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(In preparation) Koji Ichikawa In collaboration with Kohei Hayashi , Masahiro Ibe, Miho N. Ishigaki, Shigeki Matsumoto and Hajime Sugai. 1 PPP2015, Kyoto, Sep. 14-18, 2015 (In preparation) Koji Ichikawa In collaboration with Kohei Hayashi

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SLIDE 1

Koji Ichikawa

1

PPP2015, Kyoto, Sep. 14-18, 2015

In collaboration with Kohei Hayashi , Masahiro Ibe, Miho N. Ishigaki, Shigeki Matsumoto and Hajime Sugai.

(In preparation)

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SLIDE 2

Koji Ichikawa

2

PPP2015, Kyoto, Sep. 14-18, 2015

In collaboration with Kohei Hayashi , Masahiro Ibe, Miho N. Ishigaki, Shigeki Matsumoto and Hajime Sugai.

(In preparation)

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SLIDE 3

DM DM SM SM

Indirect Detection

Collider Production Direct Detection

Dark Matter Search

3

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SLIDE 4

4

Signal Target

Milky-Way Galaxy

Charged CRs Extra Galaxy/ Cluster

100 kpc 10 Mpc 8.5 kpc

dSphs

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SLIDE 5

Wino DM annihilation cross section

Current(slightly old) observational limit

5

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SLIDE 6

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Wino DM annihilation cross section

Current(slightly old) observational limit

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SLIDE 7

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Current observational limit

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SLIDE 8

Dwarf spheroidal galaxies

dSphs:

  • 1. Neighbor galaxies: 10~100kpc
  • 2. Large Mass to Luminosity ratio = DM rich
  • 3. Fewer gas containment

8

Classical Ultra-faint SDSS-II

arXiv:0908.2995v6 [astro-ph.CO]

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SLIDE 9

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Current observational limit

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SLIDE 10

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Current observational limit

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SLIDE 11

Particle Physics Factor Astrophysics Factor (J-factor)

  Z ZZ WW f , , , 

Hryczuk and Iengo (2012)

arXiv:1111.2916v4 [hep-ph]

Cirelli et al. (2012) arXiv:1012.4515 [hep-ph]

Signal Flux

Error: 1-10 % level Large uncertainty: Next Slide

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SLIDE 12

Astrophysical Factor

DM Density profile

(obs) 2 l.o.s

Jeans equation for stars

(Theory) 2 l.o.s

2 1

) / 1 ( ) / (

 

s s s

r r r r 

2 1

) / 1 ( ) / 1 (

 

 

s s s

r r r r 

Cusp Cored

Fit

Stellar Density Profile: ν(r)

12

Geringer-Sameth et al., arXiv:1408.0002

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SLIDE 13

Astrophysical Factor

DM Density profile

(obs) 2 l.o.s

Jeans equation for stars

(Theory) 2 l.o.s

2 1

) / 1 ( ) / (

 

s s s

r r r r 

2 1

) / 1 ( ) / 1 (

 

 

s s s

r r r r 

Cusp Cored

Fit

Classical:

Well-determined

Ultra-faint:

Not well-determined.

Prior dependence

Stellar Density Profile: ν(r)

13

Conservative?

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SLIDE 14

Hidden Systematics…

ex:

Prior Bias?/Cut? Non Spherical? => 0.2

0.4 uncertainty Foreground Contamination? Member Star Sampling Bias?

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SLIDE 15

Hidden Systematics…

Segue1

Martinez et al., arXiv: 0902.4715

ex:

Draco

Prior Bias?/Cut? Non Spherical? => 0.2

0.4 uncertainty Foreground Contamination? Member Star Sampling Bias?

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SLIDE 16

Hidden Systematics…

ex:

Bonnivard et al., arXiv: 1407.7822 Geringer-Sameth et al., arXiv:1408.0002

Prior Bias?/Cut? Non Spherical? => 0.2

0.4 uncertainty Foreground Contamination? Member Star Sampling Bias?

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SLIDE 17

Hidden Systematics…

ex:

Prior Bias?/Cut? Non Spherical? => 0.2

0.4 uncertainty Foreground Contamination? Member Star Sampling Bias?

Bonnivard et al., arXiv: 1407.7822

Axisymmetric: Hayasi and Chiba., arXiv: 1206.3888 By K. Hayashi (Preliminary)

Spherical

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SLIDE 18

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MMFS (M. G. Walker et al,. (2007))

Prime Focus Spectroscopy

FoV 1.3 deg (diam) with 2394 Fiber

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MMFS (M. G. Walker et al,. (2007))

Prime Focus Spectroscopy

FoV 1.3 deg (diam) with 2394 Fiber

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SLIDE 20

Prime Focus Spectroscopy

#Obs Star (<V)

More accurate DM profile estimation ↓ More Robust constraints

by M. Ishigaki #Obs Star (<V)

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Strategy

  • 1. Mock Observable:

(R, v, Metalicity, Luminosity)

= dSph Stellar + Foreground

dSph Stellar Mock

Boltzmann Equation under DM profile

Foreground Mock

Besancon Model (Robin+ (2003))

  • 2. Detector Convolution:

1. fix: dv = 3.0km/s

  • 3. Fit:

(DM profile, anisotropy, dSph stellar profile, dSph v, foreground norm + metalicity)

Fit to (v, r) probability density.

