Cores - usp conference

Transcrição

Introduction | Simulations | Cores | Bulges| Conclusions
Sao Paulo Feb 2013
Cusps, Cores & CDM?
F. Governato, A.Pontzen, C.Christensen, F.Munshi, A.Brooks, A.Zolotov
& the N-Body Shop collaboration
segunda-feira, 11 de fevereiro de 13
Introduction | Simulations | Cores | Bulges| Conclusions
Sao Paulo Feb 2013
Cusps, Cores & CDM?
F. Governato, A.Pontzen, C.Christensen, F.Munshi, A.Brooks, A.Zolotov
& the N-Body Shop collaboration
Introduction| Simulations| Cores| Bulges | Conclusions
Bulgeless, Cored Disk Galaxies in a CDM Cosmology: End the Small Scales Crisis
Introduction | Simulations | Cores | Bulges | Conclusions
Outline of This Talk
Understand how out(in)flows shape
the central mass distribution of galaxies
using cosmological hydro simulations
Make predictions of DM Cores’
properties vs galaxy stellar mass
Is alternative DM (WDM, SIDM) needed?
Pontzen & Governato
arXiv:1210.1849/MNRAS 2013
Dwarf
MW
Cluster
M200 = 2.8 x 1010 M☉
r200 = 98 kpc
M200 = 8.0 x 1011 M☉
r200 = 301 kpc
M200 = 8.7 x 1013 M☉
r200 = 1.43 Mpc
Pontzen & Governato
arXiv:1210.1849/MNRAS 2013
Introduction| Simulations| Cores| Bulges| Conclusion
The Substructure Overabundance Problem
.
Moore, Ghigna Governato...1998
Outflows, Bulges and Cores
log ρDM
d log ρDM / dr = –1
Dwarf
Galaxies
“NFW”
log r
log ρDM
~1 kpc
exotic
dark
matter?
Dwarf
Galaxies
“NFW”
log r
Dwarf
Galaxies
Oh et al
2011, AJ
Dwarf
Galaxies
Oh et al
2011, AJ
Dwarf
Galaxies
Oh et al
2011, AJ
Introduction| Simulations | Cores| Bulges| Conclusions
The Problem with Dwarfs (3): Rmax vs Vmax - Boylan
Kolchin..Bullock et al ‘11
The Angular Momentum Catastrophe
Maller & Dekel
Outflows, Cores & Bulges
EARLY SIMULATIONS ANGULAR MOMENTUM
PROBLEM
NO FEEDBACK
P(n)
Introduction
| Simulations | Cores| Bulges| Conclusions
The Angular Momentum Distribution of Disk Dominated
Galaxies
p(s)
vdBosch 01, Bullock et al
01.
The angular momentum distribution of the stars in
observed bulgeless galaxies is different from the one
predicted for CDM Halos
What happened to the low J gas?
s=J/<Jtot>
A unique solution for all these problems?
July 1, 2011
‘Baryonic physics’, Star Formation and GAS OUTFLOWS
M82
July 1, 2011
Benson 06
Introduction |
Simulations | Cores | Conclusions
“Resolving” Star Formation Regions
High Threshold
Low Threshold
2009- Feedback becomes more efficient
2011- H2 fraction = replaces ‘high threshold’
see also: Ceverino & Klypin (2008), Robertson & Kravtsov (2008), Tasker & Bryan (2008)
Gas Outflows with Thermal Feedback:
Temperature map
High z
Pontzen & Governato ‘11
July 1, 2011
Introduction|
Simulations | Cores | Bulges | Conclusions
Low z
Movie: the Formation of a bulgeless disk galaxy with a DM core.
Light green: gas. Red and blue: stars. The frame is 50 kpc
across.
Only 2.5% of gas turns into stars. 70% is ejected.
July 20, 2011
Introduction| Simulations | Cores | Bulges | Conclusions
1- NUMERICAL SIMULATIONS
G+ 2010
July 1, 2011
Introduction|
Simulations | Cores | Bulges| Conclusions
Simulating the ‘perfect’ dwarf galaxy.
•Exponential stellar disk Rd =
1
kpc
•Gas rich: HI/stars mass ratio ~ 2
•Thin disk b/a
•Vc = 55 km/sec
•blue colors g-r = 0.5
• SFH bursty SFR = 0.01 sol.
masses/yr
•just your regular dwarf...
