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<!-- DOI: 10.1051/0004-6361/200911995 -->

<h2 class="sec">Online Material</h2>

<h2 class="sec"><a name="SECTION00090000000000000000"></a>
Appendix A: Properties of individual galaxies
</h2>
<A NAME="individual"></A>
<p>
In this appendix, we present the morphological, kinematical and dynamical properties for each galaxy derived from
<I>I</I>-band images, H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
flux maps, radial velocity maps, velocity dispersion maps and their associated error maps (Figs.&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#map1">A.1</a> to&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#map9">A.9</a>). On each velocity map, the kinematical center used for the kinematical analysis is plotted with a black and white double cross.
The kinematical position angle is also displayed and ends at half light radius <I>r</I><SUB>1/2</SUB> (Table&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#table_mass">5</a>). The flux contours are overplotted on both velocity fields and velocity dispersion maps. In all figures, North is up and East is to the left. The kinematical parameters and the masses are given in Tables&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#table_kin">4</a> and&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#table_mass">5</a>.
In error maps, pixels with values out of the scale range are displayed in white.<br>

<p>
<div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="map1">&#160;</A><!-- end Label--><A NAME="3287"></A><A NAME="figure2887"
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<td class="img-txt"><span class="bold">Figure A.1:</span><p>
VVDS020116027 maps. <I> From left to right</I>: <I>I</I>-band CFHT legacy survey best seeing image, H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
flux (<I> top</I>) and signal to noise ratio (<I> bottom</I>) maps, H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
velocity field (<I> top</I>) and associated errors (<I> bottom</I>), H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
velocity dispersion map and associated errors (<I> bottom</I>) obtained from Gaussian fits to the SINFONI data cubes after smoothing spatially with a two-dimensional Gaussian of 
<!-- MATH: ${\it FWHM} = 2$ -->
<IMG
 WIDTH="69" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img12.png"
 ALT="${\it FWHM} = 2$">
pixels. Except for the instrumental spectral PSF, no correction has been applied to compute the velocity dispersion map. Kinematical maps have been masked using the following criteria: (i)&nbsp;the line width must be larger than the one of the spectral PSF (the majority white pixels in the velocity dispersion error map), (ii) the uncertainty on the velocity must be less than 30&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">
and (iii) the signal to noise ratio larger than <IMG
 WIDTH="12" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img14.png"
 ALT="$\sim $">2. The <I>I</I>-band image and H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
maps are color-coded with a linear scaling such that the values increase from light to dark. The integrated H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
flux is quoted in each H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
flux map in 10<sup>-17</sup>&nbsp;ergs&nbsp;s<sup>-1</sup>&nbsp;cm<sup>-2</sup>. In error maps, values larger than the scale maximum are displayed using white.
The angular size is indicated and the final seeing <I> FWHM</I> (including observational seeing and Gaussian smoothing) is plotted as a circle on the velocity field.
North is up, East is left. The center used for kinematical analysis is marked on each kinematical map with a black and white double cross. The solid line represents the orientation of the kinematical major axis and ends at the half light radius measured on <I>I</I>-band images. The flux contours are overplotted on the velocity field, the velocity dispersion map and their associated error maps. The redshift derived from SINFONI data and the dynamical classification are quoted (RD for rotating disks, PR for perturbed rotators, MS for merging systems).</p></td>
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<table>
<tr><td><!-- init Label --><A NAME="map2">&#160;</A><!-- end Label--><A NAME="3289"></A><A NAME="figure2903"
 HREF="img237.png"><IMG
