2010
DOI: 10.1051/0004-6361/200913381
|View full text |Cite
|
Sign up to set email alerts
|

Determination of the local dark matter density in our Galaxy

Abstract: Context. The rotation curve, the total mass and the gravitational potential of the Galaxy are sensitive measurements of the dark matter halo profile. Aims. Cuspy and cored DM halo profiles are analysed with respect to recent astronomical constraints in order to constrain the shape of the Galactic DM halo and the local DM density. Methods. All Galactic density components (luminous matter and DM) are parametrized. Then the total density distribution is constrained by astronomical observations: 1) the total mass … Show more

Help me understand this report
View preprint versions

Search citation statements

Order By: Relevance

Paper Sections

Select...
2
1
1
1

Citation Types

18
228
2
1

Year Published

2010
2010
2024
2024

Publication Types

Select...
5
3

Relationship

0
8

Authors

Journals

citations
Cited by 228 publications
(249 citation statements)
references
References 60 publications
18
228
2
1
Order By: Relevance
“…The values of ρ found in previous studies by means of the traditional methods (e.g. Sofue et al 2009;Weber & de Boer 2010) differ among themselves and also from the present value only by a small factor. This relatively good agreement in the values does not imply a concordance in the underlying mass models, in the various assumptions taken or in the data set employed, but is mainly due to the fact that ω or equivalently A − B (the well known combination of Oort constants) is measured with good precision.…”
Section: Discussioncontrasting
confidence: 84%
See 2 more Smart Citations
“…The values of ρ found in previous studies by means of the traditional methods (e.g. Sofue et al 2009;Weber & de Boer 2010) differ among themselves and also from the present value only by a small factor. This relatively good agreement in the values does not imply a concordance in the underlying mass models, in the various assumptions taken or in the data set employed, but is mainly due to the fact that ω or equivalently A − B (the well known combination of Oort constants) is measured with good precision.…”
Section: Discussioncontrasting
confidence: 84%
“…While this result would be noticeable, it has not been confirmed by a subsequent work (Weber & de Boer 2010) and it seems unlikely, in view of Eqs. (2) and (3), reflecting the state of art of our (lack of) knowledge.…”
Section: Introductioncontrasting
confidence: 55%
See 1 more Smart Citation
“…following the Navarro-Frenk-White (NFW) profile Navarro et al (1997) and flatter for warm dark matter (e.g. isothermal profile) (Weber & de Boer 2010) or when including baryons (Dutton & Macciò 2014). Both cases can be described by the generalised profile…”
Section: Mass Within Field Of Viewmentioning
confidence: 99%
“…The gaussian priors and the astrophysical likelihood are given in details in [87]. Only in the case of Maxwellian velocity distribution we do not vary the astrophysical observable in their allowed range but keep them fixed at their mean values, which arev 0 = 230 kms −1 [97,98], v esc = 544 kms −1 [99,100] andρ = 0.4 GeVcm −3 [101,102].…”
Section: Experiments Mcmc Parameter Priormentioning
confidence: 99%