GMASS ultradeep spectroscopy of galaxies at z ~ 2 - V. Witnessing the assembly at z = 1.6 of a galaxy cluster

Free Access

Issue		A&A Volume 504, Number 2, September III 2009


Page(s)		331 - 346
Section		Cosmology (including clusters of galaxies)
DOI		https://doi.org/10.1051/0004-6361/200809964
Published online		15 July 2009

Online Material

Appendix A: Spectra and images of the member galaxies

Figures A.1-A.4 show the spectra and images of the member galaxies.

$\begin{figure} \par\includegraphics[width=18cm]{09964f08.ps} % \end{figure}$

Figure A.1:

Spectra and postage stamp images of the 42 member galaxies. Wavelength in Ångstrom on the horizontal axis and flux in 10^-19 erg s^-1 Å^-1 cm^-2. Uncertainties caused by background noise are indicated by the underlying filled grey spectra. As the flux calibration of the GOODS spectra is not very accurate (Vanzella et al. 2006) but the absolute flux level of these spectra seem systematically higher than the GMASS spectra (for the same magnitudes), they have been divided by a factor two. The origin of the spectra is plotted: GMASS (Kurk et al., in prep.) or GOODS (Vanzella et al. 2006), the GMASS identification numbers, and the spectroscopic classes (see text). Robust (tentative) spectral features are shown by solid (dashed) lines with numbers (see below). The postage stamps are constructed from the HST/ACS observations in the B, V, and I bands, convolved with a Gaussian kernel. Indicated are the morphological class (on the left) and the z magnitude (on the right). The spectra are sorted on z-J colour, starting with the reddest galaxies. The numbers for the spectral features refer to: (1) Si II $\lambda$ 1527, (2) C IV $\lambda$ 1550, (3) Fe II $\lambda$ 1608, (4) Al II $\lambda$ 1671, (5) Al III $\lambda$ 1855, (6) C III] $\lambda$ 1909, (7) Fe III $\lambda$ 1926, (8) C II] $\lambda$ 2326, (9) Fe II $\lambda$ 2344, (10) Fe II $\lambda$ 2375, (11) Fe II $\lambda$ 2383, (12) Fe II $\lambda$ 2587, (13) Fe II $\lambda$ 2600, (14) Mg II $\lambda$ 2796, (15) Mg II $\lambda$ 2804, (16) Mg I $\lambda$ 2853, (17) [O II] $\lambda$ 3727.

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$\begin{figure} \par\includegraphics[width=18cm]{09964f09.ps} % \end{figure}$	Figure A.2: See Fig. A.1 for description.
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$\begin{figure} \par\includegraphics[width=18cm]{09964f10.ps} % \end{figure}$	Figure A.3: See Fig. A.1 for description.
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$\begin{figure} \par\includegraphics[width=18cm]{09964f11.ps} % \end{figure}$	Figure A.4: See Fig. A.1 for description.
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