CONSTRAINING THE NATURE OF DARK MATTER WITH SUBSTRUCTURE LENSING: - - PowerPoint PPT Presentation
CONSTRAINING THE NATURE OF DARK MATTER WITH SUBSTRUCTURE LENSING: PREDICTIONS FROM THEORY AND SIMULATIONS Giulia Despali Simona Vegetti Elisa Ritondale MPA - Garching Simon White Carlo Giocoli Mark Lovell Mark Vogelsberger Martin Sparre
MPA - Garching
Simona Vegetti Elisa Ritondale Simon White Carlo Giocoli Mark Lovell Mark Vogelsberger Martin Sparre Jesús Zavala Frank van den Bosch Miramare 02.07.2018
MPA - Garching
Simona Vegetti Elisa Ritondale Simon White Carlo Giocoli Mark Lovell Mark Vogelsberger Martin Sparre Jesús Zavala Frank van den Bosch Miramare 02.07.2018
(Despali et al. 2018) how many LOS haloes we expect vs substructures in the main lens predictions for CDM vs WDM (Despali, Lovell, Vegetti et al. in prep.) (Despali, Sparre, Vogelsberger, Zavala, Vegetti et al in prep.) subhalo counts from sterile neutrino WDM zoom simulations subhalo profiles, distribution and lensing power spectrum impact of SIDM on the main halo properties different distribution of Einstein rings? subhalo counts and profiles …see Elisa’ s talk!
PREDICTIONS
(Despali et al. 2018)
NLOS = Z zS Z Mmax
MLOW (z)
n(m, z)dmdV dz dz lensing is sensitive to the whole mass distribution between the observer and the source
PREDICTIONS
(Despali et al. 2018)
NLOS = Z zS Z Mmax
MLOW (z)
n(m, z)dmdV dz dz lensing is sensitive to the whole mass distribution between the observer and the source
“EQUIVALENT LINE-OF-SIGHT” used to rescale the sensitivity function at z ≠ zL
log Mvir(z) = (0.41x + 0.57x2 + 0.9x3)
PREDICTIONS
(Despali et al. 2018)
nW DM nCDM = (1 + γMhmM −1)β
CDM WDM 3.3keV
PREDICTIONS
(Despali et al. 2018)
CDM WDM 3.3keV current detection limit
nW DM nCDM = (1 + γMhmM −1)β
PREDICTIONS
(Despali et al. 2018)
CDM WDM 3.3keV current detection limit future
nW DM nCDM = (1 + γMhmM −1)β
PREDICTIONS
(Despali et al. 2018)
CDM WDM 3.3keV future
current detection limit
ratio subhaloes/line-of-sight
nW DM nCDM = (1 + γMhmM −1)β
the line-of-sight population dominates
the LOS population dominates and provides cleaner constrains with better sensitivities we’ll be able to discriminate CDM/WDM we need to be careful with mass definitions
SIMULATIONS
2 x 1013 M⦿ 1 x 6 1012 M⦿ 1x 4 1012 M⦿
1 200 k [h/Mpc] 10 100 1000 Δ2 = k3P(k) 107 108 109 1010 1011 1012 1013 MSK [h-1MO
1 10 100 k [h/Mpc]
L6 = 120.0, sin2(2θ) = 8.0x10-13 L6 = 11.2, sin2(2θ) = 2.1x10-11 L6 = 10.0, sin2(2θ) = 3.7x10-11 L6 = 9.0, sin2(2θ) = 8.1x10-11 L6 = 8.0, sin2(2θ) = 2.1x10-10 CDM
z
(Despali, Lovell et al. in prep.)
SIMULATIONS
(Despali, Lovell et al. in prep.) same number of “luminous” satellites - as in Lovell+16 difference in the “dark” population
SIMULATIONS
(Despali, Lovell et al. in prep.)
SIMULATIONS
colder than the equivalent thermal relic WDM model (Despali, Lovell et al. in prep.)
nW DM nCDM = (1 + γMhmM −1)β
“classic” WDM Sterile Neutrinos
the LOS population dominates and provides cleaner constrains with better sensitivities we’ll be able to discriminate CDM/WDM we need to be careful with mass definitions
the properties of the main lens remain similar slightly colder than the equivalent thermal relic models fewer subhaloes
SIMULATIONS
Vogelsberger et al. 2014
(Despali et al. in prep.)
SIMULATIONS
similar subhalo population subhaloes have on average more cored profiles (Despali et al. in prep.) might be degenerate with WDM abundances
SIMULATIONS
the self-interaction influences the main halo profile (Despali et al. in prep.)
SIMULATIONS
(Despali et al. in prep.) the self-interaction influences the main halo profile in the presence of baryons things are more complicated
SIMULATIONS
the self-interaction influences the main halo profile in the presence of baryons things are more complicated (Despali et al. in prep.)
SIMULATIONS
(Despali & Vegetti 2017)
the LOS population dominates and provides cleaner constrains with better sensitivities we’ll be able to discriminate CDM/WDM we need to be careful with mass definitions
the properties of the main lens remain similar slightly colder than the equivalent thermal relic models fewer subhaloes similar subhalo population but more cored sub profiles stronger effect on the main lens properties ..depending on morphological type? ..accretion history? possible different Einstein radii distribution …we need to be careful the baryonic physics effects!