magic highlights - in2p3vietnam.in2p3.fr/.../wednesdaymorning/lopez-coto.pdfrubén lópez-coto -...

Rubén López-Coto - IFAE, BarcelonaVery high energy phenomena in the Universe - Quy Nhon - 06/08/14

MAGIC Highlights

1

Rubén López-Coto - Very high energy phenomena in the universe - Quy Nhon - 06/08/14

Overview

The MAGIC telescopes

Galactic sources• Crab nebula and pulsar• The PWN 3C 58

Extragalactic sources• IC 310 radiogalaxy

Dark matter searches• Segue1

Future prospects

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The MAGIC telescopes

The MAGIC Collaboration: 170 collaborators in 10 countries.Stereo system of two Imaging Atmospheric Cherenkov telescopes (IACTs) (MAGIC-I 2004, MAGIC-II 2009).17m diameter reflectors.Light weight ➜ fast movement to catch GRBs (20s/180º).The telescopes were recently upgraded to homogenize the system.

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The MAGIC locationThis is

still Spain

Observatory

The Canary Island of La Palma (Spain) hosts one of the best astronomical observatories in the world.

The Observatory “Roque de los Muchachos” is at 2200 m a.s.l. It has one of the clearest skies in the world.

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MAGIC UpgradeWe had two different telescopes making the maintenance and operation twice as difficult We exchanged:

• M1 camera (577 pixels (different sizes) -> 1039 pixels)

• M1 trigger region size was increased by 70%

• Readout system (dead time reduction from 500 μs to 26 μs)

M1 new camera

DRS4 readout

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M1 new trigger


Performances of upgraded system today:

Trigger threshold reduced to ~50 GeV (low zenith observations). Analysis threshold down to 70 GeV.

Forthcoming publication

MAGIC Performance

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Energy resolution 15%-23% below 10 TeV

Angular resolution <0.07˚ above 300 GeV

Sensitivity 0.6% Crab Nebula flux in 50 hours


SCIENTIFIC HIGHLIGHTS

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GALACTIC SOURCES

SNRs

Pulsars

Binary systems PWNe

(MAGIC Analysis Reconstruction Software)

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Crab Pulsar

J. Aleksić et al. (MAGIC Coll.), A&A. 540 (2012) 69

MAGIC discovered pulsed gamma-ray emission above 25 GeV (Science, 2008, 322, 1221).

VERITAS detected this emission above 100 GeV (Science, 2011, 334, 69)

MAGIC extended the spectrum up to 400 GeV (A&A, 2012, 540, 69) and separately measured the spectrum of P1 and P2.

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N. E

vent

s

135014001450150015501600165017001750 MAGIC, 46 - 138 GeV Entries 74828

= 4366.8 minobsT) = 85.07 (6.210

2Z)H Test = 56.30 (5.7)/ndf = 116.80/50 (5.12

= 759+-93 Sig = 8.3exN

N. E

vent

s

135014001450150015501600165017001750

Phase0 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2

P1P2 P2OFF

N. E

vent

s

700

750

800

850

900

950

1000MAGIC, 138 - 416 GeV Entries 39406

= 4366.8 minobsT) = 59.88 (4.510

2Z)H Test = 23.88 (4.0)/ndf = 88.79/50 (3.42

= 416+-68 Sig = 6.2exN

N. E

vent

s

700

750

800

850

900

950

1000

N. E

vent

s

2100

2200

2300

2400

2500

2600

2700 MAGIC, 46 - 416 GeV Entries 114234 = 4366.8 minobsT

) = 128.85 (8.6102Z

)H Test = 103.33 (6.4)/ndf = 170.19/50 (7.72

= 1175+-116 Sig = 10.4exN

N. E

vent

s

2100

2200

2300

2400

2500

2600

2700


Crab Bridge

PhaseExce

ss C

ount

s/(B

in W

idth

/0.0

05)

0

50

100

150

200

250

50 - 100 GeV

P1 P2

0

50

100

150

200

250

100 - 400 GeV

Phase-1 -0.8 -0.6 -0.4 -0.2 0 0.2 0.4 0.6 0.8 1

0

100

200

300

400

500

50 - 400 GeV

Energy [GeV]-110 1 10 210 310

]-1

s-2

[TeV

cm

dEdA

dtdN

2 E

-1410

-1310

-1210

-1110

-1010

MP1 MP2

MBridge

EBridgeNebula

J. Aleksić et al. (MAGIC Coll.), A&A, 565 (2014) L12

The bridge emission was detected with a significance above 6 σ for energies above 50 GeV

J. Aleksić et al. (MAGIC Coll.), A&A, 565 (2014) L12

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50-100 GeV

100-400 GeV

50-400 GeV

Recently, MAGIC has discovered VHE emission from the bridge region between the two peaks extending beyond 100 GeV


(A couple of)VHE pulsar models

Aharonian, F. et al., Nature 482 (2012) 507

Hirotani, K., ApJ, 733 (2011) L49Hirotani, K., ApJ, 766 (2013) 98

VHE gamma rays are produced inside the magnetosphere in an “outer gap”

It can explain the spectrum extending up to 400 GeV and also the bridge emission if the magnetic field also has a toroidal component.

