The localdark matter density from SDSS-SEGUE G-dwarfs

Sivertsson, Sofia; Silverwood, H.; Read, Justin I.; Bertone, Gianfranco; Steger, Pascal

doi:10.1093/mnras/sty977

Cited by 98 publications

(140 citation statements)

References 45 publications

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“…The obtained values of ρ DM, from the analyses of the B1 and the B2 baryonic models are around ρ DM, ∼ 0.30 GeV/cm 3 and ρ DM, ∼ 0.38 GeV/cm 3 , respectively. These values are consistent with most of the previous studies (some recent examples are [16,[29][30][31][32]), but smaller than others (such as the recent estimates of [33,34]). One explanation could be the different method used to estimate ρ DM, , since [33,34] exploit the local z-Jeans equation method, which is based on the vertical movement of stars in a region close to the Solar System (see e.g.…”

Section: Estimated Local Dark Matter Densitysupporting

confidence: 92%

On the estimation of the local dark matter density using the rotation curve of the Milky Way

Salas

Malhan

Freese

et al. 2019

J. Cosmol. Astropart. Phys.

139

136

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The rotation curve of the Milky Way is commonly used to estimate the local dark matter density ρDM, . However, the estimates are subject to the choice of the distribution of baryons needed in this type of studies. In this work we explore several Galactic mass models that differ in the distribution of baryons and dark matter, in order to determine ρDM, . For this purpose we analyze the precise rotation curve measurements of the Milky Way up to ∼ 25 kpc from the Galactic centre obtained from Gaia DR2 [1]. We find that the estimated value of ρDM, stays robust to reasonable changes in the spherical dark matter halo. However, we show that ρDM, is affected by the choice of the model for the underlying baryonic components. In particular, we find that ρDM, is mostly sensitive to uncertainties in the disk components of the Galaxy. We also show that, when choosing one particular baryonic model, the estimate of ρDM, has an uncertainty of only about 10% of its best-fit value, but this uncertainty gets much bigger when we also consider the variation of the baryonic model. In particular, the rotation curve method does not allow to exclude the presence of an additional very thin component, that can increase ρDM, by more than a factor of 8. Therefore, we conclude that exclusively using the rotation curve of the Galaxy is not enough to provide a robust estimate of ρDM, . For all the models that we study without the presence of an additional thin component, our resulting estimates of the local dark matter density take values in the range ρDM, 0.3-0.4 GeV/cm 3 , consistent with many of the estimates in the literature.

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Section: Estimated Local Dark Matter Densitysupporting

confidence: 92%

On the estimation of the local dark matter density using the rotation curve of the Milky Way

Salas

Malhan

Freese

et al. 2019

J. Cosmol. Astropart. Phys.

139

136

View full text Add to dashboard Cite

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“…This is opposed to the "local" method, which, instead relies on local observables only, typically the position and motions of stars within few kpc from the Solar system to infer the local gravitational potential and DM density, e.g. [52][53][54][55][56][57][58][59]. For a review and discussion of both methods see [60].…”

Section: Setup and Datamentioning

confidence: 99%

Handling the uncertainties in the Galactic Dark Matter distribution for particle Dark Matter searches

Benito

Cuoco

Iocco

2019

J. Cosmol. Astropart. Phys.

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In this work we characterize the distribution of Dark Matter (DM) in the Milky Way (MW), and its uncertainties, adopting the well known "Rotation Curve" method. We perform a full marginalization over the uncertainties of the Galactic Parameters and over the lack of knowledge on the morphology of the baryonic components of the Galaxy. The local DM density ρ 0 is constrained to the range 0.3−0.8 GeV/cm 3 at the 2σ level, and has a strong positive correlation to R 0 , the local distance from the Galactic Center. The not well-known value of R 0 is thus, at the moment, a major limitation in determining ρ 0 . Similarly, we find that the inner slope of the DM profile, γ, is very weakly constrained, showing no preference for a cored profile (γ 0) or a cuspy one (γ [1.0, 1.4]). Some combination of parameters can be, however, strongly constrained. For example the often used standard ρ 0 = 0.3 GeV/cm 3 , R 0 = 8.5 kpc is excluded at more than 4 σ. We release the full likelihood of our analysis in a tabular form over a multidimensional grid in the parameters characterizing the DM distribution, namely the scale radius R s , the scale density ρ s , the inner slope of the profile γ, and R 0 . The likelihood can be used to include the effect of the DM distribution uncertainty on the results of searches for an indirect DM signal in gamma-rays or neutrinos, from the Galactic Center (GC), or the Halo region surrounding it. As one example, we study the case of the GC excess in gamma rays. Further applications of our tabulated uncertainties in the DM distribution involve local DM searches, like direct detection and anti-matter observations, or global fits combining local and GC searches.

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“…In the master equation for the differential rate, ξ T is the mass fraction for each type of target nucleus T (the detector could be composed of different nuclides), m T is the target nucleus mass and N T = 1/m T is number of scattering centers per unit mass. ρ χ is the local DM density in the solar system, which we take to be ρ χ = 0.4 GeV/cm 3 [49][50][51]. 2f ( v) is the local DM velocity distribution in the Earth frame.…”

Section: A Dd Basicsmentioning

confidence: 99%

Implications of the Gaia sausage for dark matter nuclear interactions

2020

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The advent of the Gaia era has led to potentially revolutionary understanding of dark matter (DM) dynamics in our galaxy, which has important consequences for direct detection (DD) experiments. In this paper, we study how the empirical DM velocity distribution inferred from Gaia-Sausage, a dominant substructure in the solar neighborhood, affects the interpretation of DD data. We survey different classes of operators in the non-relativistic effective field theory that could arise from several relativistic benchmark models and emphasize that the Gaia velocity distribution could modify both the total number of events as well as the shape of the differential recoil spectra, the two primary observables in DD experiments. Employing the euclideanized signal method, we investigate the effects of the Gaia distribution on reconstructing DM model parameters and identifying the correct DM model given a positive signal at future DD experiments. We find that for light DM with mass ∼ 10 GeV, the Gaia distribution poses an additional challenge for characterizing DM interactions with ordinary matter, which may be addressed by combining complementary DD experiments with different targets and lowering the detection threshold. Meanwhile, for heavy DM with mass above ∼ 30 GeV, depending on the type of DM model, there could be a (moderate) improvement in the sensitivity at future DD experiments.

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The localdark matter density from SDSS-SEGUE G-dwarfs

Cited by 98 publications

References 45 publications

On the estimation of the local dark matter density using the rotation curve of the Milky Way

On the estimation of the local dark matter density using the rotation curve of the Milky Way

Handling the uncertainties in the Galactic Dark Matter distribution for particle Dark Matter searches

Implications of the Gaia sausage for dark matter nuclear interactions

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