Astrophysical distribution of DM - TeVPA 2017 · • Large variation in DM speed distributions...
Transcript of Astrophysical distribution of DM - TeVPA 2017 · • Large variation in DM speed distributions...
![Page 1: Astrophysical distribution of DM - TeVPA 2017 · • Large variation in DM speed distributions between the results of different simulations. Different criteria used to identify MW-like](https://reader035.fdocuments.in/reader035/viewer/2022070720/5ee0289aad6a402d666b65aa/html5/thumbnails/1.jpg)
Astrophysical distribution of DM & direct detection implications
Nassim Bozorgnia
GRAPPA Center of ExcellenceUniversity of Amsterdam
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Dark Matter halo
How is Dark Matter (DM) distributed in the Sun’s neighborhood?
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Dark Matter halo
How is Dark Matter (DM) distributed in the Sun’s neighborhood?
Uncertainties in the local DM distribution large uncertainties in the interpretation of direct detection data.
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Dark Matter halo
How is Dark Matter (DM) distributed in the Sun’s neighborhood?
Uncertainties in the local DM distribution large uncertainties in the interpretation of direct detection data.
• Standard Halo model (SHM): isothermal sphere with an isotropic Maxwell-Boltzmann velocity distribution with a peak speed equal to the local circular speed (~220 km/s).
• What can we learn from numerical simulations of galaxy formation about the local DM velocity distribution?
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Nassim Bozorgnia
Dark Matter only simulations
• Significant systematic uncertainty since the impact of baryons neglected.
Vogelsberger et al., 0812.0362
• DM speed distributions from cosmological N-body simulations without baryons, deviate substantially from a Maxwellian.
TeVPA 2017, Columbus, 10 August 2017
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• Each hydrodynamical (DM + baryons) simulation adopts a different galaxy formation model, spatial resolution, DM particle mass.
Nassim Bozorgnia
Hydrodynamical simulations
SHM Ling+'09ErisNIHAOEAGLEMaGICCSloane+'16
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• Large variation in DM speed distributions between the results of different simulations.
Bozorgnia & Bertone, 1705.05853
TeVPA 2017, Columbus, 10 August 2017
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• Each hydrodynamical (DM + baryons) simulation adopts a different galaxy formation model, spatial resolution, DM particle mass.
Nassim Bozorgnia
Hydrodynamical simulations
SHM Ling+'09ErisNIHAOEAGLEMaGICCSloane+'16
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• Large variation in DM speed distributions between the results of different simulations.
Different criteria used to identify MW-like galaxies among different groups. The most common criteria is the MW mass constraint, which has a large uncertainty.
Bozorgnia & Bertone, 1705.05853
TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
EAGLE and APOSTLE• We use the EAGLE and APOSTLE hydrodynamic simulations.
Calibrated to reproduce the observed distribution of stellar masses and sizes of low-redshift galaxies.
TeVPA 2017, Columbus, 10 August 2017
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• Identify MW-like galaxies by taking into account observational constraints on the MW, in addition to the mass constraint: rotation curves [Iocco, Pato, Bertone, 1502.03821], total stellar mass.
Nassim Bozorgnia
Identifying Milky Way analogues
2.5kpc
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EAGLE HR
Bozorgnia et al., 1601.04707 Calore, Bozorgnia et al., 1509.02164
14 MW analogues
TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
Local Dark Matter distribution
ρχ = 0.41 - 0.73 GeV/cm3Local DM density:
• To find the DM distribution at the position of the Sun, consider a torus aligned with the stellar disc.
TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
Local Dark Matter distribution
ρχ = 0.41 - 0.73 GeV/cm3Local DM density:
Local DM speed distribution:
• To find the DM distribution at the position of the Sun, consider a torus aligned with the stellar disc.
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EAGLE HR
Halo 1
Halo 2
Bozorgnia et al., 1601.04707
DMO simulations
vpeak = 223 - 289 km/s
TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
Local Dark Matter distribution
ρχ = 0.41 - 0.73 GeV/cm3Local DM density:
Local DM velocity distribution:
• To find the DM distribution at the position of the Sun, consider a torus aligned with the stellar disc.
