Density Variations in the NW Star Stream of M31
R. G. Carlberg, Harvey B. Richer, Alan W. McConnachie, Mike Irwin,, Rodrigo A. Ibata, Aaron L. Dotter, Scott Chapman, Mark Fardal, A. M. N., Ferguson, G. F. Lewis, Julio F. Navarro, Thomas H. Puzia, and David, Valls-Gabaud

TL;DR
This study analyzes the density variations in the NW star stream of M31, finding significant clumpiness that supports the presence of dark matter sub-halos predicted by LCDM models.
Contribution
It provides the first detailed measurement of density variations along the M31 star stream, supporting dark matter sub-halos as a cause.
Findings
Density varies between zero and three times the mean.
Variations are unlikely due to random fluctuations.
Results are consistent with dark matter sub-halos effects.
Abstract
The Pan Andromeda Archeological Survey (PAndAS) CFHT Megaprime survey of the M31-M33 system has found a star stream which extends about 120 kpc NW from the center of M31. The great length of the stream, and the likelihood that it does not significantly intersect the disk of M31, means that it is unusually well suited for a measurement of stream gaps and clumps along its length as a test for the predicted thousands of dark matter sub-halos. The main result of this paper is that the density of the stream varies between zero and about three times the mean along its length on scales of 2 to 20 kpc. The probability that the variations are random fluctuations in the star density is less than 10^-5. As a control sample we search for density variations at precisely the same location in stars with metallicity higher than the stream, [Fe/H]=[0, -0.5] and find no variations above the expected shot…
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