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<td class="img-txt"><span class="bold">Figure A.2:</span><p>
Same as Fig.&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#map1">A.1</a> for VVDS020182331. The signal to noise ratio threshold for this galaxy has been set to 1.5.</p></td>
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</table></div>
<p>
<B>VVDS020116027.</B>
This galaxy shows a faint and irregular velocity gradient. The H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
flux map, the velocity field and the velocity dispersion map suggest
two components separated by about 6&nbsp;kpc (0.75
<!-- MATH: $^{\prime\prime}$ -->
<IMG
 WIDTH="11" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img17.png"
 ALT="$^{\prime\prime}$">). Indeed, the velocities decrease from South to North accross the main component but decrease by around 15&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">
when reaching the faint component. The separation between the two components is characterized by a higher velocity dispersion that could indicate a merging event (<A NAME="aaref1"></A><a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#Amram:2007">Amram et&nbsp;al.  2007</a>) or an unresolved gap in velocity between the two components.
The velocity separation of the centers of these two components is close to 0&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">.
The merging timescale would be around 0.4&nbsp;Gyr (from <A NAME="aaref40"></A><a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#Kitzbichler:2008">Kitzbichler &amp; White  2008</a>). The faint component is not seen in the <I>I</I>-band CFHTLS image, but the system appears as distorted and elongated, leading to an inclination of the whole system of 50<IMG
 WIDTH="9" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img11.png"
 ALT="$^\circ $">.
The very low maximum rotation velocity (50&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">)
may indicate that the object is almost not rotating (
<!-- MATH: $V_{\rm max}/\sigma_0=1.1$ -->
<IMG
 WIDTH="84" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img238.png"
 ALT="$V_{\rm max}/\sigma_0=1.1$">)
or that the main component is seen nearly face-on.
<div class="inset-old">
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<td class="img-txt"><span class="bold">Figure A.3:</span><p>
Same as Fig.&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#map1">A.1</a> for VVDS020147106.</p></td>
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 HREF="img240.png"><IMG
 WIDTH="187" HEIGHT="75" SRC="Timg240.png"
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\par\resizebox{17cm}{!}{\includegraphics{11995f21}}
\end{figure}"></A><!-- HTML Figure number: 17 --></td>
<td class="img-txt"><span class="bold">Figure A.4:</span><p>
Same as Fig.&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#map1">A.1</a> for VVDS020261328. The East feature in the signal to noise ratio map corresponds to a badly subtracted cosmic ray.</p></td>
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</table></div>Fitting a rotating disk model for this system has been attempted both with or without masking the northern component. In both cases, a low <IMG
 WIDTH="16" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img96.png"
 ALT="$\chi^2$">
is obtained but is due to the low velocities measured in this galaxy. The <IMG
 WIDTH="12" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img188.png"
 ALT="$\sigma$">-peak around 70&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">
located at 0.3
<!-- MATH: $^{\prime\prime}$ -->
<IMG
 WIDTH="11" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img17.png"
 ALT="$^{\prime\prime}$">
to the North-East of the maximum of the H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">&nbsp;flux is not accounted for by these models.
Due to both the low velocity dispersion and maximum rotation velocity, this object is one of the least massive of our sample (
<!-- MATH: $5.5\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="83" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img241.png"
 ALT="$5.5\times10^{10}~{M_\odot}$">).
This object is classified as a major merger, presumably in a premerging state since the <I>SFR</I>
<!-- MATH: $_{\rm H\alpha}$ -->
<IMG
 WIDTH="17" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img65.png"
 ALT="$_{{\rm H}\alpha}$">
is rather faint, indicating that the starburst event would not yet have been engaged.<br>

