The surface-brightness profiles of galaxies I(R) and the density profiles of dark-matter halos ρ(r) are well represented by the same analytic function, named after either Sérsic, I ~ e-(R/R∗)1/m, or Einasto, ρ ~ e-(r/r∗)α, where R∗ and r∗ are characteristic radii. Systems with high Sérsic index m (or low Einasto index α) have steep central profiles and shallow outer profiles, while systems with low m (or high α) have shallow central profiles and steep profiles in the outskirts. We present the results of idealized numerical experiments which suggest that the origin of these profiles can be traced back to the initial density fluctuation field: high-α (low-m) systems form in smooth regions via few mergers, while low-α (high-m) systems form in clumpy regions via several mergers.
Nipoti, C. (2016). On the origin of Sérsic profiles of galaxies and Einasto profiles of dark-matter halos. Cambridge University Press [10.1017/S1743921316009455].
On the origin of Sérsic profiles of galaxies and Einasto profiles of dark-matter halos
NIPOTI, CARLO
2016
Abstract
The surface-brightness profiles of galaxies I(R) and the density profiles of dark-matter halos ρ(r) are well represented by the same analytic function, named after either Sérsic, I ~ e-(R/R∗)1/m, or Einasto, ρ ~ e-(r/r∗)α, where R∗ and r∗ are characteristic radii. Systems with high Sérsic index m (or low Einasto index α) have steep central profiles and shallow outer profiles, while systems with low m (or high α) have shallow central profiles and steep profiles in the outskirts. We present the results of idealized numerical experiments which suggest that the origin of these profiles can be traced back to the initial density fluctuation field: high-α (low-m) systems form in smooth regions via few mergers, while low-α (high-m) systems form in clumpy regions via several mergers.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