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EAGLE HR
Halo 1
Halo 2
Bozorgnia et al., 1601.04707
DMO simulations
• Maxwellian distribution with a free peak provides a better fit to haloes in the hydrodynamical simulations compared to their DMO counterparts.
• Common trend: in most hydrodynamical simulations, baryons appear to make the local DM speed distribution more Maxwellian.
vpeak = 223 - 289 km/s
TeVPA 2017, Columbus, 10 August 2017
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azimuthalradial
vertical
• Only two haloes have a rotating DM component in the disc with mean velocity comparable to that of the stars.
Nassim Bozorgnia
How common are dark disks?
Hint for the existence of a co-rotating dark disk in 2 out of 14 MW analogues.
TeVPA 2017, Columbus, 10 August 2017
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azimuthalradial
vertical
• Only two haloes have a rotating DM component in the disc with mean velocity comparable to that of the stars.
Nassim Bozorgnia
How common are dark disks?
• Sizable dark disks also rare in other hydro simulations:
• They only appear in simulations where a large satellite merged with the MW in the recent past, which is robustly excluded from MW kinematical data.
Hint for the existence of a co-rotating dark disk in 2 out of 14 MW analogues.
TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
The halo integral
• Halo integrals for the best fit Maxwellian velocity distribution (peak speed 223 - 289 km/s) fall within the 1σ uncertainty band of the halo integrals of the simulated haloes.
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EAGLE HR
Bozorgnia et al., 1601.04707
• For standard spin-independent and spin-dependent interactions:astrophysics
particle physics
TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
The halo integral
• Halo integrals for the best fit Maxwellian velocity distribution (peak speed 223 - 289 km/s) fall within the 1σ uncertainty band of the halo integrals of the simulated haloes.
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• For standard spin-independent and spin-dependent interactions:astrophysics
particle physics
• This conclusion also holds for a very general set of non-standard DM-nucleus interactions.
• Common trend: halo integrals and hence direct detection event rates obtained from a Maxwellian velocity distribution with a free peak are similar to those obtained directly from the simulated haloes.
Bozorgnia et al., 1601.04707 (EAGLE & APOSTLE) Kelso et al., 1601.04725 (MaGICC) Sloane et al., 1601.05402Bozorgnia & Bertone, 1705.05853
TeVPA 2017, Columbus, 10 August 2017
Bozorgnia et al., 1601.04707
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Nassim Bozorgnia
Implications for direct detection
LUX
DAMA
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Fix local ρχ=0.3 GeV cm-3
• Difference in the local DM density overall difference with the SHM.
• Variation in the peak of the DM speed distribution shift in the low mass region.
TeVPA 2017, Columbus, 10 August 2017
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• To make precise quantitative predictions for the DM distribution from simulations Identify MW analogues by taking into account observational constraints on the MW.
• Local DM density agrees with local and global estimates.
• Halo integrals of MW analogues match well those obtained from best fit Maxwellian velocity distributions.
• A Maxwellian velocity distribution with peak speed constrained by hydrodynamical simulations, and independent from the local circular speed, could be used for the analysis of direct detection data.
Summary
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Backup Slides
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• Spherically averaged DM density profiles of the MW analogues:
Nassim Bozorgnia
Dark Matter density profiles
Bozorgnia et al., 1601.04707
TeVPA 2017, Columbus, 10 August 2017
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• For a very general set of non-relativistic effective operators:
Nassim Bozorgnia
Non-standard interactions
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Kahlhoefer & Wild, 1607.04418
Bozorgnia & Bertone, 1705.05853
• Best fit Maxwellian falls within the 1σ uncertainty band of the h of the simulated haloes.
TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
Departure from isothermal
Hydro
DMO
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TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
Parameters of the simulations
Properties of the selected MW analogues
TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
Implications for direct detection
Fix local ρχ=0.3 GeV cm-3
Comparison to other hydrodynamical simulations:
Bozorgnia & Bertone, 1705.05853
TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
Observations vs. simulations
TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
Selection criteria for MW analogues
TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
Searching for dark disks
TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
Searching for dark disks
TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
Halo shapes
TeVPA 2017, Columbus, 10 August 2017
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Nassim Bozorgnia
Halo shapes
TeVPA 2017, Columbus, 10 August 2017