Dark matter heats up in dwarf galaxies Justin I. Read Matthew - - PowerPoint PPT Presentation

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Dark matter heats up in dwarf galaxies Justin I. Read Matthew - - PowerPoint PPT Presentation

Mar 06, 2024 270 likes •594 views

Dark matter heats up in dwarf galaxies Justin I. Read Matthew Walker, Pascal Steger, Oscar Agertz, Michelle Collins, Denis Erkal, Giuliano Iorio, Filippo Fraternali, Alexandra Gregory, Matthew Orkney, Andrew Pontzen, Martin Rey The Cusp-Core

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SLIDE 1

Dark matter heats up in dwarf galaxies

Justin I. Read

Matthew Walker, Pascal Steger, Oscar Agertz, Michelle Collins, Denis Erkal, Giuliano Iorio, Filippo Fraternali, Alexandra Gregory, Matthew Orkney, Andrew Pontzen, Martin Rey

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SLIDE 2

The Cusp-Core Problem

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SLIDE 3

WLM; Leroy, Nature 2015

The Cusp-Core Problem

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The Cusp-Core Problem

e.g. Flores & Primack 1994; Moore 1994; Read et al. 2017

0.0 0.5 1.0 1.5 2.0 2.5 3.0 R (kpc) 5 10 15 20 25 30 35 40 45 vc(km s−1)

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SLIDE 5

0.0 0.5 1.0 1.5 2.0 2.5 3.0 R (kpc) 5 10 15 20 25 30 35 40 45 vc(km s−1)

stars gas

The Cusp-Core Problem

e.g. Flores & Primack 1994; Moore 1994; Read et al. 2017

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SLIDE 6

0.0 0.5 1.0 1.5 2.0 2.5 3.0 R (kpc) 5 10 15 20 25 30 35 40 45 vc(km s−1)

stars gas

The Cusp-Core Problem

e.g. Flores & Primack 1994; Moore 1994; Read et al. 2017

102 101 100 r(kpc) 106 107 108 109 ρdm(M kpc3)

CUSP CORE

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SLIDE 7

Dark Matter Heating

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SLIDE 8

e.g. Navarro et al. 1996; Read & Gilmore 2005; Pontzen & Governato 2012; Read et al. 2016

Dark matter heating

2 kpc

View from top

ρth = 300 atoms/cc Tgas,min = 10 K Mres = 300 M⊙ Δx = 4 pc

R1/2

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SLIDE 9

Read et al. 2016

102 101 100 r [kpc] 104 105 106 107 108 109 ρDM [M kpc3]

1 Gyr 4 Gyr 8 Gyr 14 Gyr ICs

R1/2 r1/2

Dark matter heating

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102 101 100 r(kpc) 105 106 107 108 109 ρdm(M kpc3)

NFW coreNFW

R1/2

P u r e d a r k m a t t e r DM+baryons

Read et al. 2016

Dark matter heating

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SLIDE 11

The Cusp-Core Problem Revisited

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SLIDE 12

0.0 0.5 1.0 1.5 2.0 2.5 3.0 R (kpc) 5 10 15 20 25 30 35 40 45 vc(km s−1)

Read et al. 2016b,2017

Measurement | Rotation cuves

WLM s t a r s gas

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SLIDE 13

0.0 0.5 1.0 1.5 2.0 2.5 3.0 R (kpc) 5 10 15 20 25 30 35 40 45 vc(km s−1)

Read et al. 2016b,2017

Measurement | Rotation cuves

WLM s t a r s gas

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SLIDE 14

1 2 3 4 5 R (kpc) 10 20 30 40 50 60 70 vc(km s−1)

Stars Gas Fit coreNFW DDO133

0.0 0.2 0.4 0.6 0.8 1.0 1.2 R (kpc) 5 10 15 20 25 30 vc(km s−1)

Stars Gas Fit coreNFW Aquarius

1 2 3 4 5 R (kpc) 10 20 30 40 50 60 vc(km s−1)

Stars Gas Fit coreNFW DDO87

1 2 3 4 5 R (kpc) 10 20 30 40 50 60 vc(km s−1)

Stars Gas Fit coreNFW DDO126

1 2 3 4 5 R (kpc) 10 20 30 40 50 60 vc(km s−1)

Stars Gas Fit coreNFW UGC8508

1 2 3 4 5 R (kpc) 5 10 15 20 25 30 vc(km s−1)

Stars Gas Fit coreNFW CVnIdwA

1 2 3 4 5 R (kpc) 10 20 30 40 50 60 70 vc(km s−1)

Stars Gas Fit coreNFW DDO168

1 2 3 4 5 R (kpc) 10 20 30 40 50 60 vc(km s−1)

Stars Gas Fit coreNFW NGC 6822

Rmin Rmin Rmin

1 2 3 4 5 6 7 8 9 R (kpc) 10 20 30 40 50 60 70 vc(km s−1)

Stars Gas Fit coreNFW NGC2366

1 2 3 4 5 6 7 8 R (kpc) 10 20 30 40 50 60 vc(km s−1)

Stars Gas Fit coreNFW DDO154

1 2 3 4 5 R (kpc) 10 20 30 40 50 60 vc(km s−1)

Stars Gas Fit coreNFW DDO52

0.0 0.5 1.0 1.5 2.0 2.5 3.0 R (kpc) 5 10 15 20 25 30 35 40 45 vc(km s−1)

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“Smoking gun” evidence for DM heating

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Less star formation ⇒ more cusp

ESO/Digitized Sky Survey 2

Fornax WLM

Leroy, Nature 2015 Robert Lupton & SDSS

Draco D e c r e a s i n g s t a r f

  • r

m a t i

  • n

⇒

M

  • r

e D M c u s p !

