MAGIC: from Astrophysics to Fundamental Physics ...

MAGIC: from Astrophysics to MAGIC: from Astrophysics to Fundamental Physics. Fundamental Physics.

Presentation of the latest resultsPresentation of the latest results

Camilla MaggioCamilla Maggiofor the MAGIC collaborationfor the MAGIC collaboration

ICNFP2018

C.Maggio-MAGIC - ICNFP2018 2

OUTLINEOUTLINE

I. Introduction to MAGIC experimentII. Astrophysical searches

● Galactic● Extragalactic● Multimessenger

III. Fundamental Physics studies● Lorentz Invariance Violation● Dark Matter

IV.Conclusions


MAGIC COLLABORATIONMAGIC COLLABORATION

180180 260260


MAGIC TELESCOPESMAGIC TELESCOPES● La Palma, Spain● Observatorio del Roque

de los Muchachos (ORM)● ~2200m a.s.l.

● Two Imaging Atmospheric Cherenkov Telescopes (IACTs) with 17m diameter dishes

● Activity started in 2003, with M1 only (mono data)● Upgrade to stereo data in 2009, M2 construction● Energy range: 70GeV-30TeV (with standard trigger),

extended down to 30GeV low limit (thanks to the sum-trigger) and to >100TeV (in very large zenith angle mode)

● Angular resolution < 0.08° for energies E≥200GeV● Fast repositioning: < 30s for 180°

15 years of work! - Happy Birthday MAGIC!15 years of work! - Happy Birthday MAGIC!


MAGIC SENSITIVITYMAGIC SENSITIVITY

● Mono-phase:- Light Gray circlesLight Gray circles: first installation (2005)- Dark grayDark gray: different

readout system (2008)• Stereo-phase: - Black trianglesBlack triangles: stereo phase 1 (2010) - Squares: stereo after camera upgrade:

• zenith angle below 30° (red, filledred, filled),

• 30°−45° zenith angle (blue,emptyblue,empty)• Sum-trigger: allowed energy threshold < 50GeV (~30GeV) (pink squares, filledpink squares, filled)

+ Very Large Zenith Angle (VLZA) observations+ Moon data acquisition


MAGIC – Major Atmospheric MAGIC – Major Atmospheric Gamma Imaging CherenkovGamma Imaging Cherenkov

The Cherenkov The Cherenkov TechniqueTechnique


VERY HIGH ENERGY UNIVERSEVERY HIGH ENERGY UNIVERSE

211 observablesources!!!

IACT miracle!


MAGIC SOURCESMAGIC SOURCES

Cre

dits

: M

.Do

ro -

CR

IS2

01

8

Dark Catalogue (many sources

pointed and not detected)

• MAGIC is in the N-hemisphere: optimized for extra-gal. physics

60 s

ources

42 s

ources

18 s

ources


ASTROPHYSICSASTROPHYSICS

‘So remember to look up at the stars and not down at your feet. Try to make sense of what you see and wonder about what makes a universe exist. Be curious.’

S. Hawking


GALACTIC – CRAB PULSARGALACTIC – CRAB PULSAR● Discovery of the first VHE pulsar, the Crab pulsar, in 2008 (signal above 25GeV)● MAGIC detection of power low tail in 100GeV-400GeV energy range in Aleksić et al., ApJ 742 (2011), 43,

confirming the detection of VERITAS of the same year ● Detection of bridge emission (above 50GeV) in 2014 by MAGIC (Aleksić et al.,A&A 565(2014), 12) ● Detection up to 1.5 TeV in 2016

● Used 8 years of Standard trigger data: 320h● Spectra of both peaks extending as power-laws far beyond the expected cutoffs:

● P1 detected up to 0.6 TeV (Γ=3.5 ± 0.1)● P2 detected up to 1.5 TeV (Γ=3.0 ± 0.1)

● Polar cap ruled out, and other models questioned Led to rewriting of pulsar models➔

Teraelectronvolt pulsed emission from the Crab pulsar detected by MAGICAstron.Astrophys. 585 (2016) A133

Teraelectronvolt pulsed emission from the Crab pulsar detected by MAGICAstron.Astrophys. 585 (2016) A133


GALACTIC – SNR & GALACTIC – SNR & MICROQUASARMICROQUASAR

Particle acceleration efficiency

Ruled out steady VHE emission above 200GeV (interaction between the relativistic jet and the surrounding medium)

Discarded from PeVatron sources catalogue

Inefficient acceleration in the jets if VHE emitter is located further than 1x10¹ cm from the compact object⁰