Walker+, AJ 137 (2009)

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SLIDE 22

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Strategy

  • 1. Mock Observable:

(R, v, Metalicity, Luminosity)

= dSph Stellar + Foreground

dSph Stellar Mock

Boltzmann Equation under DM profile

Foreground Mock

Besancon Model (Robin+ (2003))

  • 2. Detector Convolution:

1. fix: dv = 3.0km/s

  • 3. Fit:

(DM profile, anisotropy, dSph stellar profile, dSph v, foreground norm + metalicity)

Fit to (v, r) probability density.

Walker+, AJ 137 (2009)

  • 1. Mock Samples

ρDM(r), νstar(r) => f(r,v)

Cuddeford (1991)

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SLIDE 23

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Strategy

  • 1. Mock Observable:

(R, v, Metalicity, Luminosity)

= dSph Stellar + Foreground

dSph Stellar Mock

Boltzmann Equation under DM profile

Foreground Mock

Besancon Model (Robin+ (2003))

  • 2. Detector Convolution:

1. fix: dv = 3.0km/s

  • 3. Fit:

(DM profile, anisotropy, dSph stellar profile, dSph v, foreground norm + metalicity)

Fit to (v, r) probability density.

Walker+, AJ 137 (2009)

Fit without Foreground

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SLIDE 24

24

Strategy

  • 1. Mock Observable:

(R, v, Metalicity, Luminosity)

= dSph Stellar + Foreground

dSph Stellar Mock

Boltzmann Equation under DM profile

Foreground Mock

Besancon Model (Robin+ (2003))

  • 2. Detector Convolution:

1. fix: dv = 3.0km/s

  • 3. Fit:

(DM profile, anisotropy, dSph stellar profile, dSph v, foreground norm + metalicity)

Fit to (v, r) probability density.

Walker+, AJ 137 (2009)

  • 2. Foreground

Besancon Model

  • 3. Fit

Obs

  • Prob. Density

Robin+ (2003)

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SLIDE 25

25

Strategy

  • 1. Mock Observable:

(R, v, Metalicity, Luminosity)

= dSph Stellar + Foreground

dSph Stellar Mock

Boltzmann Equation under DM profile

Foreground Mock

Besancon Model (Robin+ (2003))

  • 2. Detector Convolution:

1. fix: dv = 3.0km/s

  • 3. Fit:

(DM profile, anisotropy, dSph stellar profile, dSph v, foreground norm + metalicity)

Fit to (v, r) probability density.

Walker+, AJ 137 (2009)

  • 2. Foreground

Besancon Model

  • 3. Fit

Obs

  • Prob. Density

N = 300 700 700 w FG

Ursa Minor Like

True

Robin+ (2003)

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SLIDE 26

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Foreground Contamination

Outer Region = FG dominant How to Reduce FG stars?

~ 10 % Contamination

Bonnivard et al., arXiv:1506.08209

30 < NMem < 100

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27

Foreground Contamination

Outer Region = FG dominant How to Reduce FG stars? Cut:

  • 1. Velocity … The most effective
  • 2. Color… Not Bad
  • 3. Chemical Component… Degenerate
  • 4. Others?

~ 10 % Contamination

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SLIDE 28

28

Foreground Contamination

Outer Region = FG dominant How to Reduce FG stars? Cut:

  • 1. Velocity … The most effective
  • 2. Color… Not Bad
  • 3. Chemical Component… Degenerate
  • 4. Others?

~ 10 % Contamination

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SLIDE 29

29

Foreground Contamination

Outer Region = FG dominant How to Reduce FG stars? Cut:

  • 1. Velocity … The most effective
  • 2. Color… Not Bad
  • 3. Chemical Component… Degenerate
  • 4. Others?

~ 10 % Contamination

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SLIDE 30

30

Foreground Contamination

Outer Region = FG dominant How to Reduce FG stars? Cut:

  • 1. Velocity … The most effective
  • 2. Color… Not Bad
  • 3. Chemical Component… Degenerate
  • 4. Others?

~ 10 % Contamination

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SLIDE 31

31

Foreground Contamination

Outer Region = FG dominant How to Reduce FG stars? Cut:

  • 1. Velocity … The most effective
  • 2. Color… Not Bad
  • 3. Chemical Component… Degenerate
  • 4. Others?

~ 10 % Contamination

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SLIDE 32
  • Indirect detection is essential for DM search.
  • Gamma-ray observation of dSph can give

robust constraints on the DM annihilation cross section.

  • Investigation of stellar kinematics is important.
  • PFS will play a crucial role.

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Summary

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SLIDE 33

Thank You !

Koji Ichikawa

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In collaboration with Kohei Hayashi , Masahiro Ibe, Miho N. Ishigaki, Shigeki Matsumoto and Hajime Sugai.

PPP2015, Kyoto, Sep. 14-18, 2015