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Star formation in alternative dark matter dwarfs: then and now Mark - - PowerPoint PPT Presentation

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CDM ETHOS ETHOS-CDM Star formation in alternative dark matter dwarfs: then and now Mark R. Lovell 1,2 , Jess Zavala 1 + ( 1 University of Iceland, 2 Durham, *lovell@hi.is) DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] Mark Lovell,

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SLIDE 1

Star formation in alternative dark matter dwarfs: then and now

Mark R. Lovell⋆1,2, Jesús Zavala

1+ (1University of Iceland, 2Durham, *lovell@hi.is)

DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ]

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

CDM ETHOS ETHOS-CDM

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SLIDE 2

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

Power spectrum cutoff: low redshift

10 20 30 40 50 70 85 V1kpc [km s-1] 105 106 107 108 109 1010 M* [MO

  • ]

CDM L6=10 L6=120

X obs. Lovell+2017

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SLIDE 3

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

Power spectrum cutoff: low redshift

10 20 30 40 50 70 85 V1kpc [km s-1] 105 106 107 108 109 1010 M* [MO

  • ]

CDM L6=10 L6=120

X obs. Lovell+2017

1.5 2.0 2.5 3.0 3.5 MLG [1012MO

  • ]

20 40 60 80 100 120 N(r<2Mpc) M*>105 MO

  • CDM

L6=10 L6=120

Obs.

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SLIDE 4

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

Power spectrum cutoff: low redshift

10 20 30 40 50 70 85 V1kpc [km s-1] 105 106 107 108 109 1010 M* [MO

  • ]

CDM L6=10 L6=120

X obs. Lovell+2017

1.5 2.0 2.5 3.0 3.5 MLG [1012MO

  • ]

20 40 60 80 100 120 N(r<2Mpc) M*>105 MO

  • CDM

L6=10 L6=120

Obs. Lovell+2012

(1.4keV)

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SLIDE 5

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

Power spectrum cutoff: low redshift

10 20 30 40 50 70 85 V1kpc [km s-1] 105 106 107 108 109 1010 M* [MO

  • ]

CDM L6=10 L6=120

X obs. Lovell+2017 How is halo/galaxy formation different at high redshifts? How about the oldest stars?

1.5 2.0 2.5 3.0 3.5 MLG [1012MO

  • ]

20 40 60 80 100 120 N(r<2Mpc) M*>105 MO

  • CDM

L6=10 L6=120

Obs. Lovell+2012

(1.4keV)

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SLIDE 6

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

CDM ETHOS ETHOS-CDM

The simulations

  • Full hydro, SF

, supernova feedback

  • ETHOS model: self-interactions + dark

acoustic oscillations

  • Particle mass: 1.76 × 106Msun
  • Box size: 25Mpc/h
  • Run to z=6

Lovell+2018 Temperature map 7keV sterile neutrino

}

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SLIDE 7

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

CDM ETHOS ETHOS-CDM

The simulations

  • Full hydro, SF

, supernova feedback

  • ETHOS model: self-interactions + dark

acoustic oscillations

  • Particle mass: 1.76 × 106Msun
  • Box size: 25Mpc/h
  • Run to z=6

Lovell+2018 Temperature map 7keV sterile neutrino

}

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SLIDE 8

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

CDM ETHOS ETHOS-CDM

The simulations

  • Full hydro, SF

, supernova feedback

  • ETHOS model: self-interactions + dark

acoustic oscillations

  • Particle mass: 1.76 × 106Msun
  • Box size: 25Mpc/h
  • Run to z=6

Lovell+2018 Temperature map 7keV sterile neutrino

}

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SLIDE 9

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

CDM ETHOS ETHOS-CDM

The simulations

  • Full hydro, SF

, supernova feedback

  • ETHOS model: self-interactions + dark

acoustic oscillations

  • Particle mass: 1.76 × 106Msun
  • Box size: 25Mpc/h
  • Run to z=6

Lovell+2018 Temperature map 7keV sterile neutrino

}

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SLIDE 10

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

ETHOS vs. CDM — change in DM mass / gas mass

0.0 108 109 1010 1011 M200,X [MO

  • ]

0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 MDM,ETHOS/MDM,CDM Matched pairs Median relations 2.5 z=10 z=6

Lovell+2019

Bound DM mass

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SLIDE 11

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

ETHOS vs. CDM — change in DM mass / gas mass

0.0 108 109 1010 1011 M200,X [MO

  • ]

0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 MDM,ETHOS/MDM,CDM Matched pairs Median relations 2.5 z=10 z=6

Lovell+2019

Bound DM mass

0.0 0.5 1.0 1.5 2.0 2.5 Mg,ETHOS/Mg,CDM z=10 z=6 108 109 1010 1011 M200,X [MO

  • ]

0.0

Bound gas mass

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SLIDE 12

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

ETHOS vs. CDM — change in DM mass / gas mass

0.0 108 109 1010 1011 M200,X [MO

  • ]

