EDP Sciences
Free Access
Issue
A&A
Volume 556, August 2013
Article Number A23
Number of page(s) 12
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361/201220968
Published online 19 July 2013

Online material

Appendix A: The afterglow light curve

The afterglow of GRB 110918A was imaged for over 40 days after the trigger with GROND in the grizJHKS bands (outlined in Sect. 2.2). Using the deep observations of the host, the underlying contribution from the host galaxy was subtracted implementing the High Order Transform of PSF and Template Subtraction package, HOTPANTS11 v5.1.10b. The resulting afterglow light curve can be seen in Fig. A.1, while the raw data can be found in Tables A.2 and A.3 and the host subtracted data in Tables A.4 and A.5. The standard stars used in griz′ for relative calibration can be found in Table A.1.

thumbnail Fig. A.1

Afterglow light curve of GRB 110918A obtained with the 7-channel imager GROND (host subtracted).

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Table A.1

Optical reference stars.

Table A.2

GROND photometric data griz′.

Table A.3

GROND photometric data JHKs.

Table A.4

GROND host-subtracted photometric data griz′.

Table A.5

GROND host subtracted photometric data JHKs.

Appendix B: The afterglow’s sight-line spectrum

The spectra obtained with GMOS and OSIRIS (see Sect. 2.6) reveal many absorption lines of gas along the line-of-sight toward the afterglow, specifically of the following species: Fe ii (2344, 2374, 2382, 2586, 2600), Mg ii (2803, 2796), Mg i (2853), and Ca ii (3935, 3970). The equivalent widths of the metals are listed in Table B.1.

Table B.1

Equivalent widths measured for the absorption lines of the afterglow.

Appendix C: The host’s emission lines

Two spectra of the host galaxy were obtained with OSIRIS and X-shooter (see Sect. 3.3), showing the following emission lines: Hα and Hβ transitions from the Balmer series and also forbidden transitions of [O ii] and [N ii] (only [O ii] emission was detected with OSIRIS, and so for consistency only the X-shooter emission lines are shown). All of the 2D spectral images and 1D Gaussian fits can be seen in Fig. C.1.

thumbnail Fig. C.1

2D spectra of the host of GRB 110918A depicting four different emissions ([N ii], [O ii], Hα, Hβ). Overplotted is our Gaussian fit, where areas that overlay telluric lines are shown in white and excluded from the fit. All the values presented are raw values and do not include slit-loss or extinction corrections. Each image has been smoothed in both pixel directions for presentation purposes. a) The Balmer series transition Hα; b) the Balmer series transition Hβ; c) the forbidden transition [N ii]; d) the forbidden transition [O ii].

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© ESO, 2013

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