CTA as a γ-ray probe for dark matter structures:
Searching for the smallest clumps & the largest clusters
Moritz Hütten (MPP Munich)for the CTA consortium"The extreme Universe viewed in very-highenergy gamma rays 2018”, La Palma, 12.10.2018

1.

Introduction

2.

Dark Galactic DM clumps

3.

Galaxy clusters

mhuetten@mpp.mpg.de1. Introduction

2

M. Hütten, The extreme Universe 2018, La Palma | MPP

Gravitational evidence for dark matter on all scales
Reticulum II, 1504.03060

Dwarf galaxies
small scales (pc)
Baryonic matterbaryonic matterdark matter

Dark Matterlarge scales (Mpc)

3

M. Hütten, The extreme Universe 2018, La Palma | MPP

Gravitational evidence for dark matter on all scales
Reticulum II, 1504.03060

Begemann (1991)

Dwarf galaxies
small scales (pc)
Baryonic matterbaryonic matter

Milky Way-like galaxies
dark matter

Dark Matterlarge scales (Mpc)

3

M. Hütten, The extreme Universe 2018, La Palma | MPP

Gravitational evidence for dark matter on all scales
Reticulum II, 1504.03060

Begemann (1991)

Dwarf galaxies
small scales (pc)
Baryonic matterbaryonic matter

Milky Way-like galaxies
dark matter

Dark Matterlarge scales (Mpc)1702.04348

Galaxy cluster substructure
3M. Hütten, The extreme Universe 2018, La Palma | MPP

Gravitational evidence for dark matter on all scales
Reticulum II, 1504.03060

Begemann (1991)

Dwarf galaxies
small scales (pc)
Baryonic matterbaryonic matter

Milky Way-like galaxies
Galaxy clusters

dark matter

Dark Matterlarge scales (Mpc)1702.04348

Galaxy cluster substructure

Chandra/HST image of Abell 1689

3M. Hütten, The extreme Universe 2018, La Palma | MPP

The dark matter

γ-ray connection: indirect detection

NASA/G. Dinderman(mass > GeV)

4

M. Hütten, The extreme Universe 2018, La Palma | MPP

The dark matter

γ-ray connection: indirect detection

NASA/G. Dinderman(mass > GeV)

4

M. Hütten, The extreme Universe 2018, La Palma | MPP

The dark matter

γ-ray connection: indirect detection

NASA/G. Dinderman

typical astrophysical backgroundm = 500 GeV

γ-rays:(mass > GeV)

4+ straight toobserver+ no absorption
in the Galaxy- astrophysicalbackground
M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter structures on all scales
140 Mpc x 100 Mpc

500 Mpc x 375 Mpc

0.8 Mpc x 0.6 Mpc

0.4 Mpc x 0.3 Mpc

DMd(sim ensityulation)

Springel et al. (2005)
Diemand, Kuhlen,
Madau (2006)
color code:
brighter = denser

5

M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter structures on all scales
140 Mpc x 100 Mpc

500 Mpc x 375 Mpc

DMd(sim ensityulation)

0.8 Mpc x 0.6 Mpc

Springel et al. (2005)
Diemand, Kuhlen,Madau (2006)
color code:
brighter = denser

5M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter structures on all scales
140 Mpc x 100 Mpc

500 Mpc x 375 Mpc

DMd(sim ensityulation)

0.8 Mpc x 0.6 Mpc

Springel et al. (2005)
Diemand, Kuhlen,Madau (2006)
color code:
brighter = denser

5

M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter structures on all scales
140 Mpc x 100 Mpc

500 Mpc x 375 Mpc

DMd(sim ensityulation)

Satellitegalaxies0.8 Mpc x 0.6 Mpc

Springel et al. (2005)
Diemand, Kuhlen,
Madau (2006)
color code:
brighter = denser

5M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter structures on all scales
140 Mpc x 100 Mpc

500 Mpc x 375 Mpc

DMd(sim ensityulation)