0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 MDM,ETHOS/MDM,CDM Matched pairs Median relations 2.5 z=10 z=6

Lovell+2019

Bound DM mass

0.0 0.5 1.0 1.5 2.0 2.5 Mg,ETHOS/Mg,CDM z=10 z=6 108 109 1010 1011 M200,X [MO

  • ]

0.0

Bound gas mass SFR

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SLIDE 13

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

The galaxy population & reionisation

Lovell+2018

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SLIDE 14

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

The galaxy population & reionisation

Lovell+2018

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SLIDE 15

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

ETHOS vs. CDM — change in condensation time [t(M=108Msun)] & oldest stellar populations

−400 −200 200 400 600 −400 −200 200 400 600 tcond,ETHOS−tcond,CDM [Myr] −400 −200 200 400 600 tcond,ETHOS−tcond,CDM [Myr]

200 300 400 500 600 700 800 900 1000 tcond [Myr] 6 7 8 9 10 12 15 18 z

z= 6.0 R>0.90 All [8,9] [9,10] [10,11] log(M200,CDM/MO

  • )=

Lovell+2019

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SLIDE 16

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

ETHOS vs. CDM — change in condensation time [t(M=108Msun)] & oldest stellar populations

−400 −200 200 400 600 −400 −200 200 400 600 tcond,ETHOS−tcond,CDM [Myr] −400 −200 200 400 600 tcond,ETHOS−tcond,CDM [Myr]

200 300 400 500 600 700 800 900 1000 tcond [Myr] 6 7 8 9 10 12 15 18 z

z= 6.0 R>0.90 All [8,9] [9,10] [10,11] log(M200,CDM/MO

  • )=

Lovell+2019

0.0 0.2 0.4 0.6 0.8 1.0 0.0 0.2 0.4 0.6 0.8 1.0 CDF(tage o/f.s.>t)

300 400 500 600 700 800 900 t [Myr] 9 10 12 15 17 20 25 z log(M*/MO

  • )=[6.5,7.0],

Mgas<0.1M* CDM ETHOS z=6, t(z=0->z=6)= 12.7Gyr

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SLIDE 17

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

ETHOS vs. CDM — change in condensation time [t(M=108Msun)] & oldest stellar populations

−400 −200 200 400 600 −400 −200 200 400 600 tcond,ETHOS−tcond,CDM [Myr] −400 −200 200 400 600 tcond,ETHOS−tcond,CDM [Myr]

200 300 400 500 600 700 800 900 1000 tcond [Myr] 6 7 8 9 10 12 15 18 z

z= 6.0 R>0.90 All [8,9] [9,10] [10,11] log(M200,CDM/MO

  • )=

Lovell+2019

0.0 0.2 0.4 0.6 0.8 1.0 0.0 0.2 0.4 0.6 0.8 1.0 CDF(tage o/f.s.>t)

300 400 500 600 700 800 900 t [Myr] 9 10 12 15 17 20 25 z log(M*/MO

  • )=[6.5,7.0],

Mgas<0.1M* CDM ETHOS z=6, t(z=0->z=6)= 12.7Gyr

X LG-oMSTO

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SLIDE 18

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

ETHOS vs. CDM — change in condensation time [t(M=108Msun)] & oldest stellar populations

−400 −200 200 400 600 −400 −200 200 400 600 tcond,ETHOS−tcond,CDM [Myr] −400 −200 200 400 600 tcond,ETHOS−tcond,CDM [Myr]

200 300 400 500 600 700 800 900 1000 tcond [Myr] 6 7 8 9 10 12 15 18 z

z= 6.0 R>0.90 All [8,9] [9,10] [10,11] log(M200,CDM/MO

  • )=

Lovell+2019

0.0 0.2 0.4 0.6 0.8 1.0 0.0 0.2 0.4 0.6 0.8 1.0 CDF(tage o/f.s.>t)

300 400 500 600 700 800 900 t [Myr] 9 10 12 15 17 20 25 z log(M*/MO

  • )=[6.5,7.0],

Mgas<0.1M* CDM ETHOS z=6, t(z=0->z=6)= 12.7Gyr

X LG-oMSTO X LG-all obs.

