Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
ANNALISA PILLEPICH(UCSC)
with Javiera Guedes, Sijing Shen, Mike Kuhlen, Piero Madau, Lucio Mayer, Simone Callegari, Valery Rashkov
The Eris Project: the effects of baryons on the
subhaloes of MW-like galaxies
Zoom-in simulationN-body/SPH: PKDGRAV/GASOLINE
Halo Finder: Amiga Halo Finder
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
Eris
Dar
k: D
M o
nly Eris: D
M, gas, stars
DM-only Density Field
600 kpc
ErisDark Eris
20 Mpc Eris Recipe:(Guedes et al 2011, ApJ 742, 76)
• radiative cooling (Compton, atomic, low T metallicity-dependent)
• heating from cosmic UV (~ Haardt & Madau 1996)
• Supernova feedback (εSN = 0.8) (Stinson et al. 2006)
• Star Formation: • threshold nSF = 5 atoms/cm3• efficiency εSF = 0.1• IMF: Kroupa et al. 1993
NO AGN feedback
The simulation
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
Eris
Dar
k: D
M o
nly Eris: D
M, gas, stars
DM-only Density Field
Vmax
Eris MWs
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
0.2 0.4 0.6 0.8 1
102
a
Rvi
r (k
pc)
ErisDark: Rvir
= 246.59
Eris: Rvir
= 234.77
0.2 0.4 0.6 0.8 1
108
1010
1012
TOT Mass
a
M (
Msu
n)
TOT DM GAS STARS
0.2 0.4 0.6 0.8 10.08
0.09
0.1
0.11
0.12
0.13
0.14
0.15
0.16
a
f b
Baryon Fraction
ErisDarkEris
ErisDark
Eris
Eris MWs
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
100
101
10210
0
102
104
106
108
1010
R (kpc)
(M
su
n /
kpc
3 )
Eris.00001 at z = 0.0
soft
enin
g
Pow
er:2
003
=~
D
iem
and:
2004
TOTDMGASSTARS
0 10 20 30 40 500
50
100
150
200
250
R (kpc)
V c
irc (
km/s)
Eris.00001 at z = 0.0
TOTDMGASSTARS
Eris MWs
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
100
101
10210
0
102
104
106
108
1010
R (kpc)
(M
su
n /
kpc
3 )
Eris.00001 at z = 0.0
soft
enin
g
Pow
er:2
003
=~
D
iem
and:
2004
TOTDMGASSTARS
0 10 20 30 40 500
50
100
150
200
250
R (kpc)
V c
irc (
km/s)
Eris.00001 at z = 0.0
TOTDMGASSTARS
Eris MWs
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
100
10210
0
102
104
106
108
1010
R (com kpc)
(M
su
n /
kpc
3 )
z = 0.0
3 x
soft
enin
g Pow
er:2
003
=~
Die
man
d:20
04
TOTDMGASSTARS
Convergence Estimate
Eris Dark Low Resolution9.5 10^5 Msun495 pc
> 0.9 kpc~ 8 x softening!
Eris MWs
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
Eris Satellites
0 100 200 300 400 500 600 700 800⌧400
⌧200
0
200
400
Vre
l, M
W (
km/s)
ErisDark590
0 100 200 300 400 500 600 700 800⌧400
⌧200
0
200
400
d MW
(kpc)
Vre
l, M
W (
km/s)
Eris432
0 100 200 300 400 500 600 700 8000
20
40
60
N
z = 0.0
ErisDark: 590Eris: 432
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
Eris Satellites
0 100 200 300 400 500 600 700 800⌧400
⌧200
0
200
400
Vre
l, M
W (
km/s)
ErisDark590
0 100 200 300 400 500 600 700 800⌧400
⌧200
0
200
400
d MW
(kpc)
Vre
l, M
W (
km/s)
Eris432
0 100 200 300 400 500 600 700 8000
20
40
60
N
z = 0.0
ErisDark: 590Eris: 432
• NTOT > 100, AHF Analog pairs by DM particle tracking
• Effective high-res region no further than 850 kpc....
