Quenching of Central Galaxies in the Next Generation Illustris - - PowerPoint PPT Presentation

▶
quenching of central galaxies in the next generation
SMART_READER_LITE
LIVE PREVIEW

Quenching of Central Galaxies in the Next Generation Illustris - - PowerPoint PPT Presentation

Nov 26, 2022 340 likes •539 views

Quenching of Central Galaxies in the Next Generation Illustris Simulations (IllustrisTNG) Rainer Weinberger Rainer Weinberger (Heidelberg Institute for Theoretical Studies) Heidelberg Institute for Theoretical Studies (HITS) The role

slide-1
SLIDE 1

Rainer Weinberger (Heidelberg Institute for Theoretical Studies)

  • The role of gas in galaxy dynamics — Valetta, Malta

xx/10/2017

Quenching of Central Galaxies in the Next Generation Illustris Simulations (IllustrisTNG)

Rainer Weinberger Heidelberg Institute for Theoretical Studies (HITS)

  • Oct. 06, 2017 The Role of Gas in Galaxy Dynamics — Valletta

Volker Springel, Rüdiger Pakmor (HITS), Lars Hernquist, Jill Naiman (CfA, Harvard), Federico Marinacci, Paul Torrey, Mark Vogelsberger (MIT), Annalisa Pillepich (MPIA), Dylan Nelson (MPA), Shy Genel (CCA)

movie: Mark Vogelsberger, IllustrisTNG collaboration

http://www.tng-project.org

slide-2
SLIDE 2
  • Updated model for galaxy

formation physics

  • New model for AGN feedback
  • Magnetohydrodynamics
  • Extended scope 


(3 different boxes)

The IllustrisTNG simulations — details

slide-3
SLIDE 3

106 107 108 109 MBH [M] 105 104 103 102 101 100 ˙ MBondi/ ˙ MEdd

The IllustrisTNG simulations — the black hole model

n [cm−3] T [K] |v| [km s−1]

M

10−4 10−3 10−2 10−1 100 107 108 109 102 103 104 100 101

RW et al. (2017)

two-mode AGN feedback


  • low mass, high 


accretion rate:
 thermal 
 (rather inefficient)


  • high mass, low


accretion rate:
 kinetic 
 (very efficient)

thermal kinetic

slide-4
SLIDE 4

The IllustrisTNG simulations — the black hole model

n [cm−3] T [K] |v| [km s−1]

M

10−4 10−3 10−2 10−1 100 107 108 109 102 103 104 100 101

RW et al. (2017)

two-mode AGN feedback


  • low mass, high 


accretion rate:
 thermal 
 (rather inefficient)


  • high mass, low


accretion rate:
 kinetic 
 (very efficient)

Yuan et al. (2015)

4.00

  • 2
  • 1

1 2 X (kpc) 1 2 3 4 5 Z (kpc) 4.00 4.67 5.33 6.00 6.67 7.33 8.00 Log[T (K)]

Time: 1.65 Myr

Mukherjee et al (2016)

slide-5
SLIDE 5

Observed and simulated signatures of quiescence

  • Use galaxy colors

proxy of star formation rate

  • Comparison to SDSS
  • Kinetic AGN feedback

is necessary to get a color bimodality

109 1010 1011 1012 M? [M] 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 B - V

fid no kin.

9.0 9.5 10.0 10.5 11.0 11.5 12.0

M ⋆ [ log Msun ]

0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0

(u-i) color [ mag ]

SDSS z<0.1 TNG100-1

9.0 9.5 10.0 10.5 11.0 11.5 12.0

M ⋆ [ log Msun ]

0.0 0.2 0.4 0.6 0.8 1.0

(g-r) color [ mag ]

9.0 9.5 10.0 10.5 11.0 11.5 12.0

M ⋆ [ log Msun ]

0.0 0.1 0.2 0.3 0.4 0.5 0.6

(r-i) color [ mag ]

9.0 9.5 10.0 10.5 11.0 11.5 12.0

M ⋆ [ log Msun ]

0.5 1.0 1.5 2.0 2.5 3.0 3.5

(u-r) color [ mag ]

