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Home All issues Volume 519 (September 2010) A&A, 519 (2010) A40 Online Material
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Issue
A&A
Volume 519, September 2010
Article Number A40
Number of page(s) 31
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361/200913774
Published online 09 September 2010

Online Material

Table 2:   Observed emission line fluxes in units of ${\rm 10^{-16}~erg~s^{-1}~cm^{-2}\hbox{$^{\prime\prime}$ }^{-2}}$.

Table 3:   Observed emission line equivalent widths.

Appendix A: Short description of morphological and kinematic characteristics and peculiarities of the galaxy sample (Paper I+Paper II)

We collect in Table A1 the morphological and kinematic characteristics, as well as the peculiarities, of the complete R05+A06 sample. The morphological and kinematic properties in Table A1 are derived from the literature, and were in part already described in the Appendix (provided as on-line material) of Paper I and Paper II.

We list in Cols. 3 and 4 the galaxy ellipticity, $\epsilon$, and the ($V/\sigma$) $_{\rm scaled}$. The latter is computed from slit spectroscopy measurements through the relation provided by Cappellari et al. (2007), ($V/\sigma$) $_{\rm scaled}= 0.57 \times$(V/ $\sigma)_{\rm slit}$. It should be a reasonable approximation of the ($V/\sigma$)$_{\rm e}$, computed on a luminosity weighted spectrum within $r_{\rm e}$. For the eight galaxies in common with the SAURON sample, i.e. NGC 2974, NGC 3489, NGC 4374, NGC 4552, NGC 5813, NGC 5831, NGC 5846 and NGC 7332, the $\epsilon$ and $V/\sigma$values are those derived through integral field spectroscopy. Cappellari et al. (2007) noticed that there is a good agreement between $\epsilon$ values derived in the literature with different methods.

Emsellem et al. (2007) defined a new parameter, $\lambda_R = \langle R\vert V\vert\rangle/\langle R \sqrt{V^2 + \sigma^2}\rangle$, where R is the galacto-centric distance, and V and $\sigma $ are luminosity weighted averages over the two-dimensional kinematic field. This parameter is a proxy to quantify the observed projected stellar angular momentum per unit mass, and can be used to classify ETGs into slow or fast rotators. In the $\epsilon$ vs. ($V/\sigma$)$_{\rm e}$ plane, Cappellari et al. (2007) identified a region (0.0 $ \lesssim \epsilon \lesssim 0.3$, $0.0\lesssim (V/\sigma)_{\rm e} \lesssim$0.13) where slow- rotators are generally found. Lacking the 2D V and $\sigma $ information for most of our galaxies, we used ($V/\sigma$) $_{\rm scaled}$ to identify in the $\epsilon$ vs. ($V/\sigma$)$_{\rm e}$ plane the fast and slow rotators. The derived classification is provided in Col. 5 of Table A1 (F = fast rotator; S = slow rotator). We obtain that $\approx$68% (36/53) of our sample is fast rotator (to be compared with 75% fast rotators in the SAURON sample). Less than 1/3 of our galaxies are slow rotators (vs. 25% in the SAURON sample).

In Cols. 6 and 7 of Table A1 we provide the kinematic and morphological peculiarities, respectively. A large fraction, approximately 50% of our ETGs, displays kinematic peculiarities, like counter-rotation, or peculiar faint features, like shells, tails, or decoupled gas distributions with respect to the stars.

Table A.1:   Kinematic and morphological overview.

Appendix B: Emission line ratios for the total sample in annuli of increasing galacto-centric distance

\begin{figure} \par\includegraphics[width=16.4cm,clip]{annibali.fig20.eps} \end{figure} Figure B.1:

${\rm \log [NII]/H\alpha}$ ratio for the sample in the annuli $r \leq r_{\rm e}$/16, $r_{\rm e}$/ $16 < r \leq r_{\rm e}$/8, re/ $8 < r \leq r_{\rm e}$/4, and $r_{\rm e}$/ $4 < r \leq r_{\rm e}$/2.

Open with DEXTER

\begin{figure} \par\includegraphics[width=16.4cm,clip]{annibali.fig21.eps} \end{figure} Figure B.2:

${\rm \log [NII]/H\alpha}$ ratio for the sample in the annuli $r \leq r_{\rm e}$/16, $r_{\rm e}$/ $16 < r \leq r_{\rm e}$/8, $r_{\rm e}$/ $8 < r \leq r_{\rm e}$/4, and $r_{\rm e}$/ $4 < r \leq r_{\rm e}$/2.

Open with DEXTER

\begin{figure} \par\includegraphics[width=16.4cm,clip]{annibali.fig22.eps} \end{figure} Figure B.3:

${\rm \log [OIII]/H\beta}$ ratio for the sample in the annuli $r \leq r_{\rm e}$/16, $r_{\rm e}$/ $16 < r \leq r_{\rm e}$/8, $r _{\rm e} /8 < r \leq r_{\rm e}$/4, and $r_{\rm e}$/ $4 < r \leq r_{\rm e}$/2.

Open with DEXTER

\begin{figure} \par\includegraphics[width=16.4cm,clip]{annibali.fig23.eps} \end{figure} Figure B.4:

${\rm \log [OIII]/H\beta}$ ratio for the sample in the annuli $r \leq r_{\rm e}$/16, $r_{\rm e}$/ $16 < r \leq r_{\rm e}$/8, $r _{e}/8 < r \leq r _{\rm e}$/4, and $r_{\rm e}$/ $4 < r \leq r_{\rm e}$/2.

Open with DEXTER

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