Abelardo Moralejo!for the MAGIC collaboration!

  Galactic Center!!(17 h) ApJ Lett. 638 (2006) L101!

  Perseus Galaxy Cluster !

!(25 h) ApJ 710 (2010) 634!

  Dwarf Spheroidals !

!Draco (8 h): Apj 679 (2008) 428!

!Willman 1 (16 h): ApJ 697 (2009) 1299!

!Segue 1 (30 h): JCAP 06 (2011) 035!

  Subhalos (Fermi UFOs)!

  Sustained effort in indirect dark matter searches:!

Dark Matter Searches with MAGIC!

2"MD workshop, Nov 2013! Segue-I observations with MAGIC!

  All previous MAGIC publications on dark matter searches with one telescope only (MAGIC-I)!

  Goal: improve our constraints by a factor 10!

  Stereoscopic MAGIC system since late 2009!�  Plus major upgrade finished in

2012 (M-1 camera + DAQs)!

 Observational approach:!

�  Long-term campaign on best dark matter candidate!

�  Dedicated analysis for DM searches!

3"MD workshop, Nov 2013! Segue-I observations with MAGIC!

Results first presented in Summer 2013 conferences. Paper draft in internal refereeing stage, expect submission by the end of the year ( J. Aleksić corresponding author )!

MAGIC)II"(2009)"

New"MAGIC)I"camera"(2012)"

Dark Matter Searches with MAGIC!

Segue 1!

  The most dark matter dominated object known so far!

  The least luminous dSph!

  Nearby, Northern hemisphere, culminates at 13° for MAGIC!

  Largest Jann factor after GC!

  Jann (θ < 0.15°): !  Segue 1 : 1×1019 GeV2 cm-5!

  Perseus : 3×1017 GeV2 cm-5!

  GC : 5×1020 GeV2 cm-5!

SEGUE"="Sloan"Extension"for"Galaxy"Understanding"and"ExploraFon"

Strigari"2012"arXiv:1211.7090"NFW"profiles"θ"="0.5°"

4"MD workshop, Nov 2013! Segue-I observations with MAGIC!

Observations!  January 2011 – February 2013!

  Low zenith angle (13 – 35 deg) !  Total effective observation time 157.9 h (good data)!

  No signal found (S = − 0.5 �) !

The deepest survey of any dSph by an IACT !

5"MD workshop, Nov 2013! Segue-I observations with MAGIC!

Full likelihood method!  makes use of the expected gamma-ray spectral shape to improve

constraints on flux (hence on <�v > )!

Full Likelihood Method!

NOBS","NEST"–"measured"and"esFmated"total"number"of"events"

E,"E’"–"measured"and"true"energy"

M(θ)"–"DM"model"with"parameters"θ"

Spectral"shape:" DifferenFal"rate:"

i.e."normalized"differenFal"rate"(for"background"+"signal)"

i.e."real"flux"Φ"convoluted"with"instrument"response"funcFon"(R)"

Aleksić,"Rico"&"Marcnez"JCAP"10"(2012)"032"

6"MD workshop, Nov 2013! Segue-I observations with MAGIC!

NUM"OF"EVTS" Spectral"shape"

Expected sensitivity Improvement!

BM mχ [GeV]

σv [cm3 s-1] IF

<σv>EDL [cm3 s-1] IF

<σv>EDL [cm3 s-1]

I’" 141" 3.6x10)27" 1.57" 5.65x10)23" 1.48" 1.39x10)23"

J’" 315" 3.2x10)28" 1.80" 1.01x10)23" 1.65" 1.91x10)24"

K’" 565" 2.6x10)26" 1.23" 3.91x10)23" 1.58" 8.39x10)24"

BM3" 233" 9.2x10)29" 1.89" 7.21x10)25" 1.61" 1.35x10)25"

BM4" 1957" 2.6x10)27" 2.10" 2.87x10)23" 3.81" 4.82x10)24"

MAGIC CTA

BM mχ [GeV]

σv [cm3 s-1] IF

<σv>EDL [cm3 s-1] IF

<σv>EDL [cm3 s-1]

I’" 141" 3.6x10)27" 1.57% 5.65x10)23" 1.48% 1.39x10)23"

J’" 315" 3.2x10)28" 1.80% 1.01x10)23" 1.65% 1.91x10)24"

K’" 565" 2.6x10)26" 1.23% 3.91x10)23" 1.58% 8.39x10)24"

BM3" 233" 9.2x10)29" 1.89% 7.21x10)25" 1.61% 1.35x10)25"