Satellite
galaxies

Segue I

0.8 Mpc x 0.6 Mpc

LMC
SMC

Springel et al. (2005)
Diemand, Kuhlen,
Madau (2006)
color code:
brighter = denser

5M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter structures on all scales140 Mpc x 100 Mpc

500 Mpc x 375 Mpc

Satellitegalaxies

Segue I“Dark”
0.8 Mpc x 0.6 Mpc
clumps: toolight to trigger
star formation

DMd(sim ensityulation)

LMC
SMC

Springel et al. (2005)
Diemand, Kuhlen,
Madau (2006)
color code:
brighter = denser

5M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter structures on all scales
140 Mpc x 100 Mpc

500 Mpc x 375 Mpc

0.8 Mpc x 0.6 Mpc

0.4 Mpc x 0.3 Mpc

DMd(sim ensityulation)

Springel et al. (2005)
Diemand, Kuhlen,Madau (2006)
color code:
brighter = denser

6M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter structures on all scales
500 Mpc x 375 Mpc

0.8 Mpc x 0.6 Mpc

DMd(sim ensityulation)

0.4 Mpc x 0.3 Mpc

Springel et al. (2005)
Diemand, Kuhlen,Madau (2006)
color code:
brighter = denser

6

M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter structures on all scales
500 Mpc x 375 Mpc

DMd(sim ensityulation)

Assuming this wasPerseus cluster(d = 80 Mpc)

0.8 Mpc x 0.6 Mpc

0.4 Mpc x 0.3 Mpc

Springel et al. (2005)
Diemand, Kuhlen,Madau (2006)
color code:brighter = denser

6M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter structures on all scales
500 Mpc x 375 Mpc

DMd(sim ensityulation)

Assuming this was
Perseus cluster(d = 80 Mpc)

CTA field of view
0.8 Mpc x 0.6 Mpc (6°diameter)

0.4 Mpc x 0.3 Mpc
Central 1 Mpc of the Perseus cluster(0.7° x 0.7°)

Springel et al. (2005)
Diemand, Kuhlen,Madau (2006)
color code:brighter = denser

6M. Hütten, The extreme Universe 2018, La Palma | MPP

The dark matter sky seen from Earth (annihilation)

χχSM
SMlog (γ-ray intensity from DM annihilation), Galactic coordinates10221023
7

synthetic map
24
calculatedwith CLUMPY

101806.08639

M. Hütten, The extreme Universe 2018, La Palma | MPP

The dark matter sky seen from Earth (annihilation)

χχ

SMSM

Galactic center+ strong signal– γ-ray backgrounds(Silk and Bloemen, 1987,…)log (γ-ray intensity from DM annihilation), Galactic coordinates10221023
7

synthetic map
24
calculatedwith CLUMPY

101806.08639

M. Hütten, The extreme Universe 2018, La Palma | MPP

The dark matter sky seen from Earth (annihilation)

χχ

SM
SM

Galactic center+ strong signal– γ-ray backgrounds(Silk and Bloemen, 1987,…)

Milky Waysatellite galaxies+ no background– lower fluxes
1504.02048,1408.0002,…

log (γ-ray intensity from DM annihilation), Galactic coordinates10221023
7

synthetic map
24
calculatedwith CLUMPY

101806.08639

M. Hütten, The extreme Universe 2018, La Palma | MPP

The dark matter sky seen from Earth (annihilation)

χχSMSMDark clumps+ no background? brighter than satellites– unknown position

Galactic center+ strong signal– γ-ray backgrounds(Silk and Bloemen, 1987,…)

Milky Waysatellite galaxies+ no background– lower fluxes
1504.02048,1408.0002,…

log (γ-ray intensity from DM annihilation), Galactic coordinates10221023
7

synthetic map
24
calculatedwith CLUMPY

101806.08639

M. Hütten, The extreme Universe 2018, La Palma | MPP

The dark matter sky seen from Earth (annihilation)

χχ

SMSM

Dark clumps

Galaxy clusters+ no background? brighter than satellites– unknown position+ massive DM targets– far away
– γ-ray backgrounds

