XMM-Newton detection of two clusters of galaxies with strong SPT Sunyaev-Zel'dovich effect signatures

Free Access

Issue		A&A Volume 514, May 2010


Article Number		L3
Number of page(s)		6
Section		Letters
DOI		https://doi.org/10.1051/0004-6361/201014434
Published online		18 May 2010

Online Material

Appendix A: Supplementary electronic material

$\begin{figure} \par\includegraphics[width=9cm,clip]{14434f2a.ps} \end{figure}$

Figure A.1:

The growth curve of SPT-CL J2332-5358: red curve shows the integrated flux as a function of outer integration radius for the MOS2 camera in the 0.5-2.0 keV band. Error bars on the growth curve indicate the Poisson error of the flux measurement including a 5% systematic error in the background estimation. Source flux is detected out to $196\hbox {$^{\prime \prime }$ }$ ( $r_{{\rm plat}}$ , dashed line). The total measured flux in this aperture and band is $F_{{\rm plat}} = 9.4 \pm 0.5 \times 10^{-13}$ erg s^-1 cm^-2 (horizontal dot-dashed level). We omitted the use of the pn and MOS1 camera for the growth curve analysis (see Sect. 2.2).

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$\begin{figure} \par\includegraphics[width=9cm,clip]{14434f3a.ps} \end{figure}$

Figure A.2:

The growth curve of SPT-CL J2342-5411: red curve shows the integrated flux as a function of outer integration radius for the joint MOS1 and MOS2 cameras (0.5-2.0 keV band), blue curve for the pn camera. Error bars on the growth curve indicate the Poisson error of the flux measurement including a 5% systematic error in the background estimation. Source flux is detected out to $r_{{\rm plat}}=62\hbox {$^{\prime \prime }$ }$ (dashed line). The total measured flux, estimated as the weighted average of the MOS and pn plateau fluxes, is $F_{{\rm plat}} = 5.7 \pm 0.6 \times 10^{-14}$ erg s^-1 cm^-2 (dot-dashed level).

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The Appendix provides additional information concerning the X-ray analysis of SPT-CL J2332-5358 and SPT-CL J2342-5411.

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Figure A.3:

XMM-Newton X-ray spectrum of SPT-CL J2332-5358 fitted with a single temperature MEKAL model which gives T =9.3^+3.3_-1.9 keV. The column density is fixed to the galactic value $n_{{\rm H}} = 1.62 \times 10^{20}$ cm^-2 (Dickey & Lockman 1990), the metal abundance to $Z=0.3~Z_{\hbox{$\odot$ }}$ and the redshift to z =0.32 (photometric). The spectra were binned only for display purposes, the fit was carried out with $\ge$ 1 cts/bin binning and C-statistic. Red: MOS1, black: MOS2, green: pn. See Sect. 2.2.1 for details.

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$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{14434f5a.ps} \end{figure}$

Figure A.4:

XMM-Newton X-ray spectrum of SPT-CL J2342-5411. The available low-count spectrum (displayed for completeness) allows us to draw only tentative conclusions. The spectrum is consistent with a single temperature MEKAL model, with the temperature only weakly constrained to T =6.7^+5.2_-2.4 keV. The column density is fixed to the galactic value $n_{{\rm H}} = 1.86 \times 10^{20}$ cm^-2 (Dickey & Lockman 1990), the metal abundance to $Z=0.3~Z_{\hbox{$\odot$ }}$ and the redshift to z =1.08 (photometric). The spectra were binned only for display purposes, the fit was carried out with $\ge$ 1 cts/bin binning and C-statistic. Red: MOS1, black: MOS2, green: pn. See Sect. 2.2.1 for details.

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$\begin{figure} \par\includegraphics[width=9cm,clip]{14434f6a.eps}\includegraphics[width=9cm,clip]{14434f6b.eps} \end{figure}$

Figure A.5:

Left: color image of SPT-CL J2332-5358 (photo-z = 0.32). Right: color image of SPT-CL J2342-5411 (photo-z=1.08). Both images were obtained from the Blanco Cosmology Survey imaging in the gri bands. X-ray contours are overlaid in white. Green circles show the estimated r $_{{\rm plat}}$ (see Sect. 2.2). Both clusters have a large BCG (brightest cluster galaxy) within few arcseconds ( ${\lesssim }10\hbox {$^{\prime \prime }$ }$ ) from the X-ray emission peak.

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