Stellar population gradients in galaxy discs from the CALIFA survey - The influence of bars

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Volume 570 (October 2014)

A&A, 570 (2014) A6

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Issue		A&A Volume 570, October 2014


Article Number		A6
Number of page(s)		85
Section		Extragalactic astronomy
DOI		https://doi.org/10.1051/0004-6361/201423635
Published online		06 October 2014

Online material

Table 1

Main characteristics of the sample.

Table 2

Luminosity- and mass-weighted log(age) and metallicity gradient calculated as the slope of a linear fit of the form a + blog (r/r_eff for our sample of galaxies.

Table 3

Luminosity- and mass-weighted log(age) and metallicity gradient calculated as the difference of the metallicity and age between 1.5 r_eff and r_disc0.

Appendix A: Derivation of the age-metallicity relation

One of the advantages of deriving star formation histories with STECKMAP is that, in principle, one can also derive the metallicity of the stellar population with different ages. However, due to the existent degeneracies in the determination of these parameters, one has to test if this is really possible. In Sánchez-Blázquez et al. (2011) – see their Appendix B – we already probed that we were able to recover the evolution of metallicity with time for the data with a similar S/N, resolution and wavelength coverage than that used in paper. In this appendix we repeat the test but using synthetic data with the characteristics of the CALIFA spectra. We have generated synthetic spectra for an exponentially declining star formation history e^{(− t/τ)} with different values of τ, τ = 1, 5, 10 and 20 Gyr and with two different chemical evolution, one with constant metallicity and one where the metallicity increase with age with the law Z = 0.2 − (age (Gyr) − 1.0)/(16.0).

We have used the models of V10 broadened to 150 km s^-1 and we have added noise to simulate a spectrum of S/N = 40. We then run STECKMAP on these spectra. Figure A.1 shows the simulated and the recovered age metallicity relation for the different synthetic spectra. The error bars in the figure are computed as the rms dispersion of the values obtained in 50 MonteCarlo simulations in which each pixel of the synthetic spectrum was modified randomly following a Gaussian distribution with a width given by the noise spectrum. As can be seen, although at all ages the metallicity is not very well constrained (the scatter from the different simulations is large), we can recover the age-metallicity relation in the synthetic spectra.

Fig. A.1

Age metallicity relation for a simulated exponential star formation history with different τ and with two different chemical evolution models. Solid lines indicate the simulated age-metallicity relation whilst the points show the recovered values. Open symbols shows the recovered age-metallicity relation in the case of constant metallicity with age whilst the filled symbols show the recovered age-metallicity relation in the case where the metallicity increase with time. Error bars represent the rms dispersion of a set of 50 Monte Carlo simulations where each pixel is moved according to a Gaussian distribution of width given by the errors. The synthetic spectra have been degraded to the resolution of the data and noise have been added to simulate a S/N per Å of 40.

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Appendix B: Age gradients

Figure B.1 shows the age gradients for our sample of galaxies.

	Fig. B.1 Mean luminosity- (light red) and mass- (dark red) age as a function of radius, normalised to the effective radius of the disc. Shaded area indicate the radial range of the surface brightness profile dominated by the bulge. The dashed line shows the bar length measured as indicated in the text. Solid lines shows the linear fit performed on the disc region.
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	Fig. B.2 Age gradients of the sample of unbarred galaxies.
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	Fig. B.3 Age gradients of the sample of weakly barred galaxies.
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Appendix C: Metallicity gradients

Figure C.1 shows the metallicity gradients for our sample of galaxies.