• Many categories of objects!
• Satellite Definition at z=0: - within Rvir at any given z - within Rvir ever
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
10110
0
101
102
103
V max
(km/s)
N (
> V
max)
ErisDark subhalo function at z=0
ErisDark within R200VLII within R200
ErisDark Subhaloes
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
10⌧2
10⌧110
0
101
102
103
V max
/ Vhost max
N (
> V
max/ V
hos
t m
ax)
ErisDark subhalo function at z=0
ErisDark within R200VLII within R200
ErisDark Subhaloes
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
10⌧2
10⌧110
0
101
102
103
relative V max
N (
> r
elat
ive V
max)
ErisDark and VLII at z=0, within R200
V ErisDark max
= 166 km/s; V ErisDark vir
= 117 km/s
V VLII max
= 201 km/s; V VLII vir
= 144 km/s
ErisDark, normalized to V host max
VLII, normalized to V host max
ErisDark, normalized to V host vir
VLII, normalized to V host vir
ErisDark Subhaloes
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
10⌧2
10⌧110
0
101
102
103
relative V max
N (
> r
elat
ive V
max)
ErisDark and VLII at z=0, within R200
V ErisDark max
= 166 km/s; V ErisDark vir
= 117 km/s
V VLII max
= 201 km/s; V VLII vir
= 144 km/s
ErisDark, normalized to V host max
VLII, normalized to V host max
ErisDark, normalized to V host vir
VLII, normalized to V host vir
ErisDark Subhaloes
?!?!? - resolution???- unlucky realization?
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
Excursus: scatter in the subhalo velocity function (I)
Bolshoi Simulation, analyzed with Rockstar by P. Berhoozi(L = 250 Mpc/h, N = 2048^3, m_DM = 1.35 10^8 Msun/h, 1 phys kpc/h)
Typical DM subhalo abundance functions, for cluster-size hosts:
102
100
101
102
103
Vmax
(km/s)
N (
> V
max)
N hosts
= 99
10⌧2
10⌧1
100
101
102
103
Vmax
/V host max
Bolshoi at z=0: 1.58e+14 < M host
<= 2.51e+14 M sun
10⌧2
10⌧1
100
101
102
103
Vmax
/V host vir
μmax μvir= =
Thanks to Joel and Peter
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
101
102
103
10⌧1
100
101
102
103
Vmax
(km/s)
N (
> V
max)
N hosts
= 56
10⌧1
10⌧1
100
101
102
103
Vmax
/V host max
Bolshoi at z=0: 1.45e+14 < M host
<= 1.73e+14 M sun
10⌧1
10⌧1
100
101
102
103
Vmax
/V host vir
101
102
103
10⌧1
100
101
102
103
Vmax
(km/s)
N (
> V
max)
N hosts
= 547
10⌧1
10⌧1
100
101
102
103
Vmax
/V host max
Bolshoi at z=0: 1.54e+13 < M host
<= 1.75e+13 M sun
10⌧1
10⌧1
100
101
102
103
Vmax
/V host vir
101
102
103
10⌧1
100
101
102
103
Vmax
(km/s)
N (
> V
max)
N hosts
= 875
10⌧1
10⌧1
100
101
102
103
Vmax
/V host max
Bolshoi at z=0: 1.95e+12 < M host
<= 2.00e+12 M sun
10⌧1
10⌧1
100
101
102
103
Vmax
/V host vir
Different host-masses:
smaller hosts
Excursus: scatter in the subhalo velocity function (II)
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
101
102
103
10⌧1
100
101
102
103
Vmax
(km/s)
N (
> V
max)
N hosts
= 56
10⌧1
10⌧1
100
101
102
103
Vmax
/V host max
Bolshoi at z=0: 1.45e+14 < M host
<= 1.73e+14 M sun
10⌧1
10⌧1
100
101
102
103
Vmax
/V host vir
101
102
103
10⌧1
100
101
102
103
Vmax
(km/s)
N (
> V
max)
N hosts
= 547
10⌧1
10⌧1
100
101
102
103
Vmax
/V host max
Bolshoi at z=0: 1.54e+13 < M host
<= 1.75e+13 M sun
10⌧1
10⌧1
100
101
102
103
Vmax
/V host vir
101
102
103
10⌧1
100
101
102
103
Vmax
(km/s)
N (
> V
max)
N hosts
= 875
10⌧1
10⌧1
100
101
102
103
Vmax
/V host max
Bolshoi at z=0: 1.95e+12 < M host
<= 2.00e+12 M sun
10⌧1
10⌧1
100
101
102
103
Vmax
/V host vir
Different host-masses:
smaller hosts
Excursus: scatter in the subhalo velocity function (III)
completeness/resolution limit:
where?50 km/s?100 km/s?