<p>
<B>VVDS020182331.</B>
The flux of this galaxy is mostly concentrated in the central parts. This galaxy shows a perturbed velocity field. A strong sky line residual (14605&nbsp;&#197;) perturbs the line measurements and is responsible for both northern velocity dispersion and line flux peaks observed towards the North.
The uncertainty on the velocity measurements is lower than 20&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">
for the central arcsecond only (in diameter). In this central part, a rotating disk model is acceptable. The corrected velocity dispersion of this object is high (71&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">). We do not detect in H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
the close-by object revealed in CFHTLS best seeing images, indicating that this object is a foreground or background galaxy or that it is a companion with no star formation with which VVDS020182331 may interact. The latter explanation could explain the perturbed rotation observed in VVDS020182331. This object is slightly more rotation supported than dispersion supported (
<!-- MATH: $V_{\rm max}/\sigma_0 = 1.9$ -->
<IMG
 WIDTH="84" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img242.png"
 ALT="$V_{\rm max}/\sigma_0 = 1.9$">)
and has a dynamical mass of 
<!-- MATH: $4.1\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="83" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img243.png"
 ALT="$4.1\times10^{10}~{M_\odot}$">.
It is classified as a perturbed rotator.<br>

<p>
<B>VVDS020147106.</B>
The H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
flux is concentrated in the center. The size of the galaxy is twice the seeing (see Table&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#runs">1</a>). This galaxy shows a faint velocity shear compatible with a face-on rotating disk. The velocity dispersion map does not show any peak but is higher on the eastern side (by about 20&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">). The northern edge shows higher velocities of about 30&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">.
However, the one pixel crown of the edges has higher uncertainties due to a low signal to noise ratio (lower than 4) and was masked to fit a rotating disk model. The fit indicates that a low velocity plateau (30&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">)
is reached close to the center. This low maximum rotation velocity suggests that the inclination of this system is even lower than suggested from the <I>I</I>-band image or that this object is strongly dispersion dominated (
<!-- MATH: $V_{\rm max}/\sigma_0 = 0.4$ -->
<IMG
 WIDTH="84" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img244.png"
 ALT="$V_{\rm max}/\sigma_0 = 0.4$">). Due to the compactness of this object (
<!-- MATH: $r_{1/2}=1.2$ -->
<I>r</I><SUB>1/2</SUB>=1.2 kpc) and compared to the total extent of H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
emission (
<!-- MATH: $R_{\rm last}=6.4$ -->
<IMG
 WIDTH="61" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img245.png"
 ALT="$R_{\rm last}=6.4$">
kpc), the dispersion mass is estimated to be 
<!-- MATH: $27.4\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="89" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img246.png"
 ALT="$27.4\times10^{10}~{M_\odot}$">,
which is 15 times larger than the stellar mass (
<!-- MATH: $1.7\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="83" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img247.png"
 ALT="$1.7\times10^{10}~{M_\odot}$">). This suggests that this star-forming galaxy is embedded in a large dark matter halo or that it contains a large amount of gas. Even if it cannot be excluded that this galaxy is a dispersion dominated spheroid
, this galaxy is classified as a perturbed rotating disk since it has a high velocity dispersion (80&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">)
and shows rotation in its perturbed velocity field. The asymmetries observed in the velocity maps could be accounted for by a minor merging event.<br>

<p>
<B>VVDS020261328.</B>
The H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
flux map is peaked and faintly extends toward the South. The velocity dispersion map has a peak around 120&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">
to the South-East. The velocity field shows a clear but irregular velocity shear of about 100&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">
that extends over 0.8
<!-- MATH: $^{\prime\prime}$ -->
<IMG
 WIDTH="11" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img17.png"
 ALT="$^{\prime\prime}$">
in radius. Fitting a rotating disk model suggests that only the central part of the galaxy is detected since the plateau is not reached. It also shows that the velocity dispersion peak cannot be explained by beam smearing effects. For the same reasons as VVDS020147106, VVDS020261328 has a dynamical mass (
<!-- MATH: $19.6\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="89" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img248.png"
 ALT="$19.6\times10^{10}~{M_\odot}$">)
30 times higher than the stellar mass (
<!-- MATH: $0.6\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="83" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img249.png"
 ALT="$0.6\times10^{10}~{M_\odot}$">), suggesting
that dark matter and cool gas dominate the gravitational potential of this galaxy. The SFR is the lowest of our sample (see Table&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#tablesfr">3</a>).
This galaxy is classified as a pertubed rotator that is mainly rotation supported (
<!-- MATH: $V_{\rm max}/\sigma_0 = 3.5$ -->
<IMG
 WIDTH="84" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img250.png"
 ALT="$V_{\rm max}/\sigma_0 = 3.5$">).<br>