BM4" 1957" 2.6x10)27" 2.10% 2.87x10)23" 3.81% 4.82x10)24"

E [100 GeV]1 10

]-1

GeV

-1 s3

[cm

PP\

-3610

-3510

-3410

-3310

-3210

-3110

-3010

-2910

-2810Benckmark IBenckmark JBenckmark KBenckmark BM3Benckmark BM4

BMhist

E [100 GeV]1 10

]-1

GeV

-1 s3

[cm

PP\

-3610

-3510

-3410

-3310

-3210

-3110

-3010

-2910

-2810Benckmark IBenckmark JBenckmark KBenckmark BM3Benckmark BM4

BMhist

E [100 GeV]1 10

]-1

GeV

-1 s3

[cm

PP\

-3610

-3510

-3410

-3310

-3210

-3110

-3010

-2910

-2810Benckmark IBenckmark JBenckmark KBenckmark BM3Benckmark BM4

BMhist

E [100 GeV]1 10

]-1

GeV

-1 s3

[cm

PP\

-3610

-3510

-3410

-3310

-3210

-3110

-3010

-2910

-2810Benckmark IBenckmark JBenckmark KBenckmark BM3Benckmark BM4

BMhist

7"MD workshop, Nov 2013! Segue-I observations with MAGIC!

  IF: Improvement factor in upper limits w.r.t. simple method (comparison of integral flux after case-by-case threshold optimization) used in previous paper!

Other analysis details!

  One-sided confidence intervals, 95% C.L.!

  Free parameter: <σannv > (or τχ for decay)"

  Signal intensity bounded positive during likelihood maximization!

  mχ in the 100 GeV – 10 TeV (200 GeV – 20 TeV) range!

  Generic limits set assuming 100% BR into different annihilation (or decay) channels!

  DM distribution: Einasto dark matter density profile!  Jann = 1.1 x 1019 GeV2 cm-5 sr!

  Jdec = 2.6 x 1017 GeV cm-2 sr!

8"MD workshop, Nov 2013! Segue-I observations with MAGIC!

Annihilation channels!

MD workshop, Nov 2013! Segue-I observations with MAGIC! 9"

Spectra"from"Cembranos"et"al"PRD83"(2011)""

[GeV]�m210 310 410

]-1 s3>

[cm

v�<

-2610

-2510

-2410

-2310

-2210

-2110

-2010This work

MAGIC mono

-LATFermi

VERITAS

bb���

Annihilation: χχ bb!

MAGIC mono, 30 h Segue 1!

Preliminary"

VERITAS, 50 h Segue 1!

Fermi-LAT, 4 yrs of 15 dSphs!

Strongest limit above 3 TeV from dSphs!

10"MD workshop, Nov 2013! Segue-I observations with MAGIC!

  Note: VERITAS limits inconsistent with their claimed sensitivity! Should be a factor ~2 worse!

[GeV]�m210 310 410

]-1 s3>

[cm

v�<

-2610

-2510

-2410

-2310

-2210

-2110

-2010This work

MAGIC mono

-LATFermi

VERITAS

)qqH.E.S.S. (

bb���

H.E.S.S., 112 h Galactic Halo!

11"MD workshop, Nov 2013! Segue-I observations with MAGIC!

Annihilation: χχ bb!

Preliminary"

  HESS limits using the galactic halo are more constraining!

  Still, all limits depend on the quite uncertain DM profiles diversification of targets seems reasonable!

Annihilation: χχ µ+µ- & χχ τ+τ- !

[GeV]�m210 310 410

]-1 s3>

[cm

v�<

-2610

-2510

-2410

-2310

-2210

-2110

-2010

-µ-µ���

This work

MAGIC mono

-LATFermi

VERITAS

[GeV]�m210 310 410

]-1 s3>

[cm

v�<

-2610

-2510

-2410

-2310

-2210

-2110

-2010

-�-����

This work

MAGIC mono

-LATFermi

VERITAS

Strongest limit above 300 GeV from dSphs! Strongest limit above 550 GeV from dSphs!

Preliminary" Preliminary"

12"MD workshop, Nov 2013! Segue-I observations with MAGIC!

Decay: χ µ+µ- & χ τ+τ- !

[GeV]r m310 410

[s]

ro

2410

2510

2610

2710

2810

2910This work

Fermi-LAT

H.E.S.S

-µ+µAr

[GeV]r m310 410

[s]

ro

2410

2510

2610

2710

2810

2910This work

Fermi-LAT

H.E.S.S

-o+oAr

Preliminary" Preliminary"

Fermi-LAT, 2 yrs isotropic data!