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SLIDE 17

Less star formation ⇒ more cusp

ESO/Digitized Sky Survey 2

Fornax WLM

Leroy, Nature 2015 Robert Lupton & SDSS

Draco Rotation curves Stellar kinematics

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SLIDE 18

101 100 Radius (kpc) 106 107 108 109 Density (M kpc3)

Less star formation ⇒ more cusp

2 4 6 8 10 12 14 Age (Gyr) 105 104 103 102 SFR (M/yr)

WLM

WLM

Read et al. 2018a,b,c: arXiv:1805.06934; arXiv:1807.07093; arXiv:1808.06634

Big Bang Today

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2 4 6 8 10 12 14 Age (Gyr) 105 104 103 102 SFR (M/yr)

Fornax

Less star formation ⇒ more cusp

Fornax

101 100 Radius (kpc) 106 107 108 109 Density (M kpc3)

Read et al. 2018a,b,c: arXiv:1805.06934; arXiv:1807.07093; arXiv:1808.06634

Big Bang Today

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2 4 6 8 10 12 14 Age (Gyr) 106 105 104 103 SFR (M/yr)

Sculptor

Less star formation ⇒ more cusp

Sculptor

101 100 Radius (kpc) 106 107 108 109 Density (M kpc3)

Read et al. 2018a,b,c: arXiv:1805.06934; arXiv:1807.07093; arXiv:1808.06634

Big Bang Today

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101 100 Radius (kpc) 106 107 108 109 Density (M kpc3) 2 4 6 8 10 12 14 Age (Gyr) 106 105 104 103 SFR (M/yr)

Draco

Less star formation ⇒ more cusp

Draco

core cusp

150pc

Read et al. 2018a,b,c: arXiv:1805.06934; arXiv:1807.07093; arXiv:1808.06634

Big Bang Today

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105 106 107 108 M⇤ [M] 107 108 109 ρDM(150 pc) [M kpc3]

Dra For UMi Scl Sex LI LII Car Tuc CVnI WLM Aq CVn D154 D87 D52 D168 N2366

Read et al. 2018a,b,c: arXiv:1805.06934; arXiv:1807.07093; arXiv:1808.06634; Gregory et al. 2019

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SLIDE 23

105 106 107 108 M⇤ [M] 107 108 109 ρDM(150 pc) [M kpc3]

Dra For UMi Scl Sex LI LII Car Tuc CVnI WLM Aq CVn D154 D87 D52 D168 N2366

ttrunc/Gyrs > 6 3 < ttrunc/Gyrs < 6 ttrunc/Gyrs < 3

Read et al. 2018a,b,c: arXiv:1805.06934; arXiv:1807.07093; arXiv:1808.06634; Gregory et al. 2019

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SLIDE 24

109 1010 M200 [M] 107 108 109 ρDM(150 pc) [M kpc3]

Dra For UMi Scl Sex LI LII Car Tuc CVnI WLM Aq CVn D154 D87 D52 D168 N2366

Read et al. 2018a,b,c: arXiv:1805.06934; arXiv:1807.07093; arXiv:1808.06634; Gregory et al. 2019

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SLIDE 25

109 1010 M200 [M] 107 108 109 ρDM(150 pc) [M kpc3]

Dra For UMi Scl Sex LI LII Car Tuc CVnI WLM Aq CVn D154 D87 D52 D168 N2366

cusp core

Read et al. 2018a,b,c: arXiv:1805.06934; arXiv:1807.07093; arXiv:1808.06634; Gregory et al. 2019

Gregory et al. 2019

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104 103 102 M⇤/M200 107 108 109 ρDM(150 pc) [M kpc3]

Dra For UMi Scl Sex LI LII Car Tuc CVnI WLM Aq CVn D154 D87 D52 D168 N2366

Di Cintio et al. (2014)

Read et al. 2018a,b,c: arXiv:1805.06934; arXiv:1807.07093; arXiv:1808.06634; Gregory et al. 2019

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Implications

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SLIDE 28

Agertz et al. 2019 | arXiv:1904.02723

Martin Rey Matt Orkney

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Read et al. 2006; Peñarrubia et al. 2010; Errani et al. 2019

Implications | Tides

Cusped Cored

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Conclusions

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Conclusions

Justin I. Read

  • We have found evidence for “dark matter heating” in

nearby dwarf galaxies.

  • If correct, this solves the cusp-core problem (at least for

the smallest dwarfs).

  • Implications ⇒
  • Dark matter appears to be a cold, collisionless, fluid that

can be heated up and moved around.

  • Densest dwarfs constrain “beyond-CDM” models.
  • Dark matter heating will impact galaxy formation from

the “bottom up”. We are exploring this with EDGE.