EDP Sciences
Free Access
Volume 557, September 2013
Article Number L18
Number of page(s) 6
Section Letters
DOI https://doi.org/10.1051/0004-6361/201322065
Published online 23 September 2013

Online material

Appendix A: Prompt emission

Table A.1 displays the results of the spectral fitting of the Fermi/GBM data.

Table A.1

GBM energy analysis of the 3 main γ-ray peaks and of the complete burst.

Appendix B: Observations

Table B.1 presents the observing log of our optical, NIR, and mm/submm observations.

Table B.1

Observing log.

thumbnail Fig. B.1

KS-band images of the field of GRB 120624B obtained 1 day after the burst (left), where the afterglow is still visible, and 6 months later (right) when only the host galaxy remains. The seeing in both frames is ~0.4′′.

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Appendix C: Spectral energy distribution and intrinsic extinction

Figure C.1 shows the fit of the NIR to X-ray SED with an extinguished power law. From this fit we derive a minimum intrinsic extinction in the line of sight of the GRB of AV = 1.5 mag, as described in Sect. 3.1.

thumbnail Fig. C.1

Near-infrared to X-ray SED at ~2 days, showing an estimation of the minimum extinction necessary to explain the detection limits. Filled circles indicate NIR and X-ray afterglow detections, whereas empty circles with arrows mark detection limits. The thick line is the minimum slope needed between NIR and X-rays to explain the detections, and the dashed line is the same slope after adding the Galactic extinction and an intrinsic extinction of AV = 1.5 mag.

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Appendix D: Spectral line fluxes

Table D.1 presents the results of fitting Gaussians to the host galaxy emission lines. In the case of the [O iiλλ3727, 3729 doublet and owing to the low S/N of the feature, the width of the Gaussian was fixed to σ = 100 km s-1 in order to constrain the number of free parameters in the fit. In all cases the spectral extractions were done with apertures of 1.4′′, which is well above the 0.9′′ seeing to minimise the loss of light. The flux errors do not include any systematic error in the absolute flux calibration, which can be estimated at ~20%.

Table D.1

Fits to the emission lines of the host galaxy.

© ESO, 2013

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