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
1012
1013
1014
0
20
40
60
80
100
120
140
160
V max
> 70 km/sV max
> 70 km/sV max
> 70 km/sV max
> 70 km/s
M host
N (
> µ
max)
Subhaloes in Bolshoi at z=0, normalized to Vhostmax
µ
max = 0.08
µ max
= 0.11
µ max
= 0.20
µ max
= 0.31
1012
1013
1014
0
20
40
60
80
100
120
140
160
V max
> 70 km/sV max
> 70 km/sV max
> 70 km/sV max
> 70 km/s
M host
N (
> µ
vir)
Subhaloes in Bolshoi at z=0, normalized to Vhostvir
µ
vir = 0.08
µ vir
= 0.11
µ vir
= 0.20
µ vir
= 0.31
Excursus: scatter in the subhalo velocity function (I)
Sectioning the subhalo abundance functions at different subhalo relative sizes...
Excursus: scatter in the subhalo velocity function (IV)
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
Excursus: scatter in the subhalo velocity function (V)
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
Excursus: scatter in the subhalo velocity function (V)
??? MW and subhaloes beyond μ~0.1 ???
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
Excursus: scatter in the subhalo velocity function (V)
MW and subhaloes beyond μ~0.1
+- ~50%
+- ~66%
Ishiyama:2009
...also Wang:2012
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
10⌧4
10⌧310
3
104
105
106
107
M hos
t v
ir
dN/d
M
z = 0
MW Satellites
ErisDark: M TOT
Eris: M TOT
Eris: M DM
10⌧4
10⌧3
0
1
2
3
4
5
M/M host vir
Eri
sDar
k/E
ris
10⌧2
10⌧110
0
101
102
103
N(
> V
max/V
hos
t v
ir)
z = 0
MW Satellites ErisDark: V TOT
max
Eris: V TOT max
Eris: V DM max
Eris: V GAS max
Eris: V STARS max
10⌧2
10⌧10
1
2
3
V max
/V host vir
Eri
sDar
k/E
ris
Satellites Abundances
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
10⌧2
10⌧110
0
101
102
103
N(
> V
max/V
hos
t v
ir)
z = 0
MW Satellites ErisDark: V TOT
max
Eris: V TOT max
Eris: V DM max
Eris: V GAS max
Eris: V STARS max
10⌧2
10⌧10
1
2
3
V max
/V host vir
Eri
sDar
k/E
ris
Satellites Abundances
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
10⌧2
10⌧110
0
101
102
103
N(
> V
max/V
hos
t v
ir)
z = 0
MW Satellites ErisDark: V TOT
max
Eris: V TOT max
Eris: V DM max
Eris: V GAS max
Eris: V STARS max
10⌧2
10⌧10
1
2
3
V max
/V host vir
Eri
sDar
k/E
ris
Satellites Abundances
see Zolotov&co talks and papers:
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
10⌧2
10⌧110
0
101
102
103
N(
> V
max/V
hos
t v
ir)
z = 0
MW Satellites ErisDark: V TOT
max
Eris: V TOT max
Eris: V DM max
Eris: V GAS max
Eris: V STARS max
10⌧2
10⌧10
1
2
3
V max
/V host vir
Eri
sDar
k/E
ris
Satellites Abundances
Mayer et al. in preparation.