<p>
<B>VVDS220596913.</B>
The H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
flux map shows two main components separated by 12.5&nbsp;kpc (1.5
<!-- MATH: $^{\prime\prime}$ -->
<IMG
 WIDTH="11" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img17.png"
 ALT="$^{\prime\prime}$">)
that are not clearly distinguished in the <I>I</I>-band image. The brigthest component is located on the western side and is composed of two peaks of equal intensity. The eastern component is much fainter. It has a smooth velocity gradient and two peaks in the velocity dispersion map (around 100&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">). One corresponds to the brightest H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
knot, and the other is more diffuse and corresponds to the transition region between the two components where the H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
emission is the faintest (signal to noise ratio around 4). The high velocity dispersion between the two components can be a signature of merging as for the Hickson compact group H31 (<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#Amram:2007">Amram et&nbsp;al.  2007</a>). The velocity shear of the faint component is misaligned by around 20<IMG
 WIDTH="9" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img11.png"
 ALT="$^\circ $">
with respect to the one of the bright component suggesting, as does the flux distribution, that this system is composed of two galaxies in the process of merging. The velocity separation of the two components is estimated to be <IMG
 WIDTH="12" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img14.png"
 ALT="$\sim $">150&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">.
The merging timescale would be around 1.2&nbsp;Gyr.
Although a large and unique rotating disk consituted by large clumps as seen in <A NAME="aaref9"></A><a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#Bournaud:2008">Bournaud et&nbsp;al. (2008)</a> cannot be excluded (leading to 
<!-- MATH: $V_{\rm max}/\sigma_0=2.3$ -->
<IMG
 WIDTH="85" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img251.png"
 ALT="$V_{\rm max}/\sigma_0=2.3$">), fitting the brightest component alone gives better results in terms of <IMG
 WIDTH="16" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img96.png"
 ALT="$\chi^2$">,
suggesting that the main component is rotating with a maximum velocity of around 200&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">.
We fixed the center between the two flux peaks of the main component, and used an inclination of 55<IMG
 WIDTH="9" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img11.png"
 ALT="$^\circ $">.
Assuming that both components have the same dimensions (half the whole system dimensions), we obtained a dynamical mass of around 
<!-- MATH: $8\pm2\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="94" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img252.png"
 ALT="$8\pm2\times10^{10}~{M_\odot}$">
(dominated by rotation) for the bright component and 
<!-- MATH: $4\pm2\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="95" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img253.png"
 ALT="$4\pm2\times10^{10}~{M_\odot}$">
(dominated by dispersion) for the faint one. This implies a total dynamical mass of <IMG
 WIDTH="12" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img14.png"
 ALT="$\sim $">
<!-- MATH: $12\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="79" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img254.png"
 ALT="$12\times10^{10}~{M_\odot}$">,
of the same order as the one computed considering a unique object (<IMG
 WIDTH="12" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img14.png"
 ALT="$\sim $">
<!-- MATH: $13\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="80" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img255.png"
 ALT="$13\times10^{10}~{M_\odot}$">).
This object is classified as a major merger system.<br>

<p>
<B>VVDS220584167.</B>
VVDS220584167 is the object that presents the most extended H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
map of the sample. It has an elongated peak in the velocity dispersion map close to the center. The observation is affected by a strong sky line residual (16195&nbsp;&#197;, see Fig.&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#profils2">8</a>) that induces large uncertainties on line measurements, mainly on the southern side.
The velocity field shows asymmetry and the galaxy presents a distorted morphology in the <I>I</I>-band image which makes possible the existence of a strong bar (see for comparison UGC 08937 in <a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#Epinat:2009">Epinat et&nbsp;al.  2009</a>). Moreover, the observed displacement between <I>I</I>-band and H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
morphologies suggests a violent star formation event compatible with the high SFR of this galaxy.
The velocity field is reasonably fit by a simple rotational disk model, and the central velocity dispersion peak is not accounted for by the model since it does not simulate the effect of a bar. VVDS220584167 is the most massive disk of the sample, with a dynamical mass of 
<!-- MATH: $21.1\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="89" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img256.png"
 ALT="$21.1\times10^{10}~{M_\odot}$">.
It is also the most rotation-dominated object (
<!-- MATH: $M_{\theta}/M_{\sigma}=18$ -->
<IMG
 WIDTH="77" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img257.png"
 ALT="$M_{\theta}/M_{\sigma}=18$">
and 
<!-- MATH: $V_{\rm max}/\sigma_0 = 5.9$ -->
<IMG
 WIDTH="84" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img258.png"
 ALT="$V_{\rm max}/\sigma_0 = 5.9$">).
Thus this galaxy is classified as a rotating disk with a bar. <br>
<div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="map5">&#160;</A><!-- end Label--><A NAME="3295"></A><A NAME="figure2964"
 HREF="img259.png"><IMG
 WIDTH="187" HEIGHT="75" SRC="Timg259.png"
 ALT="\begin{figure}
\par\resizebox{17cm}{!}{\includegraphics{11995f22}}
\end{figure}"></A><!-- HTML Figure number: 18 --></td>
<td class="img-txt"><span class="bold">Figure A.5:</span><p>
Same as Fig.&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#map1">A.1</a> for VVDS220596913. The North feature is compatible with sky line residuals. The <I>I</I>-band map is a CFH12K/CFHT image.</p></td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=18&DOI=10.1051/0004-6361/200911995" target="DEXTER">Open with DEXTER</a></td></tr>