It proposes that VHE gamma-rays are produced in the wind region.

Predicts bridge emission but broader peaks than observed.

Cold ultrarelativistic wind

Outer gap

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The Crab Nebula

Aleksić et al. JHEAP submitted (arXiv:1406.6892)

New results with 70 hours of stereo observations (2009-2011)

Spectrum extends from 50 GeV to ~30 TeV (statistical error 5% at 100 GeV)

In combination with Fermi-LAT, the IC peak is measured at 53±3stat GeV with a bad χ2, showing that the log-parabola is not a good representation of the IC peak

All the tested models have too simplistic assumptions and none of them can explain the MW spectrum of the Crab nebula

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E (GeV)

)-1

s-2

(TeV

cm

dEdA

dtdN

2 E

-1610 -1410 -1210 -1010 -810 -610 -410 -210 1 210 410

-1210

-1110

-1010

-910

-810

-710MAGIC dataFermi-LAT dataRadio - X-ray dataMTR model (total)MTR (Sync)MTR (Bremsstr.)MTR (SSC)MTR (NIR)MTR (FIR)MTR (CMB)

E (GeV)

)-1

s-2

(TeV

cm

dEdA

dtdN

2 E

-110 1 10 210 310 410

-1210

-1110

-1010

-910 MAGIC data

Systematic uncertainty

Fermi-LAT data

MTR model (total)


The PWN 3C 58Centered in PSR J0205+6449 ➜ One of the highest spin-down pulsars in the sky: E(dot)=2.7×1037 erg s-1 (5% Crab pulsar).

3C 58 has been compared to Crab due to the jet-torus morphology ➜ One of the classical sources considered to emit gamma rays.

Distance 3.2 kpc or 2kpc Age: 2.5 kyr?

Discovered by Fermi at gamma rays in 2013 with a spectrum extending beyond 100 GeV.

Up to now, there were only upper limits (lowest at 2.3% Crab) at VHE by Whipple, VERITAS and MAGIC

NASA/SAO/CXC/J.Drake et al

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Rubén López-Coto - Very high energy phenomena in the universe - Quy Nhon - 06/08/14Energy [GeV]

-110 1 10 210 310 410

]-1

s-2

/dE

[TeV

cm

! d2 E

-1410

-1310

-1210

-1110

-1010

-910MAGIC, this work3C58 Fermi points (Abdo et al. 2013)3C58 Fermi points (Ackermann et al. 2013)3C58 SED from panel 3 of Fig. 1 in Torres et al. (2013)3C58 SED Fig. 10 in Bednarek & Bartosik (2003)2.5 kyr for 3C58 SED Fig. 1 in Tanaka & Takahara (2013)1 kyr for 3C58 SED Fig. 2 in Tanaka & Takahara (2013)Systematic uncertainty

Aleksić, J. et al., A&A 567 (2014) L8

MAGIC discovered a VHE gamma-ray source at the position of 3C 58 (MAGIC J0205+6451) after 81 hours of observations in 2013-2014

We extended the spectrum up to a few tens of TeV.Above 400 GeV the spectral index is 2.4

Integral flux above 400 GeV is 0.65% Crab (weakest PWN detected at TeV).

MAGIC got it!

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Only models assuming a 2 kpc distance to 3C 58 or an unexpectedly high FIR energy density fit the gamma-ray data ➞ We favor 2 kpc distance.All the models derive magnetic fields lower than 35 μG.3C 58 is the PWN with the lowest luminosity and the less efficient PWN ever detected at TeV energies to date.