- The most massive objects undergo strongest stripping- The amount of stripped material depends on the slope of the inner densities, on the orbits, on the distance of the pericenter, ... - Haloes which are massive and with flatter inner density profiles are more likely to get completely destroyed, as the dependence of tidal shock on halo mass is stronger than linear!
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
10⌧2
10⌧110
0
101
102
103
N(
> V
max/V
hos
t v
ir)
z = 0
MW Satellites ErisDark: V TOT
max
Eris: V TOT max
Eris: V DM max
Eris: V GAS max
Eris: V STARS max
10⌧2
10⌧10
1
2
3
V max
/V host vir
Eri
sDar
k/E
ris
Satellites Abundances
Baryons not always produce reduced inner densities and shallower density profiles....
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
10⌧2
10⌧110
0
101
102
103
N(
> V
max/V
hos
t v
ir)
z = 0
MW Satellites ErisDark: V TOT
max
Eris: V TOT max
Eris: V DM max
Eris: V GAS max
Eris: V STARS max
10⌧2
10⌧10
1
2
3
V max
/V host vir
Eri
sDar
k/E
ris
Eris luminous satellites
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
0.5 1 1.5 20
10
20
30
40
50
R (com kpc)
V c
irc (
km/s)
Eris.00049 at z = 0.0
Pow
er:2
003 47, 29.9 km/s , 5.0 kpc
49, 25.8 km/s , 4.7 kpc
TOTDMGASSTARS
10⌧2
10⌧110
0
101
102
103
N(
> V
max/V
hos
t v
ir)
z = 0
MW Satellites ErisDark: V TOT
max
Eris: V TOT max
Eris: V DM max
Eris: V GAS max
Eris: V STARS max
10⌧2
10⌧10
1
2
3
V max
/V host vir
Eri
sDar
k/E
ris
Eris luminous satellites
MTOT = 2e9 MsunMstellar ~ 1e7 MsunMass loss ~ 50 %z infall = 0.99dMW = 215 kpc
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
0.5 1 1.5 20
10
20
30
40
50
R (com kpc)
V c
irc (
km/s)
Eris.00021 at z = 0.0
Pow
er:2
003 580, 15.8 km/s , 2.2 kpc
21, 32.8 km/s , 0.4 kpc
TOTDMGASSTARS
10⌧2
10⌧110
0
101
102
103
N(
> V
max/V
hos
t v
ir)
z = 0
MW Satellites ErisDark: V TOT
max
Eris: V TOT max
Eris: V DM max
Eris: V GAS max
Eris: V STARS max
10⌧2
10⌧10
1
2
3
V max
/V host vir
Eri
sDar
k/E
ris
Eris luminous satellites
MTOT = 3.7e8 MsunMstellar ~ 1.8e8 MsunMass loss ~ 96 %z infall = 1.2dMW = 34 kpc
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
0.5 1 1.5 20
10
20
30
40
50
R (com kpc)
V c
irc (
km/s)
Eris.00031 at z = 0.0
Pow
er:2
003 486, 20.9 km/s , 1.7 kpc
31, 31.7 km/s , 0.5 kpc
TOTDMGASSTARS
10⌧2
10⌧110
0
101
102
103
N(
> V
max/V
hos
t v
ir)
z = 0
MW Satellites ErisDark: V TOT
max
Eris: V TOT max
Eris: V DM max
Eris: V GAS max
Eris: V STARS max
10⌧2
10⌧10
1
2
3
V max
/V host vir
Eri
sDar
k/E
ris
Eris luminous satellites
MTOT = 3.1e8 MsunMstellar ~ 1.6e8 MsunMass loss ~ 97 %z infall = 1.8dMW = 30 kpc
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
10⌧2
10⌧110
