The Stellar Halo in the Inner MilkyWay: Predicted Shape and Kinematics
Angeles Pérez-Villegas, Matthieu Portail and Ortwin Gerhard, 2017, MNRAS, 460, L80
We have used N-body simulations for the Milky Way to investigate the kinematic and structural properties of the old metal-poor stellar halo in the barred inner region of the Galaxy. We find that the extrapolation of the density distribution for bulge RR Lyrae stars, ρ(r) ∼ r-3, approximately matches the number density of RR Lyrae in the nearby stellar halo. We follow the evolution of such a tracer population through the formation and evolution of the bar and box/peanut bulge in the N-body model. We find that its density distribution changes from oblate to triaxial, and that it acquires slow rotation in agreement with recent measurements. The maximum radial velocity is ∼15-25 km/s at |l| = 10°-30°, and the velocity dispersion is ∼120 km/s. Even though the simulated metal-poor halo in the bulge has a barred shape, just 12% of the orbits follow the bar, and it does not trace the peanut/X structure. With these properties, the RR Lyrae population in the Galactic bulge is consistent with being the inward extension of the Galactic metal-poor stellar halo.
The structure of the Milky Way's bar outside the bulge
Christopher Wegg, Ortwin Gerhard and Matthieu Portail, 2015, MNRAS, 450, 4050
While it is incontrovertible that the inner Galaxy contains a bar, its structure near the Galactic plane has remained uncertain, where extinction from intervening dust is greatest. We investigate here the Galactic bar outside the bulge, the long bar, using red clump giant (RCG) stars from UKIDSS, 2MASS, VVV, and GLIMPSE. While it is incontrovertible that the inner Galaxy contains a bar, its structure near the Galactic plane has remained uncertain, where extinction from intervening dust is greatest. We investigate here the Galactic bar outside the bulge, the long bar, using red clump giant (RCG) stars from UKIDSS, 2MASS, VVV, and GLIMPSE. We match and combine these surveys to investigate a wide area in latitude and longitude, | b |< 9 deg and | l |< 40 deg.
We find: (1) The bar extends to l~25deg at | b |~ 5 deg from the Galactic plane, and to l ~ 30 deg at lower latitudes. (2) The long bar has an angle to the line-of-sight in the range (28-33) deg, consistent with studies of the bulge at | l |< 10 deg. (3) The scale-height of RCG stars smoothly transitions from the bulge to the thinner long bar. (4) There is evidence for two scale heights in the long bar. We find a ~180pc thin bar component reminiscent of the old thin disk near the sun, and a ~45pc super-thin bar component which exists predominantly towards the bar end. (5) Constructing parametric models for the RC magnitude distributions, we find a bar half length of 5.0+-0.2kpc for the 2-component bar, and 4.6+-0.3kpc for the thin bar component alone. We conclude that the Milky Way contains a central box/peanut bulge which is the vertical extension of a longer, flatter bar, similar as seen in both external galaxies and N-body models.
Mapping the Three-Dimensional Density of the Galactic Bulge with VVV Red Clump Stars
Chris Wegg & Ortwin Gerhard, 2013, MNRAS, 435, 1874
Using red clump giant stars identified in the VVV survey we produced the most accurate and high resolution map of the inner regions of the Milky Way. Our density map covers the inner (2.2x1.4x1.1)kpc of the bulge/bar. Line-of-sight density distributions were estimated by deconvolving extinction and completeness corrected K-band magnitude distributions. In constructing our measurement, we assumed that the three-dimensional bulge is 8-fold mirror triaxially symmetric, but the map is otherwise completely non-parametric. In doing so we measure the angle of the bar-bulge to the line-of-sight to be (27+- 2)deg, where the dominant error is systematic arising from the details of the deconvolution process. Our density distribution shows a highly elongated bar with projected axis ratios ~(1:2.1) for isophotes reaching ~2kpc along the major axis. Along the bar axes the density falls off roughly exponentially, with axis ratios (10:6.3:2.6) and exponential scale-lengths (0.70:0.44:0.18)kpc. From about 400pc above the Galactic plane, the bulge density distribution displays a prominent X-structure. Overall, the density distribution of the Galactic bulge is characteristic for a strongly boxy/peanut shaped bulge within a barred galaxy.
Anyone is welcome to use the movie we made to vizualize the measured 3D structure. Just reference the original paper if you use the movie (Creative Commons attribution share-alike license).
The inner Galactic bulge: evidence for a nuclear bar?
Gerhard, O., Martinez-Valpuesta, I., 2012, ApJ, 744, L8
|l|~4◦. With an N-body barred galaxy simulation we showed that a boxy bulge formed through the bar and buckling instabilities matches these observations. The change in the slope of the model longitude profiles is caused by a transition from highly elongated to more nearly axisymmetric isodensity contours in the inner boxy bulge. This transition is confined to a few degrees from the Galactic plane.
The same simulation snapshot was earlier used to clarify the apparent boxy bulge—long bar dichotomy. Furthermore, the nuclear star count map derived from this simulation snapshot displays a longitudinal asymmetry similar to that observed in the TwoMicron All Sky Survey (2MASS) data. These combined results
- support the interpretation that the Galactic bulge originated from disk evolution,
- and question arguments based on star count data for the existence of a secondary nuclear bar in the Milky Way.