EDP Sciences
Free Access
Issue
A&A
Volume 582, October 2015
Article Number A97
Number of page(s) 26
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361/201423838
Published online 15 October 2015

Online material

Appendix A: Zoom in to individual bands

In this section, we present the spectral energy distribution of our single stellar population models over the J, H and K-bands. Figures A.1 to A.3 present the SEDs at solar metallicity and different ages. Figures A.4 to A.6 present the SEDs at solar metallicity and different ages.

thumbnail Fig. A.1

Same as Fig. 7 except over the J-band (1.041.44 μm).

Open with DEXTER

thumbnail Fig. A.2

Same as Fig. 7 expect over the H-band (1.461.84 μm).

Open with DEXTER

thumbnail Fig. A.3

Same as Fig. 7 expect over the K-band (1.902.48 μm).

Open with DEXTER

thumbnail Fig. A.4

Same as Fig. 8 expect over the J-band (1.041.44 μm).

Open with DEXTER

thumbnail Fig. A.5

Same as Fig. 8 expect over the H-band (1.461.84 μm).

Open with DEXTER

thumbnail Fig. A.6

Same as Fig. 8 expect over the K-band (1.902.48 μm).

Open with DEXTER

Appendix B: Integrated colours and line-strength indices from our models

These are the integrated colours and the line strength indices from the spectral energy distributions of the our single stellar population. The SEDs were convolved to a velocity dispersion of 350 km s-1 before calculating indices.

Table B.1

Integrated colours and abundances for the MarS models as a function of age and metallicity.

Table B.2

Integrated colours and abundances for the GirS models as a function of age and metallicity.

Table B.3

Integrated colours and abundances for the BaSS models as a function of age and metallicity.


© ESO, 2015

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