H.E.S.S., 15 h Fornax Cluster!PAMELA best-fit!

For decaying DM galaxy clusters are in general better targets: large amounts of DM although less concentrated, but J � ρ"

13"MD workshop, Nov 2013! Segue-I observations with MAGIC!

Monochromatic Line (annihilation)!

[GeV]r m10 210 310 410

]-1 s3

v> [c

mm

<

-2910

-2810

-2710

-2610

-2510

-2410

-2310

This workH.E.S.S.Fermi-LAT

aaArrFermi-LAT, 3.7 yrs GC region!

H.E.S.S., 112 h Galactic Halo!

Preliminary"

130 GeV line!

14"MD workshop, Nov 2013! Segue-I observations with MAGIC!

Monochromatic Line (annihilation)!

[GeV]� m210 310 410

]-1 s3v>

[cm

� <

-2610

-2510

-2410

-2310This workExpected

expected�+1

expected�+2

�����

Preliminary"  Maximum deviation from null-hypothesis expectation:!

!~2σ (pre-trials) for mχ ~1.3 TeV!

15"MD workshop, Nov 2013! Segue-I observations with MAGIC!

Monochromatic Line (decay)!

[GeV]� m10 210 310 410

[s]

��

2510

2610

2710

2810

2910

3010

This work

Fermi-LAT

���3/2

�

Preliminary"

  Only existing limits (to our knowledge) above mχ ~500 GeV!

  Results from GC halo not very constraining because signal & background regions contain almost as much DM-induced γ-ray flux!

  Factor ~10 could be gained by going for clusters (also extended but not that much)!

16"MD workshop, Nov 2013! Segue-I observations with MAGIC!

  Mass splitting parameter �:!

  Degenerate � values !  Extended spectrum; softened

peak !E [GeV]

210 310 410

]-1dN

/dE

[GeV

-810

-710

-610

-510

-410

-310

-210

-110

1

10 = 1.05µ = 317.2 GeV, rm = 2.00µ = 317.2 GeV, rm = 1.05µ = 1000.0 GeV, rm = 2.00µ = 1000.0 GeV, rm = 1.05µ = 3172.0 GeV, rm = 2.00µ = 3172.0 GeV, rm

before the convolutionafter the convolution

)a(-µ+µArr

17"MD workshop, Nov 2013! Segue-I observations with MAGIC!

Virtual Internal Bremsstrahlung!

Virtual Internal Bremsstrahlung!

[GeV]r m210 310 410

]-1 s3v>

[cm

m <

-2610

-2510

-2410

-2310

-2210

= 1.05µ

= 1.50µ

= 2.00µ-µ+µArr

)a(-µ+µArr

Up to factor 50 better constraint on models with VIB!

10-25 cm3 s-1!

Preliminary"

18"MD workshop, Nov 2013! Segue-I observations with MAGIC!

19"

E [GeV]210 310 410

]-1dN

/dE

[GeV

-610

-510

-410

-310

-210

-110

1

r = 0.50*mqmr = 0.70*mqmr = 0.80*mqmr = 0.90*mqmr = 0.99*mqm

before the convolutionafter the convolution

= 1000.0 GeVrm

center!

width!

  Box edges smoothed after the convolution with the instrument energy response!

MD workshop, Nov 2013! Segue-I observations with MAGIC!

Gamma-ray Boxes!

[GeV]r m210 310 410

]-1 s3v>

[cm

m <

-2610

-2510

-2410

-2310

aaArr

aaaaAqqArr

Gamma-ray Boxes!

[GeV]r m210 310 410

]-1 s3v>

[cm

m <

-2610

-2510

-2410

-2310 = 0.10r/mqm = 0.50r/mqm = 0.70r/mqm = 0.90r/mqm = 0.99r/mqm

aaaaAqqArr

6x10-26 cm3 s-1! Significance comparable to the line!

20"MD workshop, Nov 2013! Segue-I observations with MAGIC!

Conclusions!  157.9 h of Segue 1 observations with MAGIC: deepest ever survey

of any dSph with any IACT!

  Dedicated analysis, optimized for spectra with features!

  Strongest limits on various models of dark matter annihilation/decay from dSph with IACT!

  Above certain mχ , strongest limits from dSphs!

  We are willing to collaborate in a global DM search with other gamma-ray telescopes to maximize chances of discovering or of setting the most stringent limits attainable by this kind of observations, placing a new landmark in the field.!

21"MD workshop, Nov 2013! Segue-I observations with MAGIC!