The Milky Way’s Circular Velocity Curve to 60 kpc and an Estimate of the Dark Matter Halo Mass from the Kinematics of ∼2400 SDSS Blue Horizontal‐Branch Stars

Xue, Xiang-Xiang; Rix, Hans─Walter; Zhao, Gang; Fiorentin, P. Re; Naab, Thorsten; Steinmetz, Matthias; Bosch, Frank C. van den; Beers, Timothy C.; Lee, Young Sun; Bell, Eric F.; Rockosi, C. M.; Yanny, B.; Newberg, Heidi Jo; Wilhelm, Ronald; Kang, Xi; Smith, M. C.; Schneider, Donald P.

doi:10.1086/589500

Cited by 628 publications

(574 citation statements)

References 64 publications

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“…In this case, the fact that the MW has only three satellites with V max ≥ 30 km s −1 (the two MCs and Sagittarius) requires the virial mass of the MW halo to be M 200 < 1.4 × 10 12 M at 90 per cent confidence; on the other hand, the existence of the two MCs, which have V max ≥ 60 km s −1 , requires M 200 > 1.0 × 10 12 M , also at 90 per cent confidence. This conclusion is consistent with some, but not all, recent measurements of the MW mass (Battaglia et al 2005;Smith et al 2007;Xue et al 2008;Guo et al 2010;Watkins, Evans & An 2010;Busha et al 2011a;González, Kravtsov & Gnedin 2014;Diaz et al 2014;Piffl et al 2014).…”

Section: Discussionsupporting

confidence: 92%

“…We take haloes in the mass range (0.8-3) × 10 12 M as reference since this interval encompasses the likely value for the MW as seen in the preceding section and also as argued by e.g. Battaglia et al (2005), Dehnen, McLaughlin & Sachania (2006), Xue et al (2008), Gnedin et al (2010), Guo et al (2010). The figure shows that, to (10-20) per cent accuracy, the number of substructures is independent of host halo mass over the mass range 10 11 -10 13 M .…”

Section: T H E M a S S D I S T R I B U T I O N O F T H E M Wmentioning

confidence: 99%

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Milky Way mass constraints from the Galactic satellite gap

Cautun

Frenk

Weygaert

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We use the distribution of maximum circular velocities, V max , of satellites in the Milky Way (MW) to constrain the virial mass, M 200 , of the Galactic halo under an assumed prior of a ΛCDM universe. This is done by analysing the subhalo populations of a large sample of halos found in the Millennium II cosmological simulation. The observation that the MW has at most three subhalos with V max 30 km/s requires a halo mass M 200 1.4 × 10 12 M , while the existence of the Magellanic Clouds (assumed to have V max 60 km/s) requires M 200 1.0 × 10 12 M . The first of these conditions is necessary to avoid the "too-big-to-fail" problem highlighted by Boylan-Kolchin et al., while the second stems from the observation that massive satellites like the Magellanic Clouds are rare. When combining both requirements, we find that the MW halo mass must lie in the range 0.25 M 200 /(10 12 M ) 1.4 at 90% confidence. The gap in the abundance of Galactic satellites between 30 km/s V max 60 km/s places our galaxy in the tail of the expected satellite distribution.

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Section: Discussionsupporting

confidence: 92%

Section: T H E M a S S D I S T R I B U T I O N O F T H E M Wmentioning

confidence: 99%

Milky Way mass constraints from the Galactic satellite gap

Cautun

Frenk

Weygaert

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…Although the halo mass of Milky Way itself is in debate (e.g. Xue et al (2008) and references therein), we take a relatively lower mass among suggested values. For a (slightly) small value of M halo , the relative mass ratio M satellite /M halo becomes larger.…”

Section: Numerical Simulationsmentioning

confidence: 99%

Structure of dark matter halos in warm dark matter models and in models with long-lived charged massive particles