	Fig. C.1 Luminosity- (light red) and mass- (dark red) metallicity gradients for our sample of barred galaxies.
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	Fig. C.2 Luminosity- (light red) and mass- (dark red) metallicity gradients for our sample of barred galaxies.
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	Fig. C.3 Light- (light yellow) and mass-weighted (dark yellow) metallicity gradient for the galaxies morphologically classified as weakly barred.
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	Fig. C.4 Mean log(age) and metallicity maps for IC 1256.
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	Fig. C.5 Mean log(age) and metallicity maps for IC1683.
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	Fig. C.6 Mean log(age) and metallicity maps for NGC 0001.
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	Fig. C.7 Mean log(age) and metallicity maps for NGC 0036.
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	Fig. C.8 Mean log(age) and metallicity maps for NGC 0160.
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	Fig. C.9 Mean log(age) and metallicity maps for NGC 0214.
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	Fig. C.10 Mean log(age) and metallicity maps for NGC 0234.
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	Fig. C.11 Mean log(age) and metallicity maps for NGC 0257.
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	Fig. C.12 Mean log(age) and metallicity maps for NGC 0776.
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	Fig. C.13 Mean log(age) and metallicity maps for NGC 1167.
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	Fig. C.14 Mean log(age) and metallicity maps for NGC 1645.
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	Fig. C.15 Mean log(age) and metallicity maps for NGC 2253.
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	Fig. C.16 Mean log(age) and metallicity maps for NGC 2347.
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	Fig. C.17 Mean log(age) and metallicity maps for NGC 2906.
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	Fig. C.18 Mean log(age) and metallicity maps for NGC 2916.
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	Fig. C.19 Mean log(age) and metallicity maps for NGC 3106.
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	Fig. C.20 Mean log(age) and metallicity maps for NGC 3300.
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	Fig. C.21 Mean log(age) and metallicity maps for NGC 3614.
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	Fig. C.22 Mean log(age) and metallicity maps for NGC 3687.
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	Fig. C.23 Mean log(age) and metallicity maps for NGC 4047.
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	Fig. C.24 Mean log(age) and metallicity maps for NGC 4185.
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	Fig. C.25 Mean log(age) and metallicity maps for NGC 4210.
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	Fig. C.26 Mean log(age) and metallicity maps for NGC 4470.
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	Fig. C.27 Mean log(age) and metallicity maps for NGC 5000.
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	Fig. C.28 Mean log(age) and metallicity maps for NGC 5016.
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	Fig. C.29 Mean log(age) and metallicity maps for NGC 5205.
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	Fig. C.30 Mean log(age) and metallicity maps for NGC 5218.
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	Fig. C.31 Mean log(age) and metallicity maps for NGC 5378.
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	Fig. C.32 Mean log(age) and metallicity maps for NGC 5394.
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	Fig. C.33 Mean log(age) and metallicity maps for NGC 5406.
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	Fig. C.34 Mean log(age) and metallicity maps for NGC 5614.
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	Fig. C.35 Mean log(age) and metallicity maps for NGC 5633.
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	Fig. C.36 Mean log(age) and metallicity maps for NGC 5720.
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	Fig. C.37 Mean log(age) and metallicity maps for NGC 5732.
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	Fig. C.38 Mean log(age) and metallicity maps for NGC 5784.
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	Fig. C.39 Mean log(age) and metallicity maps for NGC 6004.
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	Fig. C.40 Mean log(age) and metallicity maps for NGC 6063.
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	Fig. C.41 Mean log(age) and metallicity maps for NGC 6154.
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	Fig. C.42 Mean log(age) and metallicity maps for NGC 6155.
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	Fig. C.43 Mean log(age) and metallicity maps for NGC 6301.
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	Fig. C.44 Mean log(age) and metallicity maps for NGC 6497.
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	Fig. C.45 Mean log(age) and metallicity maps for NGC 6941.
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	Fig. C.46 Mean log(age) and metallicity maps for NGC 7025.
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	Fig. C.47 Mean log(age) and metallicity maps for NGC 7321.
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	Fig. C.48 Mean log(age) and metallicity maps for NGC 7489.
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	Fig. C.49 Mean log(age) and metallicity maps for NGC 7549.
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	Fig. C.50 Mean log(age) and metallicity maps for NGC 7563.
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	Fig. C.51 Mean log(age) and metallicity maps for NGC 7591.
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	Fig. C.52 Mean log(age) and metallicity maps for NGC 7653.
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	Fig. C.53 Mean log(age) and metallicity maps for NGC 7671.
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	Fig. C.54 Mean log(age) and metallicity maps for NGC 7782.
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	Fig. C.55 Mean log(age) and metallicity maps for UGC 00005.
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	Fig. C.56 Mean log(age) and metallicity maps for UGC 00036.
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	Fig. C.57 Mean log(age) and metallicity maps for UGC 03253.
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	Fig. C.58 Mean log(age) and metallicity maps for UGC 07012.
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	Fig. C.59 Mean log(age) and metallicity maps for UGC 08234.
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	Fig. C.60 Mean log(age) and metallicity maps for UGC 10205.
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	Fig. C.61 Mean log(age) and metallicity maps for UGC 11649.
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	Fig. C.62 Mean log(age) and metallicity maps for UGC 11680.
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	Fig. C.63 Mean log(age) and metallicity maps for UGC 12224.
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	Fig. C.64 Mean log(age) and metallicity maps for UGC 12816.
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© ESO, 2014

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