The Local Halo Density

Gates, Evalyn; Gyuk, G.; Turner, Michael S.

doi:10.1086/309652

Cited by 159 publications

(150 citation statements)

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“…However, this value is often given without a reference, and when a reference is given, it can be traced back to papers which are a few decades old, e.g. [7,8]. Notice that the link between observed galaxy masses and their host dark matter halo masses has been studied extensively using satellite kinematics [9,10], weak lensing [11] as well as via abundance matching [12].…”

Section: Introductionmentioning

confidence: 99%

Systematic uncertainties in the determination of the local dark matter density

et al. 2010

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A precise determination of the local dark matter density and an accurate control over the corresponding uncertainties are of paramount importance for Dark Matter (DM) searches. Using very recent high-resolution numerical simulations of a Milky Way like object, we study the systematic uncertainties that affect the determination of the local dark matter density based on dynamical measurements in the Galaxy. In particular, extracting from the simulation with baryons the orientation of the Galactic stellar disk with respect to the DM distribution, we study the DM density for an observer located at ∼8 kpc from the Galactic center on the stellar disk, ρ0. This quantity is found to be always larger than the average density in a spherical shell of same radiusρ0, which is the quantity inferred from dynamical measurements in the Galaxy, and to vary in the range ρ0/ρ0 = 1.01 − 1.41. This suggests that the actual dark matter density in the solar neighbourhood is on average 21% larger than the value inferred from most dynamical measurements, and that the associated systematic errors are larger than the statistical errors recently discussed in the literature.

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Section: Introductionmentioning

confidence: 99%

Systematic uncertainties in the determination of the local dark matter density

et al. 2010

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“…Lensing constraints on the density parameter for compact objects al. 1998), an old superthick disc (Gates & Gyuk 1999), intervening debris (Zhao 1998) or the LMC's own halo (Kerins & Evans 1999). Nevertheless, the following discussion shows that this is not the only context in which microlensing evidence for compact objects arises and it is interesting that the other cases indicate a similar lens mass.…”

Section: Lensing Evidencementioning

confidence: 89%

Recent Developments in the Search for Baryonic Dark Matter

Carr

2001

Phase Transitions in the Early Universe: Theory and Observations

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Abstract. Cosmological nucleosynthesis calculations imply that many of the baryons in the Universe must be dark. We discuss the likelihood that some of these dark baryons may reside in galaxies as Massive Compact Halo Objects (MACHOs), the remnants of a first generation of pregalactic or protogalactic stars. Various candidates have been proposed for such remnants and we review the many types of observations which can be used to detect or exclude them. Claims to have found positive evidence for some of the candidates have generally turned out to be spurious or questionable, so the status of the MACHO scenario remains controversial. However, it would be premature to reject MACHOs altogether and further observations are likely to resolve the issue soon.

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“…X-ray observations exclude the existence of extended x-ray halos or cooling ows in most spiral galaxies (Fabbiano 1989). Searches for microlensing events toward the LMC indicate that a noticeable fraction of the halo mass may consist of baryonic objects (Alcock et al 1995;Gates, Gyuk, & Turner 1994). If these objects formed in the intergalactic medium at very high redshift, then they would be essentially indistinguishable from other types of cold dark matter.…”

Section: Discussionmentioning

confidence: 99%