We determine the Milky Way (MW) mass profile inferred from fitting physically motivated models to the Gaia DR2 Galactic rotation curve and other data. Using various hydrodynamical simulations of MW-mass haloes, we show that the presence of baryons induces a contraction of the dark matter (DM) distribution in the inner regions, r ∼ 20 kpc. We provide an analytic expression that relates the baryonic distribution to the change in the DM halo profile. For our galaxy, the contraction increases the enclosedDMhalomass by factors of roughly 1.3, 2, and 4 at radial distances of 20, 8, and 1 kpc, respectively compared to an uncontracted halo. Ignoring this contraction results in systematic biases in the inferred halo mass and concentration. We provide a best-fitting contracted NFW halo model to the MW rotation curve that matches the data very well.1 The best-fit has a DM halo mass, MDM 200 = 0.97+0.24 -0.19 × 1012M⊙, and concentration before baryon contraction of 9.4+1.9 -2.6, which lie close to the median halo mass- concentration relation predicted in λCDM. The inferred total mass, Mtotal 200 = 1.08+0.20 -0.14 × 1012M⊙, is in good agreement with recent measurements. The model gives an MW stellar mass of 5.04+0.43 -0.52 × 1010M⊙ and infers that the DM density at the Solar position is pDM ⊙ = 8.8+0.5 -0.5 × 10-3M⊙ pc-3 0.33+0.02 -0.02 GeV cm-3. The rotation curve data can also be fitted with an uncontracted NFW halo model, but with very different DM and stellar parameters. The observations prefer the physically motivated contracted NFW halo, but the measurement uncertainties are too large to rule out the uncontracted NFW halo.

Cautun, M., Benitez-Llambay, A., Deason, A., Frenk, C., Fattahi, A., Gómez, F., et al. (2020). The milky way total mass profile as inferred from Gaia DR2. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 494(3), 4291-4313 [10.1093/mnras/staa1017].

The milky way total mass profile as inferred from Gaia DR2

Benitez-Llambay, Alejandro
Secondo
;
2020

Abstract

We determine the Milky Way (MW) mass profile inferred from fitting physically motivated models to the Gaia DR2 Galactic rotation curve and other data. Using various hydrodynamical simulations of MW-mass haloes, we show that the presence of baryons induces a contraction of the dark matter (DM) distribution in the inner regions, r ∼ 20 kpc. We provide an analytic expression that relates the baryonic distribution to the change in the DM halo profile. For our galaxy, the contraction increases the enclosedDMhalomass by factors of roughly 1.3, 2, and 4 at radial distances of 20, 8, and 1 kpc, respectively compared to an uncontracted halo. Ignoring this contraction results in systematic biases in the inferred halo mass and concentration. We provide a best-fitting contracted NFW halo model to the MW rotation curve that matches the data very well.1 The best-fit has a DM halo mass, MDM 200 = 0.97+0.24 -0.19 × 1012M⊙, and concentration before baryon contraction of 9.4+1.9 -2.6, which lie close to the median halo mass- concentration relation predicted in λCDM. The inferred total mass, Mtotal 200 = 1.08+0.20 -0.14 × 1012M⊙, is in good agreement with recent measurements. The model gives an MW stellar mass of 5.04+0.43 -0.52 × 1010M⊙ and infers that the DM density at the Solar position is pDM ⊙ = 8.8+0.5 -0.5 × 10-3M⊙ pc-3 0.33+0.02 -0.02 GeV cm-3. The rotation curve data can also be fitted with an uncontracted NFW halo model, but with very different DM and stellar parameters. The observations prefer the physically motivated contracted NFW halo, but the measurement uncertainties are too large to rule out the uncontracted NFW halo.
Articolo in rivista - Articolo scientifico
Galaxies: Haloes; Galaxy: Fundamental parameters; Galaxy: Halo; Galaxy: Kinematics and dynamics; Galaxy: Structure;
English
2020
494
3
4291
4313
none
Cautun, M., Benitez-Llambay, A., Deason, A., Frenk, C., Fattahi, A., Gómez, F., et al. (2020). The milky way total mass profile as inferred from Gaia DR2. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 494(3), 4291-4313 [10.1093/mnras/staa1017].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10281/396278
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