not in the immediate environment of GRB 060418, remains the same.

Since we applied the same excitation analysis in Sect. 4.1.3 of Fox et al. (2008) and in Sect. 2.3 of Ledoux et al. (2009), the distance estimates therein should also be scaled down by a factor of $\sqrt{4 π}$ $\hbox{$\sqrt{4\,\pi}$}$ . The main conclusions of these two papers are not affected by this change either.

References

Fox, A. J., Ledoux, C., Vreeswijk, P. M., Smette, A., & Jaunsen, A. O. 2008, A&A, 491, 189 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Ledoux, C., Vreeswijk, P. M., Smette, A., et al. 2009, A&A, 506, 661 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Silva, A. I., & Viegas, S. M. 2002, MNRAS, 329, 135 [NASA ADS] [CrossRef] [Google Scholar]
Vreeswijk, P. M., Ledoux, C., Smette, A., et al. 2007, A&A, 468, 83 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]

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[1] Fox, A. J., Ledoux, C., Vreeswijk, P. M., Smette, A., & Jaunsen, A. O. 2008, A&A, 491, 189 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]

[2] Ledoux, C., Vreeswijk, P. M., Smette, A., et al. 2009, A&A, 506, 661 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]

[3] Silva, A. I., & Viegas, S. M. 2002, MNRAS, 329, 135 [NASA ADS] [CrossRef] [Google Scholar]

[4] Vreeswijk, P. M., Ledoux, C., Smette, A., et al. 2007, A&A, 468, 83 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]