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
A&A
Astronomy & Astrophysics
P. M. Vreeswijk 3
C. Ledoux 1
A. Smette 1
S. L. Ellison 0
A. O. Jaunsen 7
M. I. Andersen 5 6
A. S. Fruchter 4
J. P. U. Fynbo 5
J. Hjorth 5
A. Kaufer 1
P. Møller 9
P. Petitjean 8
S. Savaglio 2
R. A. M. J. Wijers 10
0 Department of Physics and Astronomy, University of Victoria , Victoria, BC , Canada
1 European Southern Observatory , Alonso de Córdova 3107, Casilla 19001, Santiago 19 , Chile
2 Max-Planck-Institut für Extraterrestrische Physik , Giessenbachstrasse, 85748 Garching bei München , Germany
3 Centre for Astrophysics and Cosmology, Science Institute, University of Iceland , Dunhagi 5, 107 Reykjavík , Iceland
4 Space Telescope Science Institute , 3700 San Martin Drive, Baltimore, MD 21218 , USA
5 Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen , 2100 Copenhagen , Denmark
6 Space Science Center, Niels Bohr Institute, University of Copenhagen , 2100 Copenhagen , Denmark
7 Institute of Theoretical Astrophysics, University of Oslo , PO Box 1029 Blindern, 0315 Oslo , Norway
8 Institut d'Astrophysique de Paris, UMR 7095 CNRS & Université Pierre et Marie Curie , 98bis boulevard Arago, 75014 Paris , France
9 European Southern Observatory , Karl-Schwarzschild-Str. 2, 85748, Garching bei München , Germany
10 Astronomical Institute Anton Pannekoek and GRAPPA , Science Park 904, 1098 XH, Amsterdam , The Netherlands
(Corrigendum ); Gamma rays; bursts - galaxies; abundances - galaxies; ISM - galaxies; distances and redshifts - quasars; absorption lines - errata; addenda
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We have recently realized that, in Eq. (3) in
Vreeswijk et al.
(2007)
, the flux Fν(τ0) should be divided by 4 π. The relation
should therefore read as follows:
dNu = Nl Blu Fν(τ0)
dt 4 π
− Nu Aul + Bul
Fν(τ0)
4 π
·
(3)
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 √4 π ∼ 3.5.
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 √4 π. The main conclusions of these two papers are not
affected by this change either.
Fox , A. J. , Ledoux , C. , Vreeswijk , P. M. , Smette , A. , & Jaunsen , A. O. 2008 , A &A, 491 , 189
Ledoux , C. , Vreeswijk , P. M. , Smette , A. , et al. 2009 , A &A, 506 , 661 Silva, A. I. & Viegas , S. M. 2002 , MNRAS, 329 , 135
Vreeswijk , P. M. , Ledoux , C. , Smette , A. , et al. 2007 , A &A, 468 , 83 (...truncated)