Cores of Dark Matter Halos Correlate with Disk Scale Lengths

Details Cores of Dark Matter Halos Correlate with Disk Scale Lengths Cores of Dark Matter Halos Correlate with Disk Scale Lengths

2004-03-09

arxiv.org/abs/astro-ph/0403206v3

Mon.Not.Roy.Astron.Soc.353:L17-L22, 2004

Astronomy and Astrophysics

Astrophysics

MNRAS accepted, 1 appendix and 1 figure added, results unchanged

Scientific paper

10.1111/j.1365-2966.2004.08220.x

We investigate in detail the mass distribution obtained by means of high resolution rotation curves of 25 galaxies of different morphological types. The dark matter contribution to the circular rotation velocity is well-described by resorting to a dark component whose density shows an inner core, i.e. a central constant density region. We find a very strong correlation between the core radius size $R_C$ and the stellar exponential scale length $R_D$: $R_C \simeq 13 (\frac {R_D} {5 {\rm kpc}})^{1.05} {\rm kpc} $, and between $R_C$ and the galaxy dynamical mass at this distance, $M_{dyn}(R_C)$. These relationships would not be expected if the core radii were the product of an incorrect decomposition procedure, or the biased result of wrong or misunderstood observational data. The very strong correlation between the dark and luminous scale lengths found here seems to hold also for different Hubble types and opens new scenarios for the nature of the dark matter in galaxies.

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