Galactic center+ strong signal– γ-ray backgrounds(Silk and Bloemen, 1987,…)

Milky Waysatellite galaxies+ no background– lower fluxes
1504.02048,1408.0002,…

log (γ-ray intensity from DM annihilation), Galactic coordinates

1022

1023
7

synthetic map
24
calculatedwith CLUMPY

101806.08639

M. Hütten, The extreme Universe 2018, La Palma | MPPThe dark matter sky seen from Earth (annihilation)

χχSMSM

Dark clumps

Galaxy clusters+ no background? brighter than satellites– unknown position+ massive DM targets– far away
– γ-ray backgrounds

Galactic center+ strong signal– γ-ray backgrounds(Silk and Bloemen, 1987,…)

Milky Waysatellite galaxies+ no background– lower fluxes
1504.02048,1408.0002,…

log (γ-ray intensity from DM annihilation), Galactic coordinates10221023
7

synthetic map
24
calculatedwith CLUMPY

101806.08639

M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter clumpiness matters!

χSMχ

SMAnnihilation

χDecaySMSM

8M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter clumpiness matters!
Flux searched for with γ-ray telescope

χSMχ

SMAnnihilation

χ

Decay

SM
SM

8M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter clumpiness matters!
Secondary γ-rays after annihilation/decay

χSMχ

SMAnnihilation

χ

Decay

SMSM

8M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter clumpiness matters!

χSMχ

SMAnnihilation

χDecaySMSMUnknown DM particle mass: parameter

8M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter clumpiness matters!
Annihilation cross section

χSMχ

SMAnnihilation

χDecaySM
SMParticle lifetime

8M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter clumpiness matters!

χSM

χ

SM

Annihilation

χDecaySM
SM

Density distribution

8M. Hütten, The extreme Universe 2018, La Palma | MPP

Dark matter clumpiness matters!

χSMχ

SMAnnihilation

χDecaySMSM

Density distribution

What density targets do we need for CTA?
1. Bright: close and/or massive DM budget
2. Localized (“point-like”)
3. no astrophysical back-/foregrounds
8

M. Hütten, The extreme Universe 2018, La Palma | MPP

2. Dark Galactic DM clumps

9M. Hütten, The extreme Universe 2018, La Palma | MPP

χχDark clumps annihilation brightness

SMSM‣ Brightness in γ-rays (J-factor):
conservative

Hütten, Combet, Maier, Maurin (2016)

104

flux from annihilation ~counting all objects

11103 10 10J)

10[cm 2 s 1 sr 1 GeV 1 ]NX(101210 9 10 1110 1010 910 8[cm 2 s 1 sr 1 GeV 1 ]10 10

10 91010
optimistic
87[cm 2 s 1 sr 1 GeV 1 ]102counting all objects

101

10 12

Estimated J-factors ofknown satellite galaxies

10 1110 10[cm 2 s 1 sr 1 GeV 1 ]10 9 10 11

10 10

10 9

[cm 2 s 1 sr 1 GeV 1 ]100
10 11017
many faint objects

1018

1019
1020
J-factor [GeV2 cm 5 ]101021few bright objects

M. Hütten, The extreme Universe 2018, La Palma | MPP1χχDark clumps annihilation brightnessSMSM‣ Brightness in γ-rays (J-factor):
Close-by
Hütten, Combet, Maier, Maurindar(2016)kbrigh clumps
t DM
flux from annihilation ~targets

conservative
104
counting all objects

11103 10 10J)

10[cm 2 s 1 sr 1 GeV 1 ]NX(101210 9 10 1110 1010 910 8[cm 2 s 1 sr 1 GeV 1 ]10 1010 91010
optimistic
87[cm 2 s 1 sr 1 GeV 1 ]102counting all objects

101

10 12

Estimated J-factors ofknown satellite galaxies

10 1110 10[cm 2 s 1 sr 1 GeV 1 ]10 9 10 1110 1010 9[cm 2 s 1 sr 1 GeV 1 ]10010 11017
many faint objects

