The Eris Project: the effects of baryons on the …hipacc.ucsc.edu/images/2012SCGW/slides/20120817_PillepichSlides... · N-body/SPH: PKDGRAV/GASOLINE Halo Finder: Amiga Halo Finder

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

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

Dar

k: D

M o

nly Eris: D

M, gas, stars

DM-only Density Field

Vmax

Eris MWs


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


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


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


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 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 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


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


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


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


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?


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


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


<= 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


<= 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


<= 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)


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


<= 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


<= 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


<= 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?


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)


Excursus: scatter in the subhalo velocity function (V)



??? MW and subhaloes beyond μ~0.1 ???



MW and subhaloes beyond μ~0.1

+- ~50%

+- ~66%

Ishiyama:2009

...also Wang: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


10⌧2

10⌧110

0

101

102

103

N(

> V

max/V

hos

t v

ir)

z = 0


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



10⌧2

10⌧110

0

101

102

103

N(

> V

max/V

hos

t v

ir)

z = 0


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


see Zolotov&co talks and papers:


10⌧2

10⌧110

0

101

102

103

N(

> V

max/V

hos

t v

ir)

z = 0


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


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!


10⌧2

10⌧110

0

101

102

103

N(

> V

max/V

hos

t v

ir)

z = 0


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


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


10⌧2

10⌧110

0

101

102

103

N(

> V

max/V

hos

t v

ir)

z = 0


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


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


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


MTOT = 2e9 MsunMstellar ~ 1e7 MsunMass loss ~ 50 %z infall = 0.99dMW = 215 kpc


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


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


MTOT = 3.7e8 MsunMstellar ~ 1.8e8 MsunMass loss ~ 96 %z infall = 1.2dMW = 34 kpc


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


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


MTOT = 3.1e8 MsunMstellar ~ 1.6e8 MsunMass loss ~ 97 %z infall = 1.8dMW = 30 kpc


10⌧2

10⌧110

0

101

102

103

N(

> V

max/V

hos

t v

ir)

z = 0


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


ref. Toloba:2011

e.g: M32 in Andromeda

e.g: all past SPH satellites


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


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)


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)

Documents

The Eris Project: the effects of baryons on the …hipacc.ucsc.edu/images/2012SCGW/slides/20120817_PillepichSlides... · N-body/SPH: PKDGRAV/GASOLINE Halo Finder: Amiga Halo Finder