Governato+ 2010
Aug, 2011
SOLVING THE ANGULAR MOMENTUM ‘CATASTROPHE’
P(n)
SOLVING THE ANGULAR MOMENTUM ‘CATASTROPHE’
P(n)
G+10, CBrook et al.
11
bound
gas
expelled gas
Brook+ 2011
cf Binney 01, van den Bosch 01
Introduction | Simulations |
Cores | Bulges | Conclusions
Selective low angular momentum
gas removal
as SF peaks at high-z
in the halos that will merger to form
the center of present day galaxies.
C.Brook+ 2011
Outflows form DM Cores
July 1, 2011
Introduction| Simulations |
GASOLINE + H2: Focus on where/when do
stars form
(Christensen+ ‘12, Stinson+‘06)...
•Star Formation regulated by local H2 fraction
•explicit metal dependent H2 formation
• H2 and HI shielding
• H2 destruction by Lyman-Werner radiation
•SN energy as thermal energy+cooling shutoff
• 5-15 million particles, Spatial resolution
50-150pc
•
16 FIELD GALAXIES, DWARFS to L*, RANGE OF SPIN/FORMATION TIMES
Outflows, Cores and Bulges
Guedes+11,Shen+12
July 1, 2011
Artificial Images: HI, optical, IR. Kinematics, Photometry
I
MODELS VS OBSERVATIONS -
3 - COMPARING WITH OBSERVATIONS
Oh et al 2011, AJ
July 20, 2011
Outflows, Bulges & Cores
But do we know how it works?
July 1, 2011
Gas Outflows: Thermal Feedback & Buoyant
Bubbles
Virial Radius
Cosmological Dwarf Galaxy
July 1, 2011
Buoyancy
Redshift
4.2
3.63.3
3.33.0
3.02.72.7 2.4 2.4 2.1 2.1
4.2 3.6
88
10
10
Mgas(<r)/M⊙◉☉
1.0
10
1077
0.1
66
10
10
1.5
1.5
Pontzen & Governato 2012
2.0
2.0
2.0
2.5
2.5
2.5
t/Gyr
3.0
3.0 3.0
3.5
Redshift
4.2
3.63.3
3.33.0
3.02.72.7 2.4 2.4 2.1 2.1
4.2 3.6
88
10
10
Mgas(<r)/M⊙◉☉
1.0
200pc
10
1077
0.1
66
10
10
1.5
1.5
2.0
2.0
2.0
2.5
2.5
2.5
t/Gyr
3.0
3.0 3.0
3.5
Redshift
4.2
3.63.3
3.33.0
3.02.72.7 2.4 2.4 2.1 2.1
4.2 3.6
88
10
10
500pc
Mgas(<r)/M⊙◉☉
1.0
200pc
10
1077
0.1
66
10
10
1.5
1.5
2.0
2.0
2.0
2.5
2.5
2.5
t/Gyr
3.0
3.0 3.0
3.5
Mgas(<r)/M⊙◉☉
Redshift
4.2
3.63.3
3.33.0
3.02.72.7 2.4 2.4 2.1 2.1
4.2 3.6
88
10
10
1 kpc
1.0
500pc
200pc
10
1077
0.1
66
10
10
1.5
1.5
2.0
2.0
2.0
2.5
2.5
2.5
t/Gyr
3.0
3.0 3.0
3.5
Redshift
4.2
3.63.3
3.33.0
3.02.72.7 2.4 2.4 2.1 2.1
4.2 3.6
88
10
10
1 kpc
10
1077
ρ/mp cm–3
Mgas(<r)/M⊙◉☉
1.0
1.5
500pc
0.0
200pc
–1.5
10 kpc
–3.0
0.1
66
10
10
1.5
1.5
2.0
2.0
2.0
2.5
2.5
2.5
t/Gyr
3.0
3.0 3.0
3.5
Mgas(<r)/M⊙◉☉
Redshift
4.2
3.63.3
3.33.0
3.02.72.7 2.4 2.4 2.1 2.1
4.2 3.6
88
10
10
1 kpc
1.0
500pc
200pc
10
1077
0.1
66
10
10
1.5
1.5
2.0
2.0
2.0
2.5
2.5
2.5
t/Gyr
3.0
3.0 3.0
3.5
Cores | Bulges| Conclusions
When do DM cores
form?
