Kinematic Structure in the Galactic Halo at the North Galactic Pole: RR Lyrae and BHB Stars show different kinematics

Details Kinematic Structure in the Galactic Halo at the North Galactic Pole: RR Lyrae and BHB Stars show different kinematics Kinematic Structure in the Galactic Halo at the North Galactic Pole: RR Lyrae and BHB Stars show different kinematics

2006-12-15

arxiv.org/abs/astro-ph/0612416v1

Mon.Not.Roy.Astron.Soc.375:1381-1398,2007

Astronomy and Astrophysics

Astrophysics

Accepted for publication on MNRAS. 20 pages, 7 figures, 12 tables

Scientific paper

10.1111/j.1365-2966.2006.11394.x

Space motions are given for 38 RR Lyrae (RRL) stars and 79 blue horizontal branch (BHB) stars in a ~200 deg2 area around the North Galactic Pole (NGP) using a homogeneous distance scale consistent with (m-M)0=18.52 for the LMC. The kinematics of the 26 RRL and 52 BHB stars in the 10.4 cubic kpc volume that have Z<8 kpc are not homogeneous. Our BHB sample (like that of Sirko et al. 2004b) has a zero galactic rotation (V_phi) and roughly isotropic velocity dispersions. The RRL sample shows a definite retrograde rotation (V_phi = -95+/-29 km/s) and non-isotropic velocity dispersions. The combined BHB and RRL sample has a retrograde galactic rotation (V) that is similar to that found by Majewski (1992) for his sample of subdwarfs in SA 57. The velocity dispersion of the RRL stars that have a positive W motion is significantly smaller than the dispersion of those "streaming down" with a negative W. One component of our sample (rich in RRL's) shows retrograde rotation and the streaming motion that we associate with the accretion process. The other (traced by the BHB stars) shows essentially no rotation and less evidence of streaming. These two components have HB morphologies that suggest that they may be the field star equivalents of the young and old halo globular clusters respectively.

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