Journal
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
Volume 66, Issue 6, Pages -Publisher
OXFORD UNIV PRESS
DOI: 10.1093/pasj/psu124
Keywords
galaxies: halos; galaxies: individual (M 31); galaxies: interactions; galaxies: kinematics and dynamics
Categories
Funding
- JSPS [2024002, 21244013, 25400222]
- Grants-in-Aid for Scientific Research [21244013, 14J00348] Funding Source: KAKEN
Ask authors/readers for more resources
The cold dark matter (CDM) cosmology, which is the standard theory of the structure formation in the universe, predicts that the outer density profile of dark matter halos decreases with the cube of distance from the center. However, so far not much effort has been expended in examining this hypothesis. In the halo of the Andromeda galaxy (M 31), large-scale stellar structures detected by the recent observations provide a potentially suitable window to investigate the mass-density distribution of the dark matter halo. We explore the density structure of the dark matter halo in M 31 using an N-body simulation of the interaction between an accreting satellite galaxy and M 31. To reproduce the Andromeda Giant Southern Stream and the stellar shells at the east and west sides of M 31, we find the sufficient condition for the power-law index alpha of the outer density distribution of the dark matter halo. The best-fitting parameter is alpha=-3.7, which is steeper than the CDM prediction.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available