Investigating the relationship between AGN activity and stellar mass in zCOSMOS galaxies at 0 < z < 1 using emission-line diagnostic diagrams

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Volume 556 (August 2013)

A&A, 556 (2013) A11

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Issue		A&A Volume 556, August 2013


Article Number		A11
Number of page(s)		20
Section		Extragalactic astronomy
DOI		https://doi.org/10.1051/0004-6361/201220258
Published online		17 July 2013

Online material

Appendix A

Here we present the zCOSMOS stacked spectra that were in our study.

Fig. A.1

Stacked zCOSMOS spectra at lower z. Bin 9.25 ≤ log M_∗/M_⊙ < 9.5, 0.177 ≤ z < 0.242 (panel a)); 9.5 ≤ log M_∗/M_⊙ < 9.75, 0.177 ≤ z < 0.242 (panel b)); 9.75 ≤ log M_∗/M_⊙ < 10, 0.177 ≤ z < 0.242 (panel c)); 10 ≤ log M_∗/M_⊙ < 10.25, 0.177 ≤ z < 0.242 (panel d)); 10.25 ≤ log M_∗/M_⊙ < 10.5, 0.177 ≤ z < 0.242 (panel e)); 10.5 ≤ log M_∗/M_⊙ < 10.75, 0.177 ≤ z < 0.242 (panel f)); 10.75 ≤ log M_∗/M_⊙ < 11, 0.177 ≤ z < 0.242 (panel g)); 9 ≤ log M_∗/M_⊙ < 9.25, 0.242 ≤ z < 0.306 (panel h)); 9.25 ≤ log M_∗/M_⊙ < 9.5, 0.242 ≤ z < 0.306 (panel i)); 9.5 ≤ log M_∗/M_⊙ < 9.75, 0.242 ≤ z < 0.306 (panel j)); 9.75 ≤ log M_∗/M_⊙ < 10, 0.242 ≤ z < 0.306 (panel k)); 10 ≤ log M_∗/M_⊙ < 10.25, 0.242 ≤ z < 0.306 (panel l)); 10.25 ≤ log M_∗/M_⊙ < 10.5, 0.242 ≤ z < 0.306 (panel m)); 10.5 ≤ log M_∗/M_⊙ < 10.75, 0.242 ≤ z < 0.306 (panel n)); 10.75 ≤ log M_∗/M_⊙ < 11, 0.242 ≤ z < 0.306 (panel o)); 11 ≤ log M_∗/M_⊙ < 11.25, 0.242 ≤ z < 0.306 (panel p)); 9.25 ≤ log M_∗/M_⊙ < 9.5, 0.306 ≤ z < 0.371 (panel q)); 9.5 ≤ log M_∗/M_⊙ < 9.75, 0.306 ≤ z < 0.371 (panel r)); 9.75 ≤ log M_∗/M_⊙ < 10, 0.306 ≤ z < 0.371 (panel s)); 10 ≤ log M_∗/M_⊙ < 10.25, 0.306 ≤ z < 0.371 (panel t)); 10.25 ≤ log M_∗/M_⊙ < 10.5, 0.306 ≤ z < 0.371 (panel u)); 10.5 ≤ log M_∗/M_⊙ < 10.75, 0.306 ≤ z < 0.371 (panel v)); 10.75 ≤ log M_∗/M_⊙ < 11, 0.306 ≤ z < 0.371 (panel w)); 11 ≤ log M_∗/M_⊙ < 11.25, 0.306 ≤ z < 0.371 (panel x)); 9.25 ≤ log M_∗/M_⊙ < 9.5, 0.371 ≤ z ≤ 0.436 (panel y)); 9.5 ≤ log M_∗/M_⊙ < 9.75, 0.371 ≤ z ≤ 0.436 (panel z)); 9.5 ≤ log M_∗/M_⊙ < 9.75, 0.371 ≤ z ≤ 0.436 (panel a2)); 9.75 ≤ log M_∗/M_⊙ < 10, 0.371 ≤ z ≤ 0.436 (panel b2))); 10 ≤ log M_∗/M_⊙ < 10.25, 0.371 ≤ z ≤ 0.436 (panel c2)); 10.25 ≤ log M_∗/M_⊙ < 10.5, 0.371 ≤ z ≤ 0.436 (panel d2)); 10.5 ≤ log M_∗/M_⊙ < 10.75, 0.371 ≤ z ≤ 0.436 (panel e2)); 10.75 ≤ log M_∗/M_⊙ < 11, 0.371 ≤ z ≤ 0.436 (panel f2)); 11 ≤ log M_∗/M_⊙ < 11.25, 0.371 ≤ z ≤ 0.436 (panel g2)).