• The central density
DM decreases
as outflows transfer energy to the
DM.
• This process is most active at 4
> z > 1 as SF peaks in the galaxy
progenitors.
z=4
Introduction| Simulations |Cores Bulges| Conclusions
2- ANALYTICAL MODEL: Non adiabatic, repeated transfer energy to the
DM.
High-quality multi-λ data
Cores (THINGS HI, Spitzer 3.6μm
and optical data) significantly
reduce the observational
uncertainties and allow us to
derive reliable dark matter
density profiles.
Cusps
see Pontzen & Governato
2012, MNRAS
The Pontzen Scheme
Introduction| Simulations |Cores Bulges| Conclusions
2- ANALYTICAL MODEL: Non adiabatic, repeated transfer energy to the
DM.
High-quality multi-λ data
Cores (THINGS HI, Spitzer 3.6μm
and optical data) significantly
reduce the observational
uncertainties and allow us to
derive reliable dark matter
density profiles.
Cusps
see Pontzen & Governato
2012, MNRAS
The Pontzen Scheme
Flores & Primack 1994
Navarro, Eke, Frenk 1996
Gnedin & Zhao 2002
Read & Gilmore 2005
Mashchenko et al 2006/2008
El Zant 2001/2004
Weinberg & Katz 2002
Flores & Primack 1994
Navarro, Eke, Frenk 1996
Gnedin & Zhao 2002
Weinberg
Katz 2002
Read &
Gilmore&2005
Mashchenko et al 2006/2008
El Zant 2001/2004
Weinberg & Katz 2002
Subject one | Subject two | Subject three | Subject four | Conclusion
The New Sample of Galaxies
•16 field halos from MWs to ultra faints
•full cosmological context/carried to =0
•Range of halo spins and formation times
• up to 20 million particles per halo
•Force resolution 50-150pc
•Optical and HI ‘observations’ for each galaxy
4 ‘Eris’, 2 galaxies with Vpeak ~ 100 km/sec, several SMCs and dwarfs
July 1, 2011
The Slope of Dark Matter Halos: the Effect of Gas Outflows
the typical high-z
galaxy seen by HST
should have cores!
Slope
Outflows in ultra faint
galaxies are not
sufficient to turn
cusps into cores
Stellar Mass
to be submitted in Aug 2011
Feedback from SMBHs: DM Cores in
Galaxy Clusters
Martizzi, Teyssier et al 2012
Cores in L*
Galaxies
Maccio’ et al 2012
Introduction | Simulations |
Cores | Conclusions
DM SLOPE CHANGES WITH HALO MASS
THINGS
because SF
varies with
mass
Galaxies in the
THINGS survey have
average α~-0.3
Lower mass galaxies
do not undergo
repeated bursts of SF;
retain cusps
Governato, Zolotov, Pontzen, AB et al., in prep
So it’s all done?
July 1, 2011
Cores
| Bulges| Conclusions
STAR FORMATION EFFICIENCY: MODELS VS OBSERVATIONS II
Moster 2012
Faint Dwarfs
‘Eris-like’
Munshi,FG+ 2012
New SPH: Better KH Instabilities. No more
“Blobs”.
ENZO (PPM)
SPH!old
• Satellites
• Ram stripping
• Outflows
July 20, 2011
SPH!NEW
1.25
! KH
2.5
! KH
3.75
! KH
Energy Budget.
Enough to form cores?
Penarrubia+ 2012
July 1, 2011
the typical high-z
galaxy seen by HST
should have cores!
Slope
galaxies are not
sufficient to turn
cusps into cores
Stellar Mass
FG+ 2012
the typical high-z
galaxy seen by HST
should have cores!
Slope
galaxies are not
sufficient to turn
cusps into cores
Stellar Mass
FG+ 2012
the typical high-z
galaxy seen by HST
should have cores!
Slope
galaxies are not
sufficient to turn
cusps into cores
Stellar Mass
FG+ 2012
over the same interval (Paper I, Section 10). The width of the bands indicates the uncertainty, including bo
for isotropic models and a systematic component estimated by taking aniso = ±0.2 (Section 4.3). Arrows
indicate three-dimensional half-light radius rh of the BCG.