Nelson et al. (2017) RW et al. (2017)

slide-6
SLIDE 6
  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7

z=4 z=2

9.5 10.5 11.5 log10(stellar mass [M])

  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7

log10(specific star formation rate [yr1])

z=1

9.5 10.5 11.5

z=0

AGN feedback in massive galaxies

slide-7
SLIDE 7
  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7

z=4 z=2

9.5 10.5 11.5 log10(stellar mass [M])
  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7
log10(specific star formation rate [yr1])

z=1

9.5 10.5 11.5

z=0

AGN feedback in massive galaxies - quenching

2 4 6 8 10 12 lookback time of quenching [Gyr] 0.0 0.2 0.4 0.6 0.8 1.0 fraction (> t) 5 10 15 20 25 30 35 40 45 rate [10−6 Mpc−3 Gyr−1]

RW et al. (in prep.)

slide-8
SLIDE 8

1040 1041 1042 1043 1044 1045 1046 1047 energy injection during quenching [erg s−1] 10−2 10−1 100 CDF

thermal

  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7

z=4 z=2

9.5 10.5 11.5 log10(stellar mass [M])
  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7
log10(specific star formation rate [yr1])

z=1

9.5 10.5 11.5

z=0

AGN feedback in massive galaxies - quenching

2 4 6 8 10 12 lookback time of quenching [Gyr] 0.0 0.2 0.4 0.6 0.8 1.0 fraction (> t) 5 10 15 20 25 30 35 40 45 rate [10−6 Mpc−3 Gyr−1]

RW et al. (in prep.)

cooling loss not important

50%

slide-9
SLIDE 9

1040 1041 1042 1043 1044 1045 1046 1047 energy injection during quenching [erg s−1] 10−2 10−1 100 CDF

thermal kinetic

  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7

z=4 z=2

9.5 10.5 11.5 log10(stellar mass [M])
  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7
log10(specific star formation rate [yr1])

z=1

9.5 10.5 11.5

z=0

AGN feedback in massive galaxies - quenching

2 4 6 8 10 12 lookback time of quenching [Gyr] 0.0 0.2 0.4 0.6 0.8 1.0 fraction (> t) 5 10 15 20 25 30 35 40 45 rate [10−6 Mpc−3 Gyr−1]

RW et al. (in prep.)

slide-10
SLIDE 10

1040 1041 1042 1043 1044 1045 1046 1047 energy injection during quenching [erg s−1] 10−2 10−1 100 CDF

thermal kinetic

  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7

z=4 z=2

9.5 10.5 11.5 log10(stellar mass [M])
  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7
log10(specific star formation rate [yr1])

z=1

9.5 10.5 11.5

z=0

AGN feedback in massive galaxies - quenching

kinetic feedback quenches galaxies

2 4 6 8 10 12 lookback time of quenching [Gyr] 0.0 0.2 0.4 0.6 0.8 1.0 fraction (> t) 5 10 15 20 25 30 35 40 45 rate [10−6 Mpc−3 Gyr−1]

RW et al. (in prep.)

slide-11
SLIDE 11

1040 1041 1042 1043 1044 1045 1046 1047 energy injection during quenching [erg s−1] 10−2 10−1 100 CDF

thermal kinetic quiescent

  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7

z=4 z=2

9.5 10.5 11.5 log10(stellar mass [M])
  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7
log10(specific star formation rate [yr1])

z=1

9.5 10.5 11.5

z=0

AGN feedback in massive galaxies - quiescence

kinetic feedback keeps galaxies quiescent

2 4 6 8 10 12 lookback time of quenching [Gyr] 0.0 0.2 0.4 0.6 0.8 1.0 fraction (> t) 5 10 15 20 25 30 35 40 45 rate [10−6 Mpc−3 Gyr−1]

RW et al. (in prep.)

slide-12
SLIDE 12

1040 1041 1042 1043 1044 1045 1046 1047 energy injection during quenching [erg s−1] 10−2 10−1 100 CDF

thermal kinetic star forming

  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7

z=4 z=2

9.5 10.5 11.5 log10(stellar mass [M])
  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7
log10(specific star formation rate [yr1])

z=1

9.5 10.5 11.5

z=0

AGN feedback in massive galaxies - star forming

thermal feedback in star forming galaxies

2 4 6 8 10 12 lookback time of quenching [Gyr] 0.0 0.2 0.4 0.6 0.8 1.0 fraction (> t) 5 10 15 20 25 30 35 40 45 rate [10−6 Mpc−3 Gyr−1]

