this is for holding javascript data
Paola Oliva-Altamirano edited figures/central_massdyn/caption.tex
almost 9 years ago
Commit id: edec20eda24a68a94736be0c249e6474a360873f
deletions | additions
diff --git a/figures/central_massdyn/caption.tex b/figures/central_massdyn/caption.tex
index a8a1b0c..90408dc 100644
--- a/figures/central_massdyn/caption.tex
+++ b/figures/central_massdyn/caption.tex
...
Replace this text \label{fig:central}
Central stellar populations as a function of dynamical galaxy mass. The SR BCGs are shown as green-filled squares. The FR BCGs are shown as red-open squares. The FR companion galaxies are shown as open stars. The blue crosses represent the central stellar populations of the early-type galaxies in the ATLAS$^{3D}$ sample. The blue-filled circle is the BCG M87 from the ATLAS$^{3D}$ sample. The dashed line shows the mass range (M$_{dyn}> 10^{11.3}$M$_{\odot}$) used in the comparison between the two samples. \textbf{Upper panel:} Central metallicities as a function of dynamical galaxy mass. The BCGs show similar metallicities (median $[$Fe/H$]_{[\alpha/Fe]=0}= 0.13\pm0.07$) compared to the ATLAS$^{3D}$ galaxies at the same mass (median [Z/H~]$= 0.04\pm0.07$). \textbf{Lower panel:} Central ages as a function of mass. The BCGs central ages (median Age~$=8.9\pm3.3$) are consistent with
your caption the ages of the ATLAS$^{3D}$ galaxies of the same mass (median Age~$=12.2\pm1.3$) within $2\sigma$ error. The central stellar populations of BCGs show little scatter or dependence on their angular momentum.