1018

1019
1020
J-factor [GeV2 cm 5 ]101021few bright objects

M. Hütten, The extreme Universe 2018, La Palma | MPP1χ
χ

Dark clumps annihilation profiles

SMSM

log Intensity

half-lightradius ~ 0.14°

conservativel [deg]clumpy code, 1806.08639

b [deg]‣ Take advantage of CTA’s excellent angular resolution
11M. Hütten, The extreme Universe 2018, La Palma | MPPχχ

Dark clumps annihilation profiles
half-lightradius ~ 0.14°

SMSM

log Intensity

Pointemis -likesion
fromdarkclum
psconservative

l [deg]clumpy code, 1806.08639

b [deg]‣ Take advantage of CTA’s excellent angular resolution
11M. Hütten, The extreme Universe 2018, La Palma | MPP

But how to find the dark clumps?
‣ In a survey:
Observing 25% of the sky with 500 hours (extragalactic survey benchmark):

25% of sky

γ-ray brightest subhalo in thefield (assume it is a dark clump)

1022

1023
121024M. Hütten, The extreme Universe 2018, La Palma | MPP

But how to find the dark clumps?
‣ In a survey:
Observing 25% of the sky with 500 hours (extragalactic survey benchmark):‣ Chance detection

1022approximate CTA
236° diameter FOV

10121024

M. Hütten, The extreme Universe 2018, La Palma | MPP

Survey sensitivity based on CTA South (prod2-3)
5%500h, 9χ
χ

SM
SM

C.L.

(Hütten, Combet, Maier, Maurin, 2016)

1017

CTA dark subhalos, model HIGH

10 181020h vi [cm3 s 1 ]1019

CTA dark subhalos,! bb̄! bb̄

Di↵erent targets,LOW (post-trial)

VERITAS, stacked dSph
MAGIC, Segue 1 (158h)

HIGH (post-trial)
LOW(post-trial)! ⌧bb̄+ ⌧! bb̄

HIGH (post-trial)(pre-trial)

H.E.S.S., Gal. halo (254h)
Fermi -LAT, stacked dSph
CTA dark subhalos (HIGH)

10 21
10 22
10Cosmic variance

23

68%

10 24

95%

10 25
10 26
10 27

thermal relic cross section

102

103
104
WIMP mass m [GeV]

105 102

103
104
WIMP mass m [GeV]
13105 102

103
104
WIMP mass m [GeV]105

M. Hütten, The extreme Universe 2018, La Palma | MPPχχSurvey sensitivity based on CTA South (prod2-3)
5%500h, 910171020h vi [cm3 s 1 ]10(Hütten, Combet, Maier, Maurin, 2016)

CTA dark subhalos, model HIGH

! bb̄

CTA dark subhalos,! bb̄

Di↵erent targets,LOW (post-trial)conservative
model
LOW
HIGH (post-trial)(post-trial)! ⌧bb̄+ ⌧10 22 10 1223

10 1110 10[cm 2 s 1 sr 1 GeV 1 ]HIGH (post-trial)(pre-trial)
optimistic
model

10 9 10 11

10 24

10 1010 910 8[cm 2 s 1 sr 1 GeV 1 ]! bb̄

VERITAS, stacked dSph
MAGIC, Segue 1 (158h)
H.E.S.S., Gal. halo (254h)
Fermi -LAT, stacked dSph
CTA dark subhalos (HIGH)

10 2110SM

C.L.

10 1819SM

10 1010 910 810 7[cm 2 s 1 sr 1 GeV 1 ]Modeling systematics

10 25
1010 1226

10 27

thermal relic cross section

102

103
104
WIMP mass m [GeV]

105 102

103
104
WIMP mass m [GeV]14105 102

10 1110 10[cm 2 s 1 sr 1 GeV 1 ]103
104
WIMP mass m [GeV]

10 9 10 11105

M. Hütten, The extreme Universe 2018, La Palma | MPP

Survey sensitivity based on CTA South (prod2-3)
5%500h, 910171020

SM(Hütten, Combet, Maier, Maurin, 2016)

CTA dark subhalos, model HIGH

CTA dark subhalos,! bb̄! bb̄

Di↵erent targets,LOW (post-trial)conservative
model
LOW
HIGH (post-trial)(post-trial)! ⌧bb̄+ ⌧! bb̄

VERITAS, stacked dSph
MAGIC, Segue 1 (158h)
H.E.S.S., Gal. halo (254h)
Fermi -LAT, stacked dSph
CTA dark subhalos (HIGH)

HIGH (post-trial)(pre-trial)
optimistic
modelh vi [cm3 s 1 ]

10SM

C.L.

