Constraining the Galaxy's dark halo with RAVE stars

Piffl, T.; Binney, J.; McMillan, P. J.; Steinmetz, M.; Helmi, A.; Wyse, R. F. G.; Bienaymé, O.; Bland-Hawthorn, J.; Freeman, K.; Gibson, B.; Gilmore, G.; Grebel, E. K.; Kordopatis, G.; Navarro, J. F.; Parker, Q.; Reid, W. A.; Seabroke, G.; Siebert, A.; Watson, F.; Zwitter, T.

Abstract

© 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. We use the kinematics of ~200 000 giant stars that lie within ~1.5 kpc of the plane to measure the vertical profile of mass density near the Sun. We find that the dark mass contained within the isodensity surface of the dark halo that passes through the Sun ((6 ± 0.9) × 1010M⊙), and the surface density within 0.9 kpc of the plane ((69 ± 10)M⊙pc-2) are almost independent of the (oblate) halo's axis ratio q. If the halo is spherical, 46 per cent of the radial force on the Sun is provided by baryons, and only 4.3 per cent of the Galaxy's mass is baryonic. If the halo is flattened, the baryons contribute even less strongly to the local radial force and to the Galaxy's mass. The dark matter density at the location of the Sun is 0.0126 q-0.89M⊙pc-3= 0.48 q-0.89GeV cm-3. When combined with other literature results we find hints for a mildly oblate dark halo with q ≃ 0.8. Our value for the dark mass within the solar radius is larger than that predicted by cosmological dark-matter-only simulations but in good agreement with simulations once the effects of baryonic infall are taken into account. Our mass models consist of three double-exponential discs, an oblate bulge and a Navarro- Frenk-White dark matter halo, and we model the dynamics of the RAVE (RAdial Velocity Experiment) stars in the corresponding gravitational fields by finding distribution functions f (J) that depend on three action integrals. Statistical errors are completely swamped by systematic uncertainties, the most important of which are the distance to the stars in the photometric and spectroscopic samples and the solar distance to the Galactic Centre. Systematics other than the flattening of the dark halo yield overall uncertainties ~15 per cent.

Citation

Piffl, T., Binney, J., McMillan, P. J., Steinmetz, M., Helmi, A., Wyse, R. F. G., Bienaymé, O., Bland-Hawthorn, J., Freeman, K., Gibson, B., Gilmore, G., Grebel, E. K., Kordopatis, G., Navarro, J. F., Parker, Q., Reid, W. A., Seabroke, G., Siebert, A., Watson, F., & Zwitter, T. (2014). Constraining the Galaxy's dark halo with RAVE stars. Monthly notices of the Royal Astronomical Society, 445(3), 3133-3151. https://doi.org/10.1093/mnras/stu1948

• Journal Article Type: Article
• Acceptance Date: Sep 11, 2014
• Online Publication Date: Oct 24, 2014
• Publication Date: Dec 11, 2014
• Deposit Date: Jun 29, 2018
• Publicly Available Date: Jul 11, 2018
• Journal: Monthly notices of the Royal Astronomical Society
• Print ISSN: 0035-8711
• Electronic ISSN: 1365-2966
• Publisher: Oxford University Press
• Peer Reviewed: Peer Reviewed
• Volume: 445
• Issue: 3
• Pages: 3133-3151
• DOI: https://doi.org/10.1093/mnras/stu1948
• Keywords: Galaxy : disc; Galaxy : fundamental parameters; Galaxy : halo; Galaxy : kinematcs and dynamics; Solar neighborhood; Galaxy : structure
• Public URL: https://hull-repository.worktribe.com/output/543172
• Publisher URL: https://academic.oup.com/mnras/article/445/3/3133/1052064
• Contract Date: Jun 29, 2018