On the survival of metallicity gradients to major dry-mergers

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Table 1:

Galaxy parameters. Both the stellar and dark mater profiles are represented by Plummer models, having characteristic masses, respectively, given by $M_{\rm B}$ and $M_{\rm H}$ and core radii given by $r_{\rm B}$ and $r_{\rm H}$ .
	gE0	gE0l	gE0m	iE0
$M_{\rm B}\ [2.3\times 10^9 ~M_{\odot}]$	70	70	70	35
$M_{\rm H}\ [2.3\times 10^9 ~M_{\odot}]$	30	30	30	15
$r_{\rm B}\ [{\rm kpc}]$	4.0	6.0	2.0	2.8
$r_{\rm H}\ [{\rm kpc}]$	7.0	7.0	7.0	5.0
$N_{\rm star}$	80 000	80 000	80 000	40 000
$N_{\rm DM}$	40 000	40 000	40 000	20 000

Source LaTeX | All tables | In the text

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