The radial velocity dispersion profile of the Galactic halo : constraining the density profile of the dark halo of the Milky Way

By G. Battaglia, A. Helmi, H. Morrison, P. Harding, E. Olszewski, M. Mateo, Kenneth C. Freeman, J. Norris, S. Institute, U. O. Department and 5 more. 2005

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We have compiled a new sample of 240 halo objects with accurate distance and radial velocity measurements, including globular clusters, satellite galaxies, field blue horizontal branch (FHB) stars and red giant stars from the Spaghetti survey. The new data lead to a significant increase in the number of known objects for Galactocentric radii beyond 50 kpc, which allows a reliable determination of the radial velocity dispersion profile out to very large distances. The radial velocity dispersion shows an almost constant value of 120 km s −1 out to 30 kpc and then continuously declines down to 50 km s −1 at about 120 kpc. This fall-off puts important constraints on the density profile and total mass of the dark matter halo of the Milky Way. Fo ra constant velocity anisotropy, the isothermal profile is ruled out, while both a dark halo ∞

Subfields: Astronomy and Astrophysics, Instrumentation

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There's no place like home? Statistics of Milky Way-mass dark matter haloes (2009, background): “Recent estimates of the mass of the Galaxy’s dark matter halo range from 1 − 3 × 1012 M (Wilkinson & Evans 1999; Sakamoto et al. 2003; Battaglia et al. 2005; Dehnen et al. 2006; Xue et al. 2008; Li & White 2008).”
Mass and shape of the Milky Way’s dark matter halo with globular clusters from Gaia and Hubble (2018, background): “…and references therein) and Eadie & Harris (2016, and references therein) we conclude that our estimate of M20 and of the extrapolated Mvir lies somewhere in the middle of the very light (Mvir < 1012M , e.g. Battaglia et al. 2005) and of the very heavy ones (Mvir > 2 × 1012M Li & White 2008).”
The Galaxy in Context: Structural, Kinematic, and Integrated Properties (2016, background): “…near-main-sequence turnoff (nMSTO) stars (Bond et al. 2010, green), blue horizontal branch (BHB) stars (Kafle et al. 2012, purple; Deason et al. 2013, blue), blue straggler stars (Deason et al. 2012, cyan), K giants (Kafle et al. 2014, black), and mixed tracers (Battaglia et al. 2005, red).”
How do galaxies populate dark matter haloes (2009, unknown): “…& Evans 1999), 2.5+0.5 −1.0 or 1.8 +0.4 −0.7 (Sakamoto et al. 2003), depending on whether or not Leo I is included (see also, Li & White 2008, for the former case), 1.42+1.14 −0.54 (Smith & et al. 2007), 0.5 − 1.5 (Battaglia et al. 2005; Dehnen et al. 2006), and 1.0+0.3 −0.2 (Xue et al. 2008).”
The stellar halo of the Galaxy (2008, background): “Its half-mass radius lies around 150 kpc (Klypin et al. 2002; Battaglia et al. 2005, 2006), and therefore its structure is probably related to the present-day nearby large scale tidal field (Navarro et al. 2004).”
The formation of disc galaxies in high-resolution moving-mesh cosmological simulations (2013, background): “We note that recent estimates of the mass of the Galaxy’s dark matter halo range from 1−3×1012 (Wilkinson & Evans 1999; Sakamoto et al. 2003; Battaglia et al. 2005; Dehnen et al. 2006; Xue et al. 2008; Li & White 2008).”
KINEMATICS OF THE STELLAR HALO AND THE MASS DISTRIBUTION OF THE MILKY WAY USING BLUE HORIZONTAL BRANCH STARS (2012, background): “Hence theσr profile is easy to compute at large distances and this has been well studied; Battaglia et al. (2005) studied the line-of-sight velocity dispersion (σlos) of a mixture of 240 halo objects and found thatσlos decreases monotonically beyondr ∼ 30 kpc.”
Dark matter annihilation and decay in dwarf spheroidal galaxies: the classical and ultrafaint dSphs (2015, methodology): “(19) We have used both a Navarro-Frenk-White (Navarro, Frenk & White 1997; Battaglia et al. 2005) and an Einasto profile (Navarro et al. 2004; Springel et al. 2008) for the MW density, with no impact on the results.”
The APOSTLE project: Local Group kinematic mass constraints and simulation candidate selection (2015, background): “…virial1 masses of both MW and M31, typically based on the kinematics of tracers such as satellite galaxies, halo stars, or tidal debris (see e.g. Battaglia et al. 2005; Sales et al. 2007; Smith et al. 2007; Xue et al. 2008; Watkins, Evans & An 2010; Deason et al. 2012; Boylan-Kolchin et al.…”
THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3 EARLY RELEASE SCIENCE DATA: PANCHROMATIC FAINT OBJECT COUNTS FOR 0.2–2 μm WAVELENGTH (2010, background): “Theoretical disk+bulge+halo models (Battaglia et al. 2005, Klypin et al. 2002) predict velocity dispersions at R∼5-10 kpc of 150 km/sec for the Galactic bulge+thick disk components.”
Stars beyond galaxies: the origin of extended luminous haloes around galaxies (2005, unknown): “For example, just like PNe around ellipticals, the velocity dispersion of these halo tracers drops significantly in the outer regions of the Milky Way (Battaglia et al 2005, Clewley et al 2005).”
Determination of the Local Dark Matter Density in our Galaxy (2009, methodology): “…for which better data became available in recent years: 1. the total mass of the Galaxy has to be about 1012 solar masses (Wilkinson and Evans 1999; Battaglia et al. 2005; Xue et al. 2008); 2. the total mass inside the solar orbit is constrained by the well-known rotation speed of the solar…”
The missing massive satellites of the Milky Way (2012, background): “…agreement with the lower virial masses reported by estimates based on (i) the radial velocity dispersion of Milky Way satellites and halo stars (Battaglia et al. 2005; Sales et al. 2007); (ii) the escape speed in the solar neighbourhood (Smith et al. 2007); or (iii) the kinematics of halo blue…”
The RAVE Survey: Constraining the Local Galactic Escape Speed (2006, methodology): “Another complementary approach that can be adopted is to analyse the radial velocity dispersion profile of halo objects; Battaglia et al. (2005, 2006) used this method to determine a total mass of 0.5–1.5×1012 M depending on the chosen model for the halo profile (see also Dehnen, McLaughlin &…”
Galactic stellar haloes in the CDM model (2009, methodology): “Aquarius (Springel et al. 2008a) is a suite of high-resolution simulations of six DM haloes having masses within the range 1−2 × 1012 M , comparable to values typically inferred for the Milky Way halo (e.g. Battaglia et al. 2005; Smith et al. 2007; Li & White 2008; Xue et al. 2008).”
The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution (2016, background): “For halo tracers, profile of the radial velocity dispersionσr can be easily estimated from the line-of-sight velocity dispersionσlos (Battaglia et al. 2005; Dehnen et al. 2006), while their number density is found to follow a double power law with a break radiusrb around 20 kpc (Bell et al. 2008;…”
Galactic Searches for Dark Matter (2012, background): “The potential is determined assuming that ρs ∝ r−3.5 and that the orbits of the tracers are isotropic. aThe Dehnen et al. (2006) results are from a reanalysis of the Battaglia et al. (2005) data.”
`Skinny Milky Way please', says Sagittarius (2014, result): “Our results represent another piece in the growing body of evidence (Battaglia et al. 2005; Bovy et al. 2012; Deason et al. 2012; Rashkov et al. 2013) that suggests the Milky Way galaxy is less massive than previously assumed.”