10 1819

χχ

10 21
10 22
10 23
10 24
10 25
10 2610 27

thermal relic cross section

102103104
WIMP mass m [GeV]

105 102

103
104
WIMP mass m [GeV]
15105 102

103104
WIMP mass m [GeV]105

M. Hütten, The extreme Universe 2018, La Palma | MPP

Survey sensitivity based on CTA South (prod2-3)
5%500h, 910

17

1018

SM
SMC.L.
(Hütten, Combet, Maier, Maurin, 2016)

CTA dark subhalos, model HIGH

CTA dark subhalos,! bb̄

Di↵erent targets,! bb̄

CTA Segue 1 (500h)
! bb̄

10 19

CTA Gal. halo (500h, Einasto)
VERITAS, stacked dSph
MAGIC, Segue 1 (158h)
H.E.S.S., Gal. halo (254h)
Fermi -LAT, stacked dSph
CTA dark subhalos (HIGH)

LOW (post-trial)conservativemodel
HIGH (post-trial)
LOW(post-trial)! ⌧bb̄+ ⌧HIGH (post-trial)(pre-trial)
optimistic
model

20h vi [cm3 s 1 ]

10χχ

10 21
10 22
10 23
10 24
10 25
10 26
10 27

thermal relic cross section

102

103
104
WIMP mass m [GeV]

105 102

103
104
WIMP mass m [GeV]
16105 102

103
104
WIMP mass m [GeV]105

M. Hütten, The extreme Universe 2018, La Palma | MPPχχChance detection probability: “Subhalo algebra”

SMSM

1. Number of detectable objects rises linearly with ΔΩ : geometry + isotropy
2. Number of detectable objects rises with sqrt(Tobs): instrument background
3. Number of detectable objects rises inversely with sensitivity thresholdNobjects(≥ Fsens) ~ 1/Fsens : subhalo source count distribution
See Hütten et al. (2016), App. E, for details

ΔΩNFOVTobs/FOV<σv>

Nspots(≥ 2σ)

π300

100 min10-24 cm3 s-1

110-2

1100 min10-24 cm3 s-1

3·10-310-211000 min10-24 cm3 s-1

1·10-210-21100 min10-23 cm3 s-1

3·10-2

17M. Hütten, The extreme Universe 2018, La Palma | MPP

3. Galaxy clusters

18M. Hütten, The extreme Universe 2018, La Palma | MPP

The case of galaxy clusters: DM annihilation
Recall:SMAll Galactic
clumps103J)

SM1104.3530

104

NX(χχ

102
101
10010 1dwarf galaxies
1017

1018

1019
1020
25J-factor [GeV cm ]1021

19M. Hütten, The extreme Universe 2018, La Palma | MPP

The case of galaxy clusters: DM annihilation
Recall:SMAll Galactic
clumps103J)SM1104.3530

104NX(χχ

102101100
10 1dwarf galaxies
1017

1018

1019
1020
25J-factor [GeV cm ]1021

‣ DM-annihilation brightness comparable to satellite galaxies

19M. Hütten, The extreme Universe 2018, La Palma | MPP

The case of galaxy clusters: DM annihilation

χχSM
SM1104.3530‣ DM-annihilation brightness comparable to satellite galaxies‣ Emission profiles more extended (typical half-light radii > 0.5°)19