Kamada

Yoshida

Kohri

et al. 2013

J. Cosmol. Astropart. Phys.

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We study the formation of non-linear structures in Warm Dark Matter (WDM) models and in a Long-Lived Charged Massive Particle (CHAMP) model. CHAMPs with a decay lifetime of about 1 yr induce characteristic suppression in the matter power spectrum at subgalactic scales through acoustic oscillations in the thermal background. We explore structure formation in such a model. We also study three WDM models, where the dark matter particles are produced through the following mechanisms: i) WDM particles are produced in the thermal background and then kinematically decoupled; ii) WDM particles are fermions produced by the decay of thermal heavy bosons; and iii) WDM particles are produced by the decay of non-relativistic heavy particles. We show that the linear matter power spectra for the three models are all characterised by the comoving Jeans scale at the matter-radiation equality. Furthermore, we can also describe the linear matter power spectrum for the Long-Lived CHAMP model in terms of a suitably defined characteristic cut-off scale k Ch , similarly to the WDM models. We perform large cosmological N -body simulations to study the non-linear growth of structures in these four models. We compare the halo mass functions, the subhalo mass functions, and the radial distributions of subhalos in simulated Milky Way-size halos. For the characteristic cut-off scale k cut = 51 h Mpc −1 , the subhalo abundance -2 -(∼ 10 9 M sun ) is suppressed by a factor of ∼ 10 compared with the standard ΛCDM model. We then study the models with k cut ≃ 51, 410, 820 h Mpc −1 , and confirm that the halo and the subhalo abundances and the radial distributions of subhalos are indeed similar between the different WDM models and the Long-Lived CHAMP model. The result suggests that the cut-off scale k cut not only characterises the linear power spectra but also can be used to predict the non-linear clustering properties. The radial distribution of subhalos in Milky Way-size halos is consistent with the observed distribution for k cut ∼ 50 − 800 h Mpc −1 ; such models resolve the so-called "missing satellite problem".

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“…For regions beyond the Galactic disc, the RC needs to be measured using halo stars, such as the blue horizontal branch (BHB) stars (Xue et al 2008;Deason et al 2012;Kafle et al 2012;Williams & Evans 2015) and the K giants (Bhattacharjee, Chaudhury, & Kundu 2014, hereafter BCK14), globular clusters or dwarf galaxies. For those tracers of halo populations (assuming isotropically distributed), the radial velocity dispersion σr, number density ν and velocity anisotropy parameter β ≡ 1 − σ 2 t /σ 2 r , are linked to the circular velocity Vc through the Jeans equation (see, e.g.…”

mentioning

confidence: 99%

“…BCK14) or predicted by numerical simulations (e.g. Xue et al 2008;BCK14) have been adopted in the spherical Jeans equation to derive the RC. Only more recently, some constraints on the anisotropy parameter, mainly for the inner halo ( 25 kpc), have become available, based on some direct/indirect measurements (e.g.…”

mentioning

confidence: 99%

The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution

Huang

Liu

Yuan

et al. 2016

Mon. Not. R. Astron. Soc.

165

179

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The rotation curve (RC) of the Milky Way out to ∼ 100 kpc has been constructed using ∼ 16, 000 primary red clump giants (PRCGs) in the outer disk selected from the LSS-GAC and the SDSS-III/APOGEE survey, combined with ∼ 5700 halo K giants (HKGs) selected from the SDSS/SEGUE survey. To derive the RC, the PRCG sample of the warm disc population and the HKG sample of halo stellar population are respectively analyzed using a kinematical model allowing for the asymmetric drift corrections and re-analyzed using the spherical Jeans equation along with measurements of the anisotropic parameter β currently available. The typical uncertainties of RC derived from the PRCG and HKG samples are respectively 5-7 km s −1 and several tens km s −1 . We determine a circular velocity at the solar position, V c (R 0 ) = 240 ± 6 km s −1 and an azimuthal peculiar speed of the Sun, V ⊙ = 12.1 ± 7.6 km s −1 , both in good agreement with the previous determinations. The newly constructed RC has a generally flat value of 240 km s −1 within a Galactocentric distance r of 25 kpc and then decreases steadily to 150 km s −1 at r ∼ 100 kpc. On top of this overall trend, the RC exhibits two prominent localized dips, one at r ∼ 11 kpc and another at r ∼ 19 kpc. From the newly constructed RC, combined with other constraints, we have built a parametrized mass model for the Galaxy, yielding a virial mass of the Milky Way's dark matter halo of 0.90 +0.07 −0.08 × 10 12 M ⊙ and a local dark matter density, ρ ⊙,dm = 0.32 +0.02 −0.02 GeV cm −3 .

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The Milky Way’s Circular Velocity Curve to 60 kpc and an Estimate of the Dark Matter Halo Mass from the Kinematics of ∼2400 SDSS Blue Horizontal‐Branch Stars

Cited by 628 publications

References 64 publications

Milky Way mass constraints from the Galactic satellite gap

Milky Way mass constraints from the Galactic satellite gap

Structure of dark matter halos in warm dark matter models and in models with long-lived charged massive particles

The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution

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