Astrophysical Probes of Dark Matter Ting Li, Alex Drlica-Wagner - - PowerPoint PPT Presentation

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Astrophysical Probes of Dark Matter Ting Li, Alex Drlica-Wagner - - PowerPoint PPT Presentation

Aug 22, 2022 199 likes •592 views

Astrophysical Probes of Dark Matter Ting Li, Alex Drlica-Wagner Buckley & Peter 2017 arXiv:1712.06615 Cosmology/Dark Energy Dark Matter (DM) Orbital Motion in Galaxy M33 courtesy: Josh Frieman The Hunt for Dark Matter e.g., LHC

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SLIDE 1

Astrophysical Probes of Dark Matter

Ting Li, Alex Drlica-Wagner

Cosmology/Dark Energy Dark Matter (DM)

Buckley & Peter 2017 arXiv:1712.06615

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SLIDE 2

Orbital Motion in Galaxy M33

courtesy: Josh Frieman

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SLIDE 3

The Hunt for Dark Matter

?

D M D M SM SM Particle mass set by the weak scale: GeV to TeV Production Time

e.g., LHC

Indirect Detection Time

e.g., Fermi-LAT

Direct Detection Time

e.g., LUX

Courtesy Alex Drlica-Wagner

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SLIDE 4

Courtesy Alex Drlica-Wagner

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SLIDE 5

What have we learned about dark matter from astrophysical observations?

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SLIDE 6

The Hunt for Dark Matter

?

D M D M SM SM Particle mass set by the weak scale: GeV to TeV Production Time

e.g., LHC

Indirect Detection Time

e.g., Fermi-LAT

Direct Detection Time

e.g., LUX

Courtesy Alex Drlica-Wagner

DM Density/ Local Stellar Kinematics

DM Halo Density/J-Factor for dSph

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SLIDE 7
  • Dark matter is not baryon. Dark matter consist of

25% of the universe — CMB, BBN

  • Dark matter cannot be hot (i.e. sub-keV-mass) —

Structure Formation

  • Dark matter mass has to be above 3 keV —

Lyman-alpha forest/dwarf galaxies clumpy structure on small scale —> lower limit on DM particle

mass

  • Dark matter self-interaction cross section σ/m <1

cm2/g — colliding cluster

CDM vs WDM CDM vs SIDM

What have we learned about dark matter from astrophysical observations?

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SLIDE 8

ΛCDM Universe

Planck Collaboration (2016) Example: Cosmic Microwave Background 6-parameter fit to the Universe

CDM — Cold, Collisionless Dark Matter

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SLIDE 9
  • Dark matter is not baryon. Dark matter consist of 25%
  • f the universe — CMB, BBN
  • Dark matter cannot be hot (i.e. sub-keV-mass) —

Structure Formation

  • Dark matter mass has to be above 3 keV —

Lyman-alpha forest/dwarf galaxies clumpy structure on small scale —> lower limit on DM particle

mass

  • Dark matter self-interaction cross section σ/m <1

cm2/g — colliding cluster

CDM vs WDM CDM vs SIDM

What have we learned about dark matter from astrophysical observations?

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SLIDE 10

The Large-Scale Structure of the Universe

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Sloan Great Wall SDSS 2dfGRS Springel et al. (2006) Dark Matter Distribution from Simulations Galaxy Distributions from Observations

CDM vs HDM bottom-up vs top-down hierarchical vs fragmentation

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SLIDE 11
  • Dark matter is not baryon. Dark matter consist of 25%
  • f the universe — CMB, BBN
  • Dark matter cannot be hot (i.e. sub-keV-mass) —

Structure Formation

  • Dark matter mass has to be above 3 keV —

Lyman-alpha forest/dwarf galaxies clumpy structure on small scale —> lower limit on DM particle

mass

  • Dark matter self-interaction cross section σ/m <1

cm2/g — colliding cluster

CDM vs WDM CDM vs SIDM

What have we learned about dark matter from astrophysical observations?