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SLIDE 19

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

ETHOS vs. CDM — change in condensation time [t(M=108Msun)] & oldest stellar populations

−400 −200 200 400 600 −400 −200 200 400 600 tcond,ETHOS−tcond,CDM [Myr] −400 −200 200 400 600 tcond,ETHOS−tcond,CDM [Myr]

200 300 400 500 600 700 800 900 1000 tcond [Myr] 6 7 8 9 10 12 15 18 z

z= 6.0 R>0.90 All [8,9] [9,10] [10,11] log(M200,CDM/MO

  • )=

Lovell+2019

0.0 0.2 0.4 0.6 0.8 1.0 0.0 0.2 0.4 0.6 0.8 1.0 CDF(tage o/f.s.>t)

300 400 500 600 700 800 900 t [Myr] 9 10 12 15 17 20 25 z log(M*/MO

  • )=[6.5,7.0],

Mgas<0.1M* CDM ETHOS z=6, t(z=0->z=6)= 12.7Gyr

X LG-oMSTO X LG-all obs. O Apostle dwarfs

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SLIDE 20

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

ETHOS vs. CDM — change in condensation time [t(M=108Msun)] & oldest stellar populations

−400 −200 200 400 600 −400 −200 200 400 600 tcond,ETHOS−tcond,CDM [Myr] −400 −200 200 400 600 tcond,ETHOS−tcond,CDM [Myr]

200 300 400 500 600 700 800 900 1000 tcond [Myr] 6 7 8 9 10 12 15 18 z

z= 6.0 R>0.90 All [8,9] [9,10] [10,11] log(M200,CDM/MO

  • )=

Lovell+2019

0.0 0.2 0.4 0.6 0.8 1.0 0.0 0.2 0.4 0.6 0.8 1.0 CDF(tage o/f.s.>t)

300 400 500 600 700 800 900 t [Myr] 9 10 12 15 17 20 25 z log(M*/MO

  • )=[6.5,7.0],

Mgas<0.1M* CDM ETHOS z=6, t(z=0->z=6)= 12.7Gyr

X LG-oMSTO X LG-all obs. O Apostle dwarfs Lovell+(in prep.)

}

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SLIDE 21

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

ETHOS vs. CDM — change in condensation time [t(M=108Msun)] & oldest stellar populations

−400 −200 200 400 600 −400 −200 200 400 600 tcond,ETHOS−tcond,CDM [Myr] −400 −200 200 400 600 tcond,ETHOS−tcond,CDM [Myr]

200 300 400 500 600 700 800 900 1000 tcond [Myr] 6 7 8 9 10 12 15 18 z

z= 6.0 R>0.90 All [8,9] [9,10] [10,11] log(M200,CDM/MO

  • )=

Lovell+2019

0.0 0.2 0.4 0.6 0.8 1.0 0.0 0.2 0.4 0.6 0.8 1.0 CDF(tage o/f.s.>t)

300 400 500 600 700 800 900 t [Myr] 9 10 12 15 17 20 25 z log(M*/MO

  • )=[6.5,7.0],

Mgas<0.1M* CDM ETHOS z=6, t(z=0->z=6)= 12.7Gyr

X LG-oMSTO X LG-all obs. O Apostle dwarfs Lovell+(in prep.)

}

zre~8 zre~11.5

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SLIDE 22

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

Aside: Lensing arcs

Despali, MRL, Vegetti, Crain, Oppenheimer 2019

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SLIDE 23

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

Aside: DM detection in Perseus with XRISM

400 600 800 1000 1200 σ1D,DM [km/s]

1 2 4 9 20 44 93 199

#s.l., all

halo #18 P.−analog, on−center P.−analog, off−center, 1’ P.−analog, on−center P.−analog, off−center, 1’ P.−analog, on−center P.−analog, off−center, 1’ P.−analog, on−center P.−analog, off−center, 1’ 4 5 6 7 8 9 F [10−8 counts/sec/cm2] 400 600 800 1000 σ1D,DM [km/s] halo #19 τ=1028.0s m=7.1keV FoV=1.4’

  • XRISM X-ray observatory,

scheduled to launch January 2022

  • If 3.55keV line is DM, predict

XRISM will detect a line with

  • Flux ~5x10-8 counts/sec/cm2,

and:

  • Velocity dispersion ~600km/s
  • Perseus details:

DOI: 10.3847/2041-8213/ ab13ac

  • More X-ray predictions:

DOI: 10.1093/mnras/stz691

Lovell+2019c Hydrodynamical cluster simulations

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SLIDE 24

Mark Lovell, HÍ/Durham University DOI:[ 10.1093/mnras/stz766 , 10.1093/mnras/sty818 ] DG-CQ:2019

Conclusions

0.0 0.2 0.4 0.6 0.8 1.0 0.0 0.2 0.4 0.6 0.8 1.0 CDF(tage o/f.s.>t)

300 400 500 600 700 800 900 t [Myr] 9 10 12 15 17 20 25 z log(M*/MO

  • )=[6.5,7.0],

Mgas<0.1M* CDM ETHOS z=6, t(z=0->z=6)= 12.7Gyr

Lovell+2019

  • Suppresses DM mass, but gas mass

enhanced

  • SFR enhanced at high redshift with cutoff
  • Consistent with high redshift observables
  • Delay correlates inversely with galaxy

mass

  • ~100Myr delay possible in first star

formation time, BUT:

  • Need better reionisation, cooling, and

escape fraction models to discern the nature of the dark matter. Plus more precise observations