[erg/s]E3610 3710 3810 3910

Lum

inos

ity (E

>1 T

eV) [

erg/

s]

3310

3410

3510

3610

E -3

= 10!L

E -4

= 10!L

E -5

= 10!L

VHE PWNe detected at TeV energies

MAGIC J0205+6451 (3C 58)

Crab nebula

3C58 amongst the PWNe detected at VHE

Preliminary

Plot by R. López-Coto

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EXTRAGALACTIC SOURCES

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The Radiogalaxy IC 310Discovered at VHE on Fermi data (Neronov, A., Semikoz, D., & Vovk, I.2010, A&A, 519) and MAGIC (ApJ, 723 (2010) L207)

Same field of view as the radiogalaxy NGC1275 (also discovered at VHE by MAGIC) -> Both of them in the Perseus cluster.

IC 310 showed day-to-day variability in 2011(A&A 563 (2014) A91).Aleksić, J. et al., A&A, 541 (2012) 99.

NGC 1275

IC 310

MAGIC: Submitted

During flare in 2012 variability was observed with a timescale of 9.5±1.9 min and large amplitude flickering in time scales of the order of minutes

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~10 min gaussian variability

~1 min flickering

1 crab

5 crabs

Preliminary


Jet

Obscuring Torus

Black Hole

Narrow Line Region

Broad Line Region

Accretion Disk

Fast variability

18 ASTROPARTICLE PHYSICS 2014

For a 3×108 M⊙ BH, time flickering of the order of minutes is below the event horizon light-crossing-time

Similar fast variability has been found in VHE Blazars like Mrk 501 or PKS 2155-304 but they have Doppler factors of ~50. IC 310 can have a Doppler factor of 3 – 4 with the jet at 10˚-20˚ from the line of sight. Intrinsic variability is much shorter in IC 310.

Emission seen by MAGIC hard to explain by models:

• Shocks in the Jet? But difficult to explain the event horizon light-crossing-time measured

• Minijets in the Jet pointing towards the line of sight? But it would make luminosity of IC 310 huge

• Jets crossing dense matter clouds or stars? But crossing and pp cooling times are typically longer

Credit: C.M. Urry and P. Padovani


S3 0218+357Farthest AGN ever detected

19 ASTROPARTICLE PHYSICS 2014

S3 0218+357 is a blazar that underwent a series of flares separated 11.5 days, interpreted as due to the gravitationally lensed effect

Detection of a flare by MAGIC at the expected time of arrival of the Fermi gravitationally lensed component

z=0.944 ➞ breaking distance records: the most distance source ever detected at VHE


DARK MATTER

Millenium Simulation, MPA Garching, V. Springel, S. White et al.

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The Target: Segue 1

Ultra-faint satellite galaxy

The most dark matter dominated object known so far

The least luminous galaxy known

Close, no conventional gamma-ray sources expected, Northern Hemisphere

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MAGIC ObservationsMAGIC observed Segue 1 for 158 h during 2011-2013 (JCAP 02 (2014) 008).

➞ Deepest observation of a dSph by an IACT to date.

No hint of signal in the whole dataset.

Distribution of events vs distance to signal/background region center

Upper limits to differential gamma-ray flux

Aleksić, J. et al. JCAP 02 (2014) 008Aleksić, J. et al. JCAP 02 (2014) 008

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Full likelihood analysis (Aleksić, Rico & Martinez, JCAP 10 (2012) 032) method optimized to recognize spectral features like those expected from DM annihilation and decay

Computed upper limits to the annihilation and lower limits to the decay into secondary standard model particles.

χχ → τ+τ−

[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

Search for gamma-rays

Strongest limit above 600 GeV from dSphs

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The Future of MAGICSTEREO SUM TRIGGER

TOPO-TRIGGERNew concept of stereo trigger based on the NSB rejection using the position of the showers in each camera.

Allows reduction of the discriminator threshold improving the collection area at the lowest energies.

Also installed and being commissioned. TOPO-TRIGGER BOARD

Further improvements: We want to go to even lower energies!

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SUM TRIGGER-II

Same concept as used for the Crab pulsar discovery.

Stereo trigger threshold down to 30 GeV.

Already installed and currently being commissioned.


To sum up...Telescopes in good shape to continue producing scientific results for several years. System with a better performance than ever.

Currently running more ambitious Key Science Programs ➞ They will be the MAGIC legacy for the scientific community.

We are currently having very exciting and novel results:Source discoveries: 3C 58, S3 0218+357, MS1221.8+2452, RBS 0723, RX J1136.5+6737.Deep studies of known sources: Crab nebula, LS I +61º 303, Mrk 421, Mrk 501, DM searches...Surprises as IC 310 extreme variability...

What has the future waiting for us?GRB detection? ➞ Stay tuned!!

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Thanks!!!

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magic highlights - in2p3vietnam.in2p3.fr/.../wednesdaymorning/lopez-coto.pdfrubén lópez-coto -...

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