RW et al. (in prep.)

slide-13
SLIDE 13

1040 1041 1042 1043 1044 1045 1046 1047 energy injection during quenching [erg s−1] 10−2 10−1 100 CDF

thermal kinetic quiescent star forming

  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7

z=4 z=2

9.5 10.5 11.5 log10(stellar mass [M])
  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7
log10(specific star formation rate [yr1])

z=1

9.5 10.5 11.5

z=0

AGN feedback in massive galaxies

2 4 6 8 10 12 lookback time of quenching [Gyr] 0.0 0.2 0.4 0.6 0.8 1.0 fraction (> t) 5 10 15 20 25 30 35 40 45 rate [10−6 Mpc−3 Gyr−1]

RW et al. (in prep.)

slide-14
SLIDE 14

What does this mean for galaxies?

  • Need low accretion rates to trigger quenching
  • Gas fueling an AGN does not help to quench a

galaxy

slide-15
SLIDE 15

Major mergers and quenching of galaxies

  • FIG. 1.— An schematic outline of the phases of growth in a “typical” galaxy undergoing a gas-rich major merger.
Image Credit: (a) NOAO/AURA/NSF; (b) REU program/NOAO/AURA/NSF; (c) NASA/STScI/ACS Science Team; (d) Optical (left): NASA/STScI/R. P. van der Marel & J. Gerssen; X-ray (right): NASA/CXC/MPE/S. Komossa et al.; (e) Left: J. Bahcall/M. Disney/NASA; Right: Gem- ini Observatory/NSF/University of Hawaii Institute for Astronomy; (f) J. Bahcall/M. Disney/NASA; (g) F. Schweizer (CIW/DTM); (h) NOAO/AURA/NSF.

Di Matteo et al. (2005) Hopkins et al. (2008)

1.0 1.5 2.0 2.5 3.0

t/Gyr

10-11 10-10 10-9 10-8

sSFR/yr-1

6 4 3 2.5

Redshift

BH+SNe, Enhanced merger BH accretion switched off Main sequence

Pontzen et al. (2017)

slide-16
SLIDE 16

Do major gas rich mergers quench galaxies?

  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7

z=4 z=2

9.5 10.5 11.5 log10(stellar mass [M])
  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7
log10(specific star formation rate [yr1])

z=1

9.5 10.5 11.5

z=0

2 4 6 8 10 12 lookback time of quenching [Gyr] 0.0 0.2 0.4 0.6 0.8 1.0 fraction (> t) 5 10 15 20 25 30 35 40 45 rate [10−6 Mpc−3 Gyr−1]

RW et al. (in prep.)

slide-17
SLIDE 17
  • 2

2 4 6 8 10 12 time between merger and quenching [Gyr] 0.0 0.2 0.4 0.6 0.8 1.0 fraction (> t) 1 2 3 4 5 6 7 8 9 [10−5 Mpc−3 Gyr−1]

Do major gas rich mergers quench galaxies?

  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7

z=4 z=2

9.5 10.5 11.5 log10(stellar mass [M])
  • 14
  • 13
  • 12
  • 11
  • 10
  • 9
  • 8
  • 7
log10(specific star formation rate [yr1])

z=1

9.5 10.5 11.5

z=0

2 4 6 8 10 12 lookback time of quenching [Gyr] 0.0 0.2 0.4 0.6 0.8 1.0 fraction (> t) 5 10 15 20 25 30 35 40 45 rate [10−6 Mpc−3 Gyr−1]

most of the quenching events are not triggered by galaxy major mergers

RW et al. (in prep.)

slide-18
SLIDE 18

Conclusions

  • IllustrisTNG reproduces colors of central galaxies
  • Quenching via kinetic feedback at (moderately) low

accretion rates

  • Luminous AGN do not cause quenching!
  • Most quenching events not triggered by a 


(gas rich) major merger