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SLIDE 12

Matter Power Spectrum

Bullock & Boylan-Kolchin 2017

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SLIDE 13
  • Dark matter is not baryon. Dark matter consist of 25%
  • f the universe — CMB, BBN
  • Dark matter cannot be hot (i.e. sub-keV-mass) —

Structure Formation

  • Dark matter mass has to be above 3 keV —

Lyman-alpha forest/dwarf galaxies clumpy structure on small scale —> lower limit on DM particle

mass

  • Dark matter self-interaction cross section σ/m

<1 cm2/g — colliding cluster

CDM vs WDM CDM vs SIDM

What have we learned about dark matter from astrophysical observations?

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SLIDE 14

Bullet Cluster

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SLIDE 15
  • Dark matter is not baryon. Dark matter consist of 25%
  • f the universe — CMB, BBN
  • Dark matter cannot be hot (i.e. sub-keV-mass) —

Structure Formation

  • Dark matter mass has to be above 3 keV —

Lyman-alpha forest/dwarf galaxies clumpy structure on small scale —> lower limit on DM particle

mass

  • Dark matter self-interaction cross section σ/m <1

cm2/g — colliding cluster

CDM vs WDM CDM vs SIDM

What have we learned about dark matter from astrophysical observations?

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SLIDE 16

https://github.com/lsstdarkmatter/dark-matter-paper/issues/14

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SLIDE 17

Examples of Astrophysical Probes of Dark Matter

  • Dwarf Galaxy Luminosity Function
  • Density Perturbation in Stellar Streams
  • Galaxy-Galaxy Strong Lensing
  • Wobbling Brightest Cluster Galaxy (BCG)
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SLIDE 18

Bullock & Boylan-Kolchin 2017

Subhalo mass functions

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SLIDE 19

Dwarf Galaxy Discovery Timeline

SDSS Begins DECam Installed

Log Scale

Courtesy Alex Drlica-Wagner / Keith Bechtol

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SLIDE 20
  • Palomar 5 stream

Odenkirchen+2003 Bovy+2016

Subhalo Mass Function from Perturbations to Tidal Streams

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SLIDE 21

Galaxy-Galaxy Strong Lensing

  • Substructure perturbations in lens arcs/rings
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SLIDE 22

https://github.com/lsstdarkmatter/dark-matter-paper/issues/14

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SLIDE 23

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Courtesy: Stacy Kim (OSU) Kim+2017

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SLIDE 24

https://github.com/lsstdarkmatter/dark-matter-paper/issues/14

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SLIDE 25
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SLIDE 26

https://lsstdarkmatter.github.io/dark-matter-graph/network.html

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SLIDE 27

https://lsstdarkmatter.github.io/dark-matter-graph/network.html

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SLIDE 28

https://lsstdarkmatter.github.io/dark-matter-graph/network.html

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SLIDE 29

MACHO / Primordial Black Holes

Primordial black holes have re-emerged as a dark matter candidate after recent LIGO discoveries

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SLIDE 30
  • Astrophysical Observations can not
  • nly prove the existence of Dark

Matter, but also probe the microscopic properties of Dark Matter, including the mass and cross section, etc.

Combined probes for DM?

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SLIDE 31

Why Fermilab?

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SLIDE 32

Why Fermilab?

  • Need a lead from National Lab — Fundamental Physics
  • FCPA has
  • Strong DM theory group
  • Direct search experiments
  • Cosmic Surveys
  • Astrophysical probes of DM connect the 3 groups at

FCPA

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SLIDE 33

Why Fermilab?

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  • Dwarf Galaxy Luminosity Function
  • Density Perturbation in Stellar Streams
  • Galaxy-Galaxy Strong Lensing
  • Wobbling Brightest Cluster Galaxy

Near Field Cosmology

Ting, Alex, Brian Yanny…

Strong Lensing

Huan, Liz, Brian Nord.

Galaxy Clusters

Jim Annis, Yuanyuan…

These three probes are also the most active research area at Fermilab

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SLIDE 34

Why Fermilab?

  • Technology
  • CCD testing and development
  • DECam
  • DESI
  • Skipper CCD
  • Other R&D

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SLIDE 35

How?

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SLIDE 36

There is no dark matter science collaboration

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SLIDE 37

Build a Dark Matter Science Collaboration in LSST

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SLIDE 38

Next Generation Spectroscopy Instrument

  • SSSI?
  • Fiber Positioner R&D
  • Skipper CCD
  • SnowPAC2018: a white paper
  • n DM science enabled by a

wide-field spectroscopic survey (WFSS)

2020 Decadal Survey