Dark Matter halo response to gas inflows and outflows - Aaron A. Dutton New York University Abu Dhabi
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Dark Matter halo response to
gas inflows and outflows
Aaron A. Dutton
New York University Abu Dhabi
15th Potsdam Thinkshop - September 2018
The NIHAO team and collaborators
• Andrea V. Macciò (X) • Xi Kang
• Chris Brook
• Aaron A. Dutton (V, IX, XII, XVII)
• Camilla Penzo
• Liang Wang (I, VII)
• Ben Keller
• Greg S. Stinson (III)
• James Wadsley
• Aura Obreja (VI, XVI) • Jonas Frings
• Tobias Buck (XIII, XV) • Avishai Dekel
• Thales A. Gutcke (VIII) • Rosa Domínguez-Tenreiro
• Gian Luigi Granato
• Arianna Di Cintio (XI)
• Jacob Herpich
• Iryna Butsky (II)
• Jeremy D. Bradford
• Edouard Tollet (IV)
• Tom R. Quinn
• Isabel M. Santos-Santos (XIV) • Ben Moster
• Silviu M. Udrescu • Glenn van de Ven
• Marvin Blank • Ling Zhu
Cold Dark Matter works on large scales
4
orders of
magnitude
in scale
Tegmark et al 2004
Cold Dark Matter
10 S. failseton
Garrison-Kimmel al. small scales
Circular Velocity [km s-1]
Radius [kpc]
Figure 7. Plotted are the rotation curves for all halos identified Figure 8. The distribu
as massive failures around Douglas, both within 300 kpc (black each of twenty paired h
lines) and in the Local Field surrounding it (light blue lines), bining results from Figu
Garrison-Kimmel, Boylan-Kolchin, Bullock, Kirby 2014
along with constraints on the dwarf galaxies in each region (black within 300 kpc of the M
squares denote MW satellites and open light blue squares indicate The exact number of ma
Cold Dark Matter fails on small scales
Moore et al. 1994, Flores & Primack 1994, de Blok et al. 2001, 2008, …
Discrepancy: Factor ~2 in velocity factor ~ 4 in mass
Circular Velocity [km s-1]
APOSTLE
hydro
simulations
4.6 kpc
Radius [kpc]
Figure 1. Rotation curves of IC 2574 (filled circles) and of the sim-
Oman et al. 2015
ulated galaxy DG1 (open circles), taken from Oh et al. (2011). The
Cold Dark Matter works on small scales
SN driven gas outflows can expand the dark matter halo
e.g.,
8 Navarro, Eke, Frenket1996;
I. Santos-Santos al. Read & Gilmore 2005; Mashchenko et al. 2006, 2008; Governato et al. 2010;
Pontzen & Governato 2012; Teyssier et al. 2013; Di Cintio et al. 2014a,b; Chan et al. 2015; Trujillo-Gomez et al. 2015
NIHAO XIVcurves- Santos-Santos
Figure 5. Rotation et al.to that2018
of galaxies IC 2574 and UGC05750 compared - see
of their most poster
similar NIHAO counterpart. For NIHAO galaxies we show
the DM-only circular velocity, the spherical circular velocity, and the true circular velocity. In this last case, the agreement with observed data is remarkable,
showing that the formation of extremely cored dwarf galaxies is indeed possible within a ⇤CDM cosmology, and highlighting the importance of properly
What determines how Galaxy Formation modifies the
Dark Matter distribution in LCDM simulations?
Mstar / Mhalo n
Star Formation Efficiency Star Formation Threshold
Toy Model
Consider a shell of radius ri and mass Mi
Adiabatic Inflow Contraction
(Blumenthal+1986)
Impulsive Outflow Expansion
1 cycle
N cycles
NIHAO IX - Dutton et al. 2016bToy Model
N cycles β=1 rf/ri = (1 -2f +f2)N/ (1-2f)N
Net Expansion
rf/ri = 1 + N f2 + O(f3)
• Need many cycles, with f≳0.1 to generate significant expansion
• If outflow events are small, then halo cannot expand much
NIHAO IX - Dutton et al. 2016bHalo Response depends on Star Formation Efficiency
Di Cintio et al. 2014a, MaGICC simulations (Stinson et al. 2013)
inner DM slope: α
log Mstar/MhaloHalo Response depends on Star Formation Efficiency
Tollet et al. 2016, MNRAS, 456, 3542Halo Response depends on Star Formation Efficiency
Di Cintio et al. 2014, Chan et al. 2015, Tollet et al. 2016
Figure 13
Bullock & Boylan-Kolchin 2017
The impact of baryonic feedback on the inner profiles of dark matter halos. Plotted is the innerStar Formation Threshold is a common sub-grid
parameter in galaxy formation simulations
Kravtsov n(σ)
APOSTLE /
EAGLE n(Z) Teyssier13
ILLUSTRIS Governato12
AURIGA VELA NIHAO FIRE
0.01 0.1 1 10 100 103 104 105
GMC GMC cores
Hydrogen Density / cm3Re-simulate 20 NIHAO
haloes with three
SF thresholds
n=10,1,0.1 nH cm-3Stellar Mass vs Halo Mass
Abundance Matching
Moster et al. 2018
re-calibrated
efficiency
for n=0.1
NIHAO XIX - Dutton et al. 2018 in prepEnclosed Dark Matter Density Profiles
measure
slope between
1 and 2% of R200
measure
mass ratio at
1% of R200
Agrees with
APOSTLE
EAGLE
NIHAO XIX - Dutton et al. 2018 in prepHalo Response depends on (Mstar/Mhalo, n)
n=10 DMO n=1 n=0.1
NIHAO XIX - Dutton et al. 2018 in prepTBTF problem for field Dwarf Galaxies
106 < Mstar < 108
D > 500 kpc
from MW
NIHAO XIX - Dutton et al. 2018 in prepTBTF problem for field Dwarf Galaxies
106 < Mstar < 108
D > 500 kpc
CDM dies CDM dies from MW
CDM dies CDM lives
NIHAO XIX - Dutton et al. 2018 in prepHow do we test which SF threshold is most realistic?
n=10
Re-simulate 20 NIHAO
haloes with three
SF thresholds
n=10,1,0.1 nH cm-3
n=0.1 n=1Higher SF threshold gives more bursty SFH
200 Myr 5 MyrScatter in SFR - Mstar Relation
Redshift:
z107
SF thresholdSummary
• Low threshold star formation (n≤1) EAGLE / APOSTLE /
ILLUSTRIS produces cuspy haloes ( CDM fails!)
• High threshold star formation (n≥10) NIHAO/FIRE produces
expanded haloes when 0.001 < Mstar/Mhalo < 0.01 (CDM ok)
• Field galaxies in LG with Mstar ~ 107 favor high threshold
(Need more observations to improve statistics)
• High threshold yields 2x larger scatter in sSFR measured
over 5 Myr timescale. Testable with Halpha?You can also read