Clusters
4
NFW
5
Flat prior
Probability density
Probability density
4
3
2
1
0
0.0
0.2
0.4 0.6 0.8 1.0 1.2
gNFW β (DM inner slope)
1.4
3
2
1
0
−0.5
0.0
0.5
1.0
Newman+
cNFW log rc
ApJ submitted,
Fig. 4.— Marginalized posterior probability densities for the gNFW inner slope 1209.1392
(left) and the cNFW core
lines show joint constraints on the mean. Colors follow Figure 2. Each curve is normalized to integrate to
(Paper I, Table 7) are flat in log rs and b and therefore not in log rcore = log rs /b over the whole plotted ra
Clusters
4
NFW
5
Flat prior
Probability density
Probability density
4
3
2
1
0
0.0
0.2
0.4 0.6 0.8 1.0 1.2
1.4
3
2
1
0
−0.5
0.0
0.5
1.0
Newman+
cNFW log rc
ApJ submitted,
Clusters
4
NFW
5
Flat prior
Probability density
Probability density
4
3
2
1
0
0.0
0.2
0.4 0.6 0.8 1.0 1.2
1.4
3
2
1
0
−0.5
0.0
0.5
1.0
Newman+
cNFW log rc
ApJ submitted,
Pontzen & Governato
arXiv:1210.1849
Dwarf
MW
Cluster
M200 = 2.8 x 1010 M☉
r200 = 98 kpc
M200 = 8.0 x 1011 M☉
r200 = 301 kpc
M200 = 8.7 x 1013 M☉
r200 = 1.43 Mpc
Pontzen & Governato
arXiv:1210.1849
WDM?
CORES/SUBSTRUCTURE/BULGELESS
Lovell et al. 2011
SIDM
VOGELSBERGER ’12, ROCHA ’12
July 1, 2011
SIDM
VOGELSBERGER ’12, ROCHA ’12
July 1, 2011
Indirect DM detection: CDM DM-only vs CDM+baryons
The big question:
The big question:
Can we tell the difference
between exotic dark matter
and the effects of baryons?
What’s Next? The Next Generation Simulations
1.
BETTER HYDRO SOLVERS
2.
SCALING TO N>1000 CORES
3. FEEDBACK FROM RADIATION PRESSURE
Introduction| Simulations| Cores| Bulges|
Conclusions
Conclusions
OUTFLOWS REMOVE LOW J
GAS
CREATE DARK MATTER
CORES.
SIMULATIONS MATCH
OBSERVATIONS: CORES+SF
EFFICIENCY
NEW SPH
SCALING TO 1000S CORES
FEEDBACK FROM YOUNG
STARS
TEST ALTERNATIVE DM WITH
G10+,BROOK+11, PG12
BARYON PHYSICS
OH+11,G+12
AS WE SPEAK.
STARTING EARLY 2013
Introduction | Simulations | Cores| Bulges | Conclusions
The Luminosity - Size relation of CDM galaxies
(A.Brooks
2011).
et al ApJ
from artificial images were analyzed with
GALFIT.
The Baryonic Tully Fisher relation
Christensen+ et al 2012 in prep
July 20, 2011
Still Gas Rich After All These Outflows
July 1, 2011
More Worries: Resolution
Low Density
SF threshold
High Res
α=-1.5
Hi Density- Low Res 1/64
α=-0.6
Hi Density - High Res
G+10, supplemental
material
July 1, 2011
Cores
| Bulges| Conclusions
The Star Formation Histories of dwarf and disk
galaxies
Aug
2011
Introduction| Simulations | Cores|
Bulges
| Conclusions
Why do we need H2 (and metal) cooling?
DM Density
Using Metal Dependent
Cooling increases the
amount of stars formed
at high-z (in bulges)
Lower Dark
Matter
and stellar
densities due
to enhanced
outflows
H2 cooling and H2 driven Star Formation creates
Radius
a
clumpier/more realistic ISM and stronger
outflows, decreasing the central stellar and DM
densities.
July 1, 2011

Cores - usp conference

Transcrição

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