M. Hütten, The extreme Universe 2018, La Palma | MPP

The case of galaxy clusters: DM annihilation

χχSMSM1104.3530‣ DM-annihilation brightness comparable to satellite galaxies‣ Emission profiles more extended (typical half-light radii > 0.5°)‣ Astrophysical backgrounds:• γ-ray emitting galaxies (AGN, star-forming galaxies, CR interaction)• Also expect diffuse emission from the inter-cluster medium (ICM)

19M. Hütten, The extreme Universe 2018, La Palma | MPP

3 orders of magnitude

DM annihilation profile of the Perseus clusterχχSM
SM0.5°

Intensity proportional towithout substructure
random triaxiality
20M. Hütten, The extreme Universe 2018, La Palma | MPP

3 orders of magnitude

DM annihilation profile of the Perseus cluster

χχSMSMMAGIC, E > 250 GeV
1602.03099

0.5°

275
1GNC

IC031

Intensity proportional towithout substructure
random triaxiality
20M. Hütten, The extreme Universe 2018, La Palma | MPP

3 orders of magnitude

DM decay profile of the Perseus clusterχSMSM

MAGIC, E > 250 GeV
1602.03099

0.5°

275
1GNC

See MAGIC result
1806.11063:
τDM ≥ 1027 sIC

031

Intensity proportional torandom triaxiality(substructure irrelevant)
21M. Hütten, The extreme Universe 2018, La Palma | MPP

Cosmic-ray induced emission in the inter-cluster medium
Spatial profile

Spectral profile
1001.5023

1709.07997

ncexp

EnExcpeiotat

iotat0.1°
0.2°‣ CTA’s excellent angular resolution
and energy range:
disentangle the signals‣ DM substructure extends
annihilation profile
22M. Hütten, The extreme Universe 2018, La Palma | MPP

The CTA galaxy cluster working group (wg-phys-clusters)‣ CTA galaxy cluster key science project: 300 hours allocated for CTA North‣ Coordination:• Moritz Hütten (MPP Munich)• Judit Pérez-Romero, Miguel Sánchez-Conde (UAM Madrid)‣ The team:
R. Alfaro, G. Brunetti, S. Colafrancesco, C. Delgado, M. Doro, E. Fedorova, E. deGouveia Dal Pino, S. Hernandez Cadena, M. Hütten, M. Lallena, S. Nuza, J.
Pérez, O. Reimer, M. Sánchez-Conde, S. Zimmer‣ Updated performance study on galaxy clusters in progress

23

M. Hütten, The extreme Universe 2018, La Palma | MPP

Conclusions‣ Hierarchical DM clustering:
γ-ray clumps from annihilation/decay at various scales and distances‣ Search for the smallest clumps in a TeV γ-ray survey with CTA(extragalactic key science project by-catch)‣ Watch out for unidentified sources in the FOV: may be a Galactic DM clump‣ Study the closest galaxy clusters:
Perseus and Coma: Excellent observation conditions with CTA North‣ Clusters: Constrain DM particle life times beyond τDM > 1027 s = 2·109 t Universe
CTA excellent probe for TeV dark matter particle physics
in various complementary targets
24

M. Hütten, The extreme Universe 2018, La Palma | MPP

BACK UP25

M. Hütten, The extreme Universe 2018, La Palma | MPP

Perseus cluster also optimal target for DM decay

χ

SMSM

1709.07997

Perseus =1203.1164

1806.11063‣ Perseus region already extensively
studied by MAGIC telescopes:
0909.3267, 1009.2155, 1111.5544,
1310.8500, 1602.03099,1806.11063: τDM ≥ 1027 s
26

M. Hütten, The extreme Universe 2018, La Palma | MPP

Astrophysical merits of Perseus cluster observations

1709.07997

27

1709.07997

M. Hütten, The extreme Universe 2018, La Palma | MPP

Brightest Galactic DM clumps: Properties‣ Average mass and distance (from 104 runs):
Median properties ofMedian properties ofbrightest subhalo withinbrightest subhalo withinÂ ı [kpc]
Dı [kpc]Â obs
Dobs
Â ıvirlog10 (m/M )Â ıvir /M§
log110 (m§) 2
2
log10 1JÂÂıı/GeV22 cm≠5log10 J /GeV cm≠5References
Median properties ofbrightest subhalo within