</table></div><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="map6">&#160;</A><!-- end Label--><A NAME="3297"></A><A NAME="figure2972"
 HREF="img260.png"><IMG
 WIDTH="187" HEIGHT="75" SRC="Timg260.png"
 ALT="\begin{figure}
\par\resizebox{17cm}{!}{\includegraphics{11995f23}}
\end{figure}"></A><!-- HTML Figure number: 19 --></td>
<td class="img-txt"><span class="bold">Figure A.6:</span><p>
Same as Fig.&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#map5">A.5</a> for VVDS220584167. The North-West feature is compatible with sky line residuals.</p></td>
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<p>
<B>VVDS220544103.</B>
The H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
flux map of VVDS220544103 shows two peaks separated by around 6&nbsp;kpc (0.75
<!-- MATH: $^{\prime\prime}$ -->
<IMG
 WIDTH="11" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img17.png"
 ALT="$^{\prime\prime}$">). It also shows a distorted morphology both in the line flux map and in the <I>I</I>-band image. A faint velocity gradient (<IMG
 WIDTH="12" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img14.png"
 ALT="$\sim $">30&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">)
is observed toward the main northern peak, whereas a strong velocity gradient (<IMG
 WIDTH="12" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img14.png"
 ALT="$\sim $">120&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">)
is observed to the South of the fainter southern peak. The two gradients are in the same direction and the velocity field is continuous accross the whole object. The isovelocity contours are perpendicular to the distorted and elongated morphology. The strongest peaks in the velocity dispersion are located at the edges where the signal to noise ratio is low. Excluding these peaks, the velocity dispersion map shows an elongated peak close to the faint H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
flux peak.
Fitting a simple rotating disk model to the whole system leads to a ratio 
<!-- MATH: $V_{\rm max}/\sigma_0=2.1$ -->
<IMG
 WIDTH="85" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img261.png"
 ALT="$V_{\rm max}/\sigma_0=2.1$">.
However, this object is hard to fit with such a model and the dynamical mass estimates just give an indication of its total mass.
From our data, it is not possible to separate two components and compute mass estimates for both. We estimated the total dynamical mass as 
<!-- MATH: $10.3\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="89" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img262.png"
 ALT="$10.3\times10^{10}~{M_\odot}$">
using a unique rotating disk object hypothesis. However, one might guess that at least one component could be seen nearly face-on and thus have a higher maximum velocity and thus a higher total mass.
The velocity separation between the two components is around 40&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">.
The merging timescale for this system would be around 0.5&nbsp;Gyr. This object could be two or more galaxies in a merging process and is classified as a merging system.<br>
<div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="map7">&#160;</A><!-- end Label--><A NAME="3299"></A><A NAME="figure2983"
 HREF="img263.png"><IMG
 WIDTH="187" HEIGHT="75" SRC="Timg263.png"
 ALT="\begin{figure}
\par\resizebox{17cm}{!}{\includegraphics{11995f24}}
\end{figure}"></A><!-- HTML Figure number: 20 --></td>
<td class="img-txt"><span class="bold">Figure A.7:</span><p>
Same as Fig.&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#map5">A.5</a> for VVDS220544103.</p></td>
</tr><tr><td colspan="2"><a href="http://dexter.edpsciences.org/applet.php?pdf_id=20&DOI=10.1051/0004-6361/200911995" target="DEXTER">Open with DEXTER</a></td></tr>