EXTRAGALACTICEXTRAGALACTIC

SOURCESOURCE REDSHIFTREDSHIFT MAGICMAGIC H.E.S.S.H.E.S.S. VERITASVERITAS

3C 279 0.536 2006 - -

PKS1510 0.361 2012 2009 -

PKS1222+216 0.432 2010 - -

B0218+357 0.954 2014 - -

PKS1441+25 0.939 2015 - 2015

S4 0954+65 unknown 2015 - -

PKS0736+017 0.189 - 2016 -

TON 0599 0.725 2017 - -

Flat Spectrum Radio QuasarsFlat Spectrum Radio Quasars

EB

LL

EN

SL

AT

ES

T

DE

TE

CT

I ON


EXTRAGALACTICEXTRAGALACTICBACKGROUND LIGHTBACKGROUND LIGHT

MAGIC only

MAGIC +FermiLAT


EXTRAGALACTICEXTRAGALACTIC

SOURCESOURCE SEASONSSEASONS

1ES 1741+196 2017

NGC 1275 2016-2017

IC 310

Mrk421 Multi-year

Mrk501 Multi-year

BL Lac, Radio Galaxy, BL Lac, Radio Galaxy, AGNAGN

Multi-wavelength (Swift-UVOT, Swift-XRT,NuSTAR, Fermi-LAT, MAGIC, and VERITAS) and multi-year

Low-luminosity blazar

Radio-galaxy:- detected a very rapid flare (<15min)J. Aleksic et al. Black hole lightning due to particle acceleration at subhorizon scales. Science, 346:1080–1084, Nov. 2014.

- first MAGIC multi-wavelength campaign


IC 310 – MULTI-WAVELENGTHIC 310 – MULTI-WAVELENGTH


MULTIMESSENGER:MULTIMESSENGER:VHE NEUTRINOsVHE NEUTRINOs

● Not deflected by magnetic fields (like γ)

● Clear indicators of VHE/UHE cosmic ray production

● Until recently, detected by IceCube as only diffuse flux

● MAGIC is part of the Gamma-Ray Follow-up program since 2012

(see JINST, 11, P11009 (2016))● more than 30 hours

invested during previous cycle (2017)


VHE NEUTRINOs:VHE NEUTRINOs:ICECUBE EVENT ALERTICECUBE EVENT ALERT

➔ First time detection of a VHE γ-ray source directionally coincident with a HE neutrino (IC-170922A/TXS0506+056)!

STAY TUNED!STAY TUNED!


MULTIMESSENGER:MULTIMESSENGER:GRAVITATIONAL WAVESGRAVITATIONAL WAVES

Cre

dits

: M

.Pe

resa

no

● MoU among MAGIC and LIGO/VIRGO since 2014 to look for gravitational waves (GW)

→ prepared to receive more alerts● Planned to use GRBs mode

(movement of 180° in < 30s) for the GWs follow up starting from February 2019 (O3), together with the follow up of the possible EM counterpart

● MAGIC: the first IACT to follow-up a GW alert (GW151226), no detection

● GW 170817 (NS-NS event) not promptly observed by MAGIC telescopes

→ Southern hemisphere!


FUNDAMENTAL PHYSICSFUNDAMENTAL PHYSICS


LORENTZ INVARIANCE LORENTZ INVARIANCE VIOLATIONVIOLATION

Lorentz invariance violation

energy dependent dispersion of photons in vacuum

Whilst a very small effect on local scales the effect will be cumulative, and so for very high energy particles that travel very large distances the difference

in arrival times could become sufficiently large to be detectable


LORENTZ INVARIANCE VIOLATION LORENTZ INVARIANCE VIOLATION OBSERVABLE SOURCESOBSERVABLE SOURCES

Now 10⁴

- MAGIC constraints on LIV using:

- LIV Consortium created by H.E.S.S., MAGIC and VERITAS collaborations

AGNs

pulsars


LORENTZ INVARIANCE LORENTZ INVARIANCE VIOLATIONVIOLATION

- MAGIC results using likelihood method

MAGIC Collaboration, M. L. Ahnen et al., Constraining Lorentz Invariance Violation Using the Crab Pulsar Emission Observed up to TeV Energies by MAGIC. Astrophys. J. Suppl. Ser., 232(1), September 2017.

Crab pulsar(MAGIC)

Crab pulsar(MAGIC)


DARK MATTER – INDIRECT DARK MATTER – INDIRECT SEARCHESSEARCHES

ANNIHILATION / DECAY


DARK MATTER – GAMMA-RAY DARK MATTER – GAMMA-RAY FLUXFLUX

→ from the theoretical point of view:


DARK MATTER - SOURCES DARK MATTER - SOURCES

→ Main goal: high J-factor!


SEGUE - ANNIHILATIONSEGUE - ANNIHILATION

Cre

dits

: M

.Do

ro -

CR

IS2

01

8


log10

(J(θmax

)

[GeV²cm ]):⁻⁵

19.42Distance:

~30kpc

UMA II - ANNIHILATIONUMA II - ANNIHILATION

+0.44

- 0.42


PERSEUS - DECAYPERSEUS - DECAY

Constraining Dark Matter