0
101
102
103
N(
> V
max/V
hos
t v
ir)
z = 0
MW Satellites ErisDark: V TOT
max
Eris: V TOT max
Eris: V DM max
Eris: V GAS max
Eris: V STARS max
10⌧2
10⌧10
1
2
3
V max
/V host vir
Eri
sDar
k/E
ris
M32
Eris luminous satellites
ref. Toloba:2011
e.g: M32 in Andromeda
e.g: all past SPH satellites
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
Top10 satellites in ErisDark (Vmax selected)
0 1 20
10
20
30
40
50
R (kpc)
47, 29.9 km/s 48, 25.8 km/s
Vci
rc (
km/s)
0 1 20
10
20
30
40
50
R (kpc)
160, 15.1 km/s 65, 16.9 km/s
0 1 20
10
20
30
40
50
R (kpc)
176, 19.9 km/s 156, 17.4 km/s
0 1 20
10
20
30
40
50
R (kpc)
268, 15.0 km/s 282, 14.1 km/s
0 1 20
10
20
30
40
50
R (kpc)
283, 14.5 km/s 344, 11.9 km/s
0 1 20
10
20
30
40
50
R (kpc)
340, 18.7 km/s 354, 16.3 km/s
Vci
rc (
km/s)
0 1 20
10
20
30
40
50
R (kpc)
403, 18.7 km/s 463, 15.5 km/s
0 1 20
10
20
30
40
50
R (kpc)
458, 16.6 km/s 867, 12.0 km/s
0 1 20
10
20
30
40
50
R (kpc)
486, 20.9 km/s 31, 31.6 km/s
0 1 20
10
20
30
40
50
R (kpc)
582, 15.8 km/s 21, 33.0 km/s
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
0 1 20
10
20
30
40
50
R (kpc)
21, 33.0 km/s 582, 15.8 km/s
Vci
rc (
km/s)
0 1 20
10
20
30
40
50
R (kpc)
31, 31.6 km/s 486, 20.9 km/s
0 1 20
10
20
30
40
50
R (kpc)
48, 25.8 km/s 47, 29.9 km/s
0 1 20
10
20
30
40
50
R (kpc)
168, 16.3 km/s 1334, 11.6 km/s
0 1 20
10
20
30
40
50
R (kpc)
194, 14.0 km/s 306, 15.8 km/s
0 1 20
10
20
30
40
50
R (kpc)
260, 12.2 km/s 1, 166.1 km/s
Vci
rc (
km/s)
0 1 20
10
20
30
40
50
R (kpc)
282, 14.1 km/s 268, 15.0 km/s
0 1 20
10
20
30
40
50
R (kpc)
354, 16.3 km/s 340, 18.7 km/s
0 1 20
10
20
30
40
50
R (kpc)
367, 16.4 km/s 627, 15.9 km/s
0 1 20
10
20
30
40
50
R (kpc)
425, 12.1 km/s 743, 12.4 km/s
Top10 satellites in Eris (Vmax selected)
Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012
Conclusions
• ErisDark seems to be a subhalo-poor realization of a (low-mass) MW
• Even with Eris, resolution limits lie in ambush (!!!)
• The MW subhalo cumulative Vmax function at z=0 is suppressed with the presence of baryons
• Yet, in Eris we have an ankle at the high luminosity end of the subhalo cumulative Vmax function at z=0
• The interpretation of such decrement and ankle is not at all straightforward, even modulo the physics recipe
• The histories of the satellites must be studied in details: i.e. we have to understand the different tidal responses
• of the different categories of satellites falling in the MW (dark satellites vs baryonic satellites, with flatter/cuspier inner profiles, different orbits...)
• in relation to the different hosts in which they are falling in (disk vs no disk, different host shapes, thus different orbits)