</table></div><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="map8">&#160;</A><!-- end Label--><A NAME="3301"></A><A NAME="figure2991"
 HREF="img264.png"><IMG
 WIDTH="187" HEIGHT="75" SRC="Timg264.png"
 ALT="\begin{figure}
\par\resizebox{17cm}{!}{\includegraphics{11995f25}} %
\end{figure}"></A><!-- HTML Figure number: 21 --></td>
<td class="img-txt"><span class="bold">Figure A.8:</span><p>
Same as Fig.&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#map5">A.5</a> for VVDS220015726.</p></td>
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<p>
<B>VVDS220015726.</B>
The central regions give a clean signal, while the low signal regions are affected by sky residuals due to the proximity of two strong sky lines next to H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
(15053&nbsp;&#197; and 15056&nbsp;&#197;).
The H<IMG
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 SRC="img6.png"
 ALT="$\alpha $">
map is peaked at the center and it also has a peak at the same location in the velocity dispersion map (<IMG
 WIDTH="12" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img14.png"
 ALT="$\sim $">100&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">). The kinematical maps of this galaxy are well reproduced by the rotating disk model. In particular, this model shows that the central velocity dispersion is due to beam smearing effects (see Fig.&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#models">11</a>). The relatively high <IMG
 WIDTH="16" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img96.png"
 ALT="$\chi^2$">
value of the fit is only due to the fact that this object shows the highest velocities. VVDS220015726 is clearly dominated by rotation (
<!-- MATH: $V_{\rm max}/\sigma_0=8.5$ -->
<IMG
 WIDTH="85" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img265.png"
 ALT="$V_{\rm max}/\sigma_0=8.5$">)
since it is the fastest rotator of the sample (
<!-- MATH: $V_{\rm max}=323$ -->
<IMG
 WIDTH="66" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img266.png"
 ALT="$V_{\rm max}=323$">&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">)
but also the object with the lowest velocity dispersion (
<!-- MATH: $\sigma_0=38$ -->
<IMG
 WIDTH="49" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img267.png"
 ALT="$\sigma_0=38$">&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">). Its total dynamical mass (
<!-- MATH: $16.7\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="89" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img268.png"
 ALT="$16.7\times10^{10}~{M_\odot}$">)
is compatible within the error bars to its stellar mass (
<!-- MATH: $6.2\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="83" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img269.png"
 ALT="$6.2\times10^{10}~{M_\odot}$">). This indicates that the halo contribution is low in the central parts of this galaxy. This object is classified as a rotating disk.<br>
<div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="map9">&#160;</A><!-- end Label--><A NAME="3303"></A><A NAME="figure3005"
 HREF="img270.png"><IMG
 WIDTH="187" HEIGHT="75" SRC="Timg270.png"
 ALT="\begin{figure}
\par\resizebox{17cm}{!}{\includegraphics{11995f26}}
\end{figure}"></A><!-- HTML Figure number: 22 --></td>
<td class="img-txt"><span class="bold">Figure A.9:</span><p>
Same as Fig.&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#map5">A.5</a> for VVDS220014252.</p></td>
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<p>
<B>VVDS220014252.</B>
The H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
flux map of VVDS220014252 shows an elongated peak and diffuse emission in the outer parts, compatible with the <I>I</I>-band morphology. The peak does not perfectly match the center of external isophotes. The H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
flux map also suggests the presence of an arm on the western side.
The velocity field is the one of a rotating disk except in the eastern side where it shows unexpectedly high velocities.
A rotating disk model correctly fits the velocity field. The fit is better (smaller <IMG
 WIDTH="16" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img96.png"
 ALT="$\chi^2$">)
when the center does not match the H<IMG
 WIDTH="11" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img6.png"
 ALT="$\alpha $">
flux peak, but the center of external isophotes. Adopting an inclination of 56<IMG
 WIDTH="9" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img11.png"
 ALT="$^\circ $">,
the deprojected maximum rotation velocity is quite low (103&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">). The model shows that the maximum rotation velocity is reached close to the kinematical center.
The North-West side of the velocity field shows a bump and thus a small decrease.
Around this bump, profiles are broad and asymmetric. Broad profiles (more than 150&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">)
are also observed at the North-East edge, with a rather good signal to noise ratio (larger than 5). The velocity dispersion is not peaked at the center of the galaxy but is high everywhere. Moreover, the mean velocity dispersion of this galaxy is the highest of the whole sample (92&nbsp;
<!-- MATH: $\rm km~s^{-1}$ -->
<IMG
 WIDTH="42" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img25.png"
 ALT="$\rm km~s^{-1}$">). The model shows that the velocity dispersion is not due to beam smearing effects(see Fig.&nbsp;<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#models">11</a>).
The broad and asymmetric profiles suggests the possibility of having intrinsic double profiles that can be signatures of interactions (<a href="/articles/aa/full_html/2009/36/aa11995-09/aa11995-09.html#Amram:2007">Amram et&nbsp;al.  2007</a>). Moreover, the kinematics is not dominated by rotation since 
<!-- MATH: $V_{\rm max}/\sigma_0=1.1$ -->
<IMG
 WIDTH="84" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img238.png"
 ALT="$V_{\rm max}/\sigma_0=1.1$">
and the total dynamical mass (
<!-- MATH: $10.2\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="90" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img271.png"
 ALT="$10.2\times10^{10}~{M_\odot}$">)
is dominated by the dispersion mass (
<!-- MATH: $7.9\times10^{10}~{M_\odot}$ -->
<IMG
 WIDTH="82" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img272.png"
 ALT="$7.9\times10^{10}~{M_\odot}$">).
For these reasons, this galaxy showing the highest SFR of the sample is classified as a perturbed rotator possibly in the process of a minor merging event.

<p>

<p>
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