Free Access
Issue
A&A
Volume 524, December 2010
Article Number A33
Number of page(s) 20
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361/201015504
Published online 22 November 2010

Online material

Appendix A: Spectra and best fit-templates

In Fig. A, we present our spectra and the best-fit templates among the 21 templates described in Sect. 4.1 using the method described in Bertincourt et al. (2009). We also plot the 24 μm flux densities from the SWIRE catalogue and the values determined from the IRS spectra convolved with the MIPS 24 μm filter.

thumbnail Fig. A.1

IRS spectra of our sources. The black line is our data. In shaded grey, we plot the 1σ deviation. The green short-dashed line is the best-fit PAH template from Smith et al. (2007). The red diamond is the 24 μm flux density from the SWIRE catalogue. The red square is the 24 μm flux density extracted from the spectrum with the 24 μm filter profile. The pink shape shows the region where the transmission of the 24 μm is maximum. All these spectra are plotted in observed wavelength. The templates are scaled to the “(1 + z) × 7.7   μm” flux. The source ID, the names of the best-fit templates, and zPAH are reported in each panel.

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Appendix B: Spectral decomposition of the spectra

In Fig. B, we present the decompositions of our spectra made with the PAHFIT code developed by Smith et al. (2007).

thumbnail Fig. B.1

Decompositions of the spectra of our sources. The solid green line is the fitted model. The blue lines above the continuum are the PAH features. The violet lines are the spectral lines. The thin grey lines represent the thermal dust continuum components. The thick red line shows the total continuum (stars+dust). The dotted black line shows the extinction (eτλ,  = 1 if no extinction). The source ID is reported as the title of each panel.

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© ESO, 2010

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