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Investigating the Origins of Dark Matter Halo Density Profiles

  • Authors: Liliya L. R. Williams, Arif Babul, and Julianne J. Dalcanton

Williams, Babul, & Dalcanton 2004 The Astrophysical Journal 604 18.

  • Provider: AAS Journals

Caption: Fig. 2.

Top panels show apo‐ and pericenters, while bottom panels show angular and radial momenta of individual shells (points), and averaged over shells from many halos at the same initial comoving position x (lines). Solid lines and points represent the reference halo (§ 4.3). The dashed lines represent halos generated using a smoothed power spectrum with ﹩r_{f}=0.1﹩ Mpc (§ 4.6). Notice the scatter in properties from shell to shell. Also note that shells in halos with less fluctuation power on small scales (dashed lines) have more angular and radial momentum and do not penetrate deep into the halo’s interior (see § 5.5.)

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