English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We investigate the kinematics of red clump stars in the Solar Neighbourhoodby combining data from TGAS and RAVE to constrain the local dark matterdensity. After calibrating the absolute magnitude of red clump stars, wecharacterize their velocity distribution over a radial distance range of$6$-$10$ kpc and up to $1.5$ kpc away from the Galactic plane. We then applythe axisymmetric Jeans equations on subsets representing the thin and thickdisks to determine the (local) distribution of mass near the disk of ourGalaxy. Our kinematic maps are well-behaved permitting a straightforward localdetermination of the vertical force, which we find to be $K_z^{\rm thin} =-2454 \pm 619$ and $K_z^{\rm thick} = -2141 \pm 774$ $(\mathrm{km/s})^2 \!/\mathrm{kpc}$ at $1.5$ kpc away from the Galactic plane for the thin and thickdisk samples and for thin and thick disk scale heights of 0.28 kpc and 1.12 kpcrespectively. These measurements can be translated into a local dark matterdensity $\rho_\textrm{DM} \sim 0.018 \pm 0.002 M_\odot/\textrm{pc}^3$. Thesystematic error on this estimate is much larger than the quoted statisticalerror, since even a 10% difference in the scale height of the thin disk leadsto a 30% change in the value of $\rho_\textrm{DM}$, and a nearly equally goodfit to the data.

The vertical force in the Solar Neighbourhood using red clump stars in TGASxRAVE - Constraints on the local dark matter density