[PPT] - The Eris Project: the effects of baryons on the subhaloes of PowerPoint Presentation

SLIDE 1

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 simulation N-body/SPH: PKDGRAV/GASOLINE Halo Finder: Amiga Halo Finder

SLIDE 2

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

ErisDark: DM only Eris: DM, 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

SLIDE 3

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

ErisDark: DM only Eris: DM, gas, stars

DM-only Density Field

Vmax

Eris MWs

SLIDE 4

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012 0.2 0.4 0.6 0.8 1 10

2

a

Rvir (kpc)

ErisDark: Rvir = 246.59 Eris: Rvir = 234.77

0.2 0.4 0.6 0.8 1 10

8

10

12

TOT Mass

a

M (Msun)

TOT DM GAS STARS

0.2 0.4 0.6 0.8 1 0.08 0.09 0.1 0.11 0.12 0.13 0.14 0.15 0.16 a

f b

Baryon Fraction

ErisDark Eris

Eris MWs

SLIDE 5

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10 10

1

10

2

10 10

2

10

4

10

6

10

8

10

R (kpc)

(M sun / kpc3)

Eris.00001 at z = 0.0

softening Power:2003 =~ Diemand:2004

TOT DM GAS STARS 10 20 30 40 50 50 100 150 200 250 R (kpc)

V circ (km/s)

Eris.00001 at z = 0.0

TOT DM GAS STARS

Eris MWs

SLIDE 6

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10 10

1

10

2

10 10

2

10

4

10

6

10

8

10

R (kpc)

(M sun / kpc3)

Eris.00001 at z = 0.0

softening Power:2003 =~ Diemand:2004

TOT DM GAS STARS 10 20 30 40 50 50 100 150 200 250 R (kpc)

V circ (km/s)

Eris.00001 at z = 0.0

TOT DM GAS STARS

Eris MWs

SLIDE 7

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012 10 10

2

10 10

2

10

4

10

6

10

8

10

R (com kpc)

(M sun / kpc3)

z = 0.0

3 x softening Power:2003 =~ Diemand:2004

TOT DM GAS STARS

Convergence Estimate

Eris Dark Low Resolution 9.5 10^5 Msun 495 pc

> 0.9 kpc ~ 8 x softening!

Eris MWs

SLIDE 8

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

Eris Satellites

100 200 300 400 500 600 700 800 −400 −200 200 400

Vrel, MW (km/s)

ErisDark 590

100 200 300 400 500 600 700 800 −400 −200 200 400 d MW (kpc)

Vrel, MW (km/s)

Eris 432

100 200 300 400 500 600 700 800 20 40 60 N z = 0.0 ErisDark: 590 Eris: 432

SLIDE 9

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

Eris Satellites

100 200 300 400 500 600 700 800 −400 −200 200 400

Vrel, MW (km/s)

ErisDark 590

100 200 300 400 500 600 700 800 −400 −200 200 400 d MW (kpc)

Vrel, MW (km/s)

Eris 432

100 200 300 400 500 600 700 800 20 40 60 N z = 0.0 ErisDark: 590 Eris: 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

SLIDE 10

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10

1

10 10

1

10

2

10

3

V max (km/s)

N (> V max) ErisDark subhalo function at z=0

ErisDark within R200

VLII within R200

ErisDark Subhaloes

SLIDE 11

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10

−2

10

−1

10 10

1

10

2

10

3

V max / Vhost

max

N (> V max/ Vhost

max)

ErisDark subhalo function at z=0

ErisDark within R200

VLII within R200

ErisDark Subhaloes

SLIDE 12

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10

−2

10

−1

10 10

1

10

2

10

3

relative V max

N (> relative 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

SLIDE 13

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10

−2

10

−1

10 10

1

10

2

10

3

relative V max

N (> relative 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?

SLIDE 14

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:

10

2

10 10

1

10

2

10

3

Vmax (km/s)

N (> Vmax) N hosts = 99 10

−2

10

−1

10 10

1

10

2

10

3

Vmax/V host

max

Bolshoi at z=0: 1.58e+14 < M host <= 2.51e+14 M sun 10

−2

10

−1

10 10

1

10

2

10

3

Vmax/V host

vir

μmax μvir = =

Thanks to Joel and Peter

SLIDE 15

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10

1

10

2

10

3

10

−1

10 10

1

10

2

10

3

Vmax (km/s)

N (> Vmax) N hosts = 56 10

−1

10

−1

10 10

1

10

2

10

3

Vmax/V host

max

Bolshoi at z=0: 1.45e+14 < M host <= 1.73e+14 M sun 10

−1

10

−1

10 10

1

10

2

10

3

Vmax/V host

vir

10

1

10

2

10

3

10

−1

10 10

1

10

2

10

3

Vmax (km/s)

