Using <i>Gaia</i> DR2 to constrain local dark matter density and thin dark disk

Buch, Jatan; Leung, Shing Chau; Fan, JiJi

doi:10.1088/1475-7516/2019/04/026

Cited by 122 publications

(148 citation statements)

References 100 publications

Supporting

Mentioning

140

Contrasting

Order By: Relevance

“…Under a fifth force model the Cepheid distances are altered tod i j , as we quantify below, so that the true galaxy distancesD i are an average over the distancesd i j implied by each of the individual Cepheids, weighted by the inverse square of their magnitude uncertainties ∆m i j (period uncertainties are subdominant and not quoted in R16). This ensures that galaxies with smaller 7 An alternative estimate of ρ local from Gaia suggests a slightly higher value of 1.6 × 10 7 M kpc −3 [125]. However, we also require the bulk of the observed Cepheids in the MW to be screened so that they calibrate the Newtonian PLR.…”

Section: Cepheid Distancesmentioning

confidence: 99%

Local resolution of the Hubble tension: The impact of screened fifth forces on the cosmic distance ladder

2019

View full text Add to dashboard Cite

The discrepancy between the values of the Hubble constant H 0 derived from the local distance ladder and the Cosmic Microwave Background provides a tantalising hint of new physics. We explore a potential resolution involving screened fifth forces in the local Universe, which alter the Cepheid calibration of supernova distances. In particular, if the Cepheids with direct distance measurements from parallax or water masers are screened but a significant fraction of those in other galaxies are not, neglecting the difference between their underlying period-luminosity relations biases the local H 0 measurement high. This difference derives from a reduction in the Cepheid pulsation period and possible increase in luminosity under a fifth force. We quantify the internal and environmental gravitational properties of the Riess et al. distance ladder galaxies to assess their degrees of screening under a range of phenomenological models, and propagate this information into the H 0 posterior as a function of fifth force strength. We consider well-studied screening models in scalar-tensor gravity theories such as chameleon, K-mouflage and Vainshtein, along with a recently-proposed mechanism based on baryon-dark matter interactions in which screening is governed by the local dark matter density. We find that a fifth force strength ∼ 5 − 30% that of gravity can alleviate the H 0 tension in many scenarios, around the sensitivity level at which tests based on other distance ladder data can constrain this strength. Our most successful models achieve consistency with Planck at the ∼1.5σ level. Although our analysis is exploratory and based on screening models that are not necessarily realised in full theories, our results demonstrate that new physics-based local resolutions of the H 0 tension are possible, supplementing those already known in the pre-recombination era. * harry.desmond@physics.ox.ac.uk

show abstract

Section: Cepheid Distancesmentioning

confidence: 99%

Local resolution of the Hubble tension: The impact of screened fifth forces on the cosmic distance ladder

2019

View full text Add to dashboard Cite

show abstract

“…These estimates are focused on a local volume that excludes the Galactic plane (for example, [16] analysed stars within a vertical distance of |z| = 515-1247 pc for their α-young population and |z| = 634-2266 pc for their α-old population). On the contrary, the three ρ DM, studies that used Gaia's information (references [17,18,19]) present larger uncertainties and some of their estimates do not agree that well with the three older studies. One important difference is that the new estimates are concentrated on the local |z| < 200 pc, including the Galactic plane.…”

Section: Differences In the Methodsmentioning

confidence: 93%

“…Those studies based on the rotation curve ( [13,14,12]), the distribution function fitting ( [8,10] are presented in pink, blue and gray, respectively. The colour is darker for the analyses [17,18,19,12] to show the use of Gaia's observations. It is easy to see a clear difference in the precision and agreement of earlier ρ DM, estimates and those performed after 2017, especially in the three estimates that included Gaia's observations and applied the vertical Jeans equation method.…”

Section: Recent Estimates Of ρ Dmmentioning

confidence: 99%

Dark matter local density determination based on recent observations

Salas

2020

J. Phys.: Conf. Ser.

View full text Add to dashboard Cite

The local density of dark matter is an important quantity. On the one hand, its value is needed for dark matter direct detection searches. On the other hand, a precise and robust determination of the local dark matter density would help us learn about the shape of the dark matter halo of our Galaxy, which plays an important role in dark matter indirect detection searches, as well as in many studies in astrophysics and cosmology. There are different methods available to determine the local dark matter density. Among them, it is common to study either the vertical kinematics of a selected group of tracers or the rotation curve of the Milky Way. Recent estimates of the local dark matter density have used the precise observations conducted by the ESA/Gaia mission. However, in spite of the quality of the data released by Gaia's observations, different analyses of the local dark matter density produce dissimilar results. After a brief review of the most common methods to estimate the local density of dark matter, here we argue about different explanations for the discrepancies in the results of recent analyses. We finish by presenting new approaches that have been proposed in the literature and could help us improve our knowledge of this important quantity.

show abstract

“…DM in the planet's rest frame defined as v d = v i + v e where | v e | ≈ 230 km s −1 is the Earth's velocity in the galactic rest frame [49,50]. We normalize N e in this Maxwell Boltzmann distribution to match a conservatively low background DM density of ρ χ = 0.3 GeV/cm 3 [51][52][53] and truncate the distribution at a conservatively low galactic escape velocity of v esc = 528 km s −1 [54]. For each simulated DM particle, an entry angle θ into the planet in question was randomly chosen, distributed according to the probability density function dP (θ) dθ = 2 sin(θ) cos(θ),…”

Section: Total Annihilationmentioning

confidence: 99%

Terrestrial and martian heat flow limits on dark matter

et al. 2020

View full text Add to dashboard Cite

If dark matter is efficiently captured by a planet, energy released in its annihilation can exceed that planet's total heat output. Building on prior work, we treat Earth's composition and dark matter capture in detail and present improved limits on dark matter-nucleon scattering cross sections for dark matter masses ranging from 0.1 to 10 10 GeV. We also extend Earth limits by applying the same treatment to Mars. The scope of dark matter models considered is expanded to include spin-dependent nuclear interactions including isospin-independent, proton only, and neutron only interactions. We find that Earth and Mars heating bounds are alleviated for dark matter s-wave self-annihilation cross sections 10 −37 cm 2 .

show abstract

Using Gaia DR2 to constrain local dark matter density and thin dark disk

Cited by 122 publications

References 100 publications

Local resolution of the Hubble tension: The impact of screened fifth forces on the cosmic distance ladder

Local resolution of the Hubble tension: The impact of screened fifth forces on the cosmic distance ladder

Dark matter local density determination based on recent observations

Terrestrial and martian heat flow limits on dark matter

Contact Info

Product

Resources

About