Fermi-LAT scenario
Fermi-LAT scenario(fsky = 82.6%)(fsky ¶= 82.6%) ¶◊int = 0.1¶ ◊int = 0.8¶
◊int = 0.1◊int = 0.8+117+108+10+11≠67≠58≠5≠6+1.2
7.7+1.3
8.1+1.3+1.2≠1.6
7.7≠1.5
8.1
≠1.5
≠1.6
+0.4
20.3+0.4
20.7
+0.4
+0.4
≠0.3
20.3≠0.3
20.7
≠0.3
≠0.3
Fermi-LAT scenario(fsky = 82.6%)◊int = 0.1¶ ◊int = 0.8¶

χ
χ

SMSM

optim

istic
CTA scenario
CTA scenario(fsky = 25%)
(fsky ¶= 25%)
◊int = 0.05¶ ◊int = 0.1¶¶◊int = 0.05
◊int = 0.1+127+10
8+10+12≠6
7≠5
8≠5≠6+1.4
7.4+1.4
7.6
+1.4
+1.4
≠1.5
7.4≠1.4
7.6
≠1.4
≠1.5
+0.4
19.7+0.3
19.9+0.3+0.4≠0.3
19.7≠0.3
19.9
≠0.3
≠0.3
conseCTA scenario(fsky = 25%)
◊int = 0.05¶ ◊int = 0.1¶

rvati

ve+42+42+27 L., Barbiellini,+26 G.,
Â ıet al.,[Ackermann
2015]
Ackermann,
M.,
Ajello,M.,
Albert,A.,
Baldini,
3230
20
19
D
[kpc]
≠23
≠22
≠15
≠14
obs
Bastieri, D., Bechtol, K., Bellazzini, R., Bissaldi, E., Bloom, E. D., Bonino, R., Bregeon,+0.9+0.9+0.8+0.9
Â ıvirlog10 (P.,m/M§ ) R., Buson,
8.7S.,
8.6
8.7
8.7
J., Bruel,
Buehler,
Caliandro,G.
A.,
Cameron,R.
A.,
Caragiulo,
≠1.3
≠1.3
≠1.4
≠1.4 M.,
1 P. A., Cecchi, C.,
2 Charles, E., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S.,
Caraveo,+0.3+0.3+0.3+0.4
Âı /GeV2 cm≠5log
J
18.9
19.1
19.4
19.8
Claus,J., Cuoco, A.,≠0.3
Cutini, S., D’Ammando,
F., deAnge10 R., Cohen-Tanugi, J., Conrad,≠0.2≠0.3≠0.3lis, A., de Palma, F., Dermer, C. D., Digel, S. W., Drell, P. S., Drlica-Wagner, A., Favuzzi,C., Ferrara, E. C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giordano, F., Giroletti, M., Godfrey, G., Guiriec, S., Gustafsson,
28
M. Hütten, The extreme Universe 2018, La Palma | MPP
References
M., Hewitt, J. W., Hou, X., Kamae, T., Kuss, M., Larsson, S., Latronico, L., Longo, F.,Dark clumps decay brightness

χSM
SM

Number of subhalos brighter than a given flux/ J-factor:CTA survey sensitivity= 1026s, m = 500 GeV
10 4
10 3

103
102
101
100
10 1
25% of the sky,
dwarf-like objects included

10 215

Sculptor dSphG# of subhalos
than JNsub(brighterD)

104

flux > 100 GeV in Crab units for ! bb̄,⌧
10 7
10 6
10 5

16
17
18
19
Astrophysical D-factor in log10(D/GeV cm 2)!29

model 1model 2model 3model 4model 5model 6
4 parametersmodel
7model168 models
model
9 lines:dashedmodel
10 c(M)highermodel 11model 12
work done bymodel 13Rumodel 14 ngployphan
ieokaewmodel K15, 2015
model 16

20M. Hütten, The extreme Universe 2018, La Palma | MPP