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	Fig. A.1 continued.
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Fig. A.2

Stacked zCOSMOS spectra at higher z. Bin 9.5 ≤ log M_∗/M_⊙ < 9.75, 0.548 ≤ z < 0.632 (panel a)); 9.75 ≤ log M_∗/M_⊙ < 10, 0.548 ≤ z < 0.632 (panel b)); 10 ≤ log M_∗/M_⊙ < 10.25, 0.548 ≤ z < 0.632 (panel c)); 10.25 ≤ log M_∗/M_⊙ < 10.5, 0.548 ≤ z < 0.632 (panel d)); 10.5 ≤ log M_∗/M_⊙ < 10.75, 0.548 ≤ z < 0.632 (panel e)); 10.75 ≤ log M_∗/M_⊙ < 11, 0.548 ≤ z < 0.632 (panel f)); 11 ≤ log M_∗/M_⊙ < 11.25, 0.548 ≤ z < 0.632 (panel g)); 9.5 ≤ log M_∗/M_⊙ < 9.75, 0.632 ≤ z < 0.716 (panel h)); 9.75 ≤ log M_∗/M_⊙ < 10, 0.632 ≤ z < 0.716 (panel i)); 10 ≤ log M_∗/M_⊙ < 10.25, 0.632 ≤ z < 0.716 (panel j)); 10.25 ≤ log M_∗/M_⊙ < 10.5, 0.632 ≤ z < 0.716 (panel k)); 10.5 ≤ log M_∗/M_⊙ < 10.75, 0.632 ≤ z < 0.716 (panel l)); 10.75 ≤ log M_∗/M_⊙ < 11, 0.632 ≤ z < 0.716 (panel m)); 11 ≤ log M_∗/M_⊙ < 11.25, 0.632 ≤ z < 0.716 (panel n)); 9.5 ≤ log M_∗/M_⊙ < 9.75, 0.716 ≤ z < 0.08 (panel o)); 9.75 ≤ log M_∗/M_⊙ < 10, 0.716 ≤ z < 0.08 (panel p)); 10 ≤ log M_∗/M_⊙ < 10.25, 0.716 ≤ z < 0.08 (panel q)); 10.25 ≤ log M_∗/M_⊙ < 10.5, 0.716 ≤ z < 0.08 (panel r)); 10.5 ≤ log M_∗/M_⊙ < 10.75, 0.716 ≤ z < 0.08 (panel s)); 10.75 ≤ log M_∗/M_⊙ < 11, 0.716 ≤ z < 0.08 (panel t)); 11 ≤ log M_∗/M_⊙ < 11.25, 0.716 ≤ z < 0.08 (panel u)); 9.5 ≤ log M_∗/M_⊙ < 9.75, 0.8 ≤ z ≤ 0.884 (panel v)); 9.75 ≤ log M_∗/M_⊙ < 10, 0.8 ≤ z ≤ 0.884 (panel w)); 10 ≤ log M_∗/M_⊙ < 10.25, 0.8 ≤ z ≤ 0.884 (panel x)); 10.25 ≤ log M_∗/M_⊙ < 10.5, 0.8 ≤ z ≤ 0.884 (panel y)); 10.5 ≤ log M_∗/M_⊙ < 10.75, 0.8 ≤ z ≤ 0.884 (panel z)); 10.75 ≤ log M_∗/M_⊙ < 11, 0.8 ≤ z ≤ 0.884 (panel a2)); 11 ≤ log M_∗/M_⊙ < 11.25, 0.8 ≤ z ≤ 0.884 (panel b2)).

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	Fig. A.2 continued.
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For a fixed redshift, the stacked spectra – before stellar continuum subtraction – show a [OIII] line whose strength decreases with the progressive increase of the stellar mass (Fig. A.1), especially if compared with the Hβ line. The latter shows a weakening as well. The Hα line is very strong at low masses. The intensity of the [NII] and Hα decreases up to the point at the highest mass bin where these lines show the same intensity. In Fig. A.2, the [OIII] and Hβ lines show the same trend as at lower redshifts. The [OII] line intensity decreases with the increase of the mass, but it is always the strongest line in the high-redshift composite spectra.

Appendix B

We used the dust-corrected flux ratios for [OII]/Hβ instead of the EW ratios originally used by Lamareille (2010).

This appendix (Fig. B.1) shows that the dust-corrected fluxes correspond well enough to the EWs for a sample of SDSS galaxies (Vitale et al. 2012), especially in the regions occupied by our sample. Hence we can use the original demarcation lines from Lamareille (2010). However, the dust-corrected flux ratios span a slightly more restricted range of [OIII]/Hβ values than the EW ratios.

	Fig. B.1 [OII] diagnostic diagram showing the consistency between EW measurements (left panel) and dust-corrected fluxes (right panel). The solid demarcation lines are taken from Lamareille (2010). The gray distribution represents the SDSS galaxies from Vitale et al. (2012).
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© ESO, 2013

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