N (> Vmax) N hosts = 547 10

−1

10

−1

10 10

1

10

2

10

3

Vmax/V host

max

Bolshoi at z=0: 1.54e+13 < M host <= 1.75e+13 M sun 10

−1

10

−1

10 10

1

10

2

10

3

Vmax/V host

vir

10

1

10

2

10

3

10

−1

10 10

1

10

2

10

3

Vmax (km/s)

N (> Vmax) N hosts = 875 10

−1

10

−1

10 10

1

10

2

10

3

Vmax/V host

max

Bolshoi at z=0: 1.95e+12 < M host <= 2.00e+12 M sun 10

−1

10

−1

10 10

1

10

2

10

3

Vmax/V host

vir

Different host-masses:

smaller hosts

Excursus: scatter in the subhalo velocity function (II)

SLIDE 16

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10

1

10

2

10

3

10

−1

10 10

1

10

2

10

3

Vmax (km/s)

N (> Vmax) N hosts = 56 10

−1

10

−1

10 10

1

10

2

10

3

Vmax/V host

max

Bolshoi at z=0: 1.45e+14 < M host <= 1.73e+14 M sun 10

−1

10

−1

10 10

1

10

2

10

3

Vmax/V host

vir

10

1

10

2

10

3

10

−1

10 10

1

10

2

10

3

Vmax (km/s)

N (> Vmax) N hosts = 547 10

−1

10

−1

10 10

1

10

2

10

3

Vmax/V host

max

Bolshoi at z=0: 1.54e+13 < M host <= 1.75e+13 M sun 10

−1

10

−1

10 10

1

10

2

10

3

Vmax/V host

vir

10

1

10

2

10

3

10

−1

10 10

1

10

2

10

3

Vmax (km/s)

N (> Vmax) N hosts = 875 10

−1

10

−1

10 10

1

10

2

10

3

Vmax/V host

max

Bolshoi at z=0: 1.95e+12 < M host <= 2.00e+12 M sun 10

−1

10

−1

10 10

1

10

2

10

3

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?

SLIDE 17

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10

12

10

13

10

14

20 40 60 80 100 120 140 160

V max > 70 km/s V max > 70 km/s V max > 70 km/s V max > 70 km/s

M host N (> µ max) Subhaloes in Bolshoi at z=0, normalized to Vhost

max

µ max = 0.08 µ max = 0.11 µ max = 0.20 µ max = 0.31 10

12

10

13

10

14

20 40 60 80 100 120 140 160

V max > 70 km/s V max > 70 km/s V max > 70 km/s V max > 70 km/s

M host N (> µ vir) Subhaloes in Bolshoi at z=0, normalized to Vhost

vir

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)

SLIDE 18

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

Excursus: scatter in the subhalo velocity function (V)

SLIDE 19

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 ???

SLIDE 20

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

SLIDE 21

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10

−4

10

−3

10

3

10

4

10

5

10

6

10

7

M host

vir dN/dM

z = 0

MW Satellites

ErisDark: M TOT Eris: M TOT Eris: M DM 10

−4

10

−3

1 2 3 4 5 M/M host

vir

ErisDark/Eris 10

−2

10

−1

10 10

1

10

2

10

3

N( > V max/V host

vir )

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

−1

1 2 3

V max/V host

vir

ErisDark/Eris

Satellites Abundances

SLIDE 22

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10

−2

10

−1

10 10

1

10

2

10

3

N( > V max/V host

vir )

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

−1

1 2 3

V max/V host

vir

ErisDark/Eris

Satellites Abundances

SLIDE 23

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10

−2

10

−1

10 10

1

10

2

10

3

N( > V max/V host

vir )

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

−1

1 2 3

V max/V host

vir

ErisDark/Eris

Satellites Abundances

see Zolotov&co talks and papers:

SLIDE 24

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10

−2

10

−1

10 10

1

10

2

10

3

N( > V max/V host

vir )

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

−1

1 2 3

V max/V host

vir

ErisDark/Eris

Satellites Abundances

Mayer et al. in preparation.

The most massive objects

undergo strongest stripping

The amount of stripped

material depends on the slope

f the inner densities, on the
rbits, 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!

SLIDE 25

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10

−2

10

−1

10 10

1

10

2

10

3

N( > V max/V host

vir )

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

−1

1 2 3

V max/V host

vir

ErisDark/Eris

Satellites Abundances

Baryons not always produce reduced inner densities and shallower density profiles....

SLIDE 26

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10

−2

10

−1

10 10

1

10

2

10

3

N( > V max/V host

vir )

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

−1

1 2 3

V max/V host

vir

ErisDark/Eris

Eris luminous satellites

SLIDE 27

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

0.5 1 1.5 2 10 20 30 40 50 R (com kpc)

V circ (km/s)

Eris.00049 at z = 0.0

Power:2003

47, 29.9 km/s , 5.0 kpc 49, 25.8 km/s , 4.7 kpc TOT DM GAS STARS

10

−2

10

−1

10 10

1

10

2

10

3

N( > V max/V host

vir )

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

−1

1 2 3

V max/V host

vir

ErisDark/Eris

Eris luminous satellites

MTOT = 2e9 Msun Mstellar ~ 1e7 Msun Mass loss ~ 50 % z infall = 0.99 dMW = 215 kpc

SLIDE 28

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

0.5 1 1.5 2 10 20 30 40 50 R (com kpc)

V circ (km/s)

Eris.00021 at z = 0.0

Power:2003

580, 15.8 km/s , 2.2 kpc 21, 32.8 km/s , 0.4 kpc TOT DM GAS STARS

10

−2

10

−1

10 10

1

10

2

10

3

N( > V max/V host

vir )

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

−1

1 2 3

V max/V host

vir

ErisDark/Eris

Eris luminous satellites

MTOT = 3.7e8 Msun Mstellar ~ 1.8e8 Msun Mass loss ~ 96 % z infall = 1.2 dMW = 34 kpc

SLIDE 29

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

0.5 1 1.5 2 10 20 30 40 50 R (com kpc)

V circ (km/s)

Eris.00031 at z = 0.0

Power:2003

486, 20.9 km/s , 1.7 kpc 31, 31.7 km/s , 0.5 kpc TOT DM GAS STARS

10

−2

10

−1

10 10

1

10

2

10

3

N( > V max/V host

vir )

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

−1

1 2 3

V max/V host

vir

ErisDark/Eris

Eris luminous satellites

MTOT = 3.1e8 Msun Mstellar ~ 1.6e8 Msun Mass loss ~ 97 % z infall = 1.8 dMW = 30 kpc

SLIDE 30

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

10

−2

10

−1

10 10

1

10

2

10

3

N( > V max/V host

vir )

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

−1

1 2 3

V max/V host

vir

ErisDark/Eris

M32

Eris luminous satellites

ref. Toloba:2011

e.g: M32 in Andromeda e.g: all past SPH satellites

SLIDE 31

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

Top10 satellites in ErisDark (Vmax selected)

1 2 10 20 30 40 50 R (kpc)

47, 29.9 km/s 48, 25.8 km/s

Vcirc (km/s)

1 2 10 20 30 40 50 R (kpc)

160, 15.1 km/s 65, 16.9 km/s

1 2 10 20 30 40 50 R (kpc)

176, 19.9 km/s 156, 17.4 km/s

1 2 10 20 30 40 50 R (kpc)

268, 15.0 km/s 282, 14.1 km/s

1 2 10 20 30 40 50 R (kpc)

283, 14.5 km/s 344, 11.9 km/s

1 2 10 20 30 40 50 R (kpc)

340, 18.7 km/s 354, 16.3 km/s

Vcirc (km/s)

1 2 10 20 30 40 50 R (kpc)

403, 18.7 km/s 463, 15.5 km/s

1 2 10 20 30 40 50 R (kpc)

458, 16.6 km/s 867, 12.0 km/s

1 2 10 20 30 40 50 R (kpc)

486, 20.9 km/s 31, 31.6 km/s

1 2 10 20 30 40 50 R (kpc)

582, 15.8 km/s 21, 33.0 km/s

SLIDE 32

Eris Project: the effects of baryons on MW galaxies Annalisa Pillepich, August 2012

1 2 10 20 30 40 50 R (kpc)

21, 33.0 km/s 582, 15.8 km/s

Vcirc (km/s)

1 2 10 20 30 40 50 R (kpc)

31, 31.6 km/s 486, 20.9 km/s

1 2 10 20 30 40 50 R (kpc)

48, 25.8 km/s 47, 29.9 km/s

1 2 10 20 30 40 50 R (kpc)

168, 16.3 km/s 1334, 11.6 km/s

1 2 10 20 30 40 50 R (kpc)

194, 14.0 km/s 306, 15.8 km/s

1 2 10 20 30 40 50 R (kpc)

260, 12.2 km/s 1, 166.1 km/s

Vcirc (km/s)

1 2 10 20 30 40 50 R (kpc)

282, 14.1 km/s 268, 15.0 km/s

1 2 10 20 30 40 50 R (kpc)

354, 16.3 km/s 340, 18.7 km/s

1 2 10 20 30 40 50 R (kpc)

367, 16.4 km/s 627, 15.9 km/s

1 2 10 20 30 40 50 R (kpc)

425, 12.1 km/s 743, 12.4 km/s

Top10 satellites in Eris (Vmax selected)

SLIDE 33

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)