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The first and second moments of stellar velocities encode important information about the formation history of the Galactic halo. However, due to the lack of tangential motion and inaccurate distances of the halo stars, the velocity moments in the Galactic halo have largely remained 'known unknowns'. Fortunately, our off-centric position within the Galaxy allows us to estimate these moments in the galactocentric frame using the observed radial velocities of the stars alone. We use these velocities coupled with the hierarchical Bayesian scheme, which allows easy marginalization over the missing data (the proper motion, and uncertainty-free distance and line-of-sight velocity), to measure the velocity dispersions, orbital anisotropy (beta) and streaming motion (v(rot)) of the halo main-sequence turn-off (MSTO) and K-giant (KG) stars in the inner stellar halo (r less than or similar to 15 kpc). We study the metallicity bias in kinematics of the halo stars and observe that the comparatively metal-rich ([Fe/H] > -1.4) and the metal-poor ([Fe/H] sigma(theta) or sigma(phi) and beta similar or equal to 0.5. The apparent metallicity contrariety in the rotation velocity among the halo sub-populations supports the co-existence of multiple populations in the galactic halo that may have formed through distinct formation scenarios, i.e. in situ versus accretion.
|Number of pages||13|
|Journal||Monthly Notices of the Royal Astronomical Society|
|Publication status||Published - 21 Sep 2017|
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How typical is our Local Galaxy Group?
Robotham, A., Driver, S. & Drinkwater, M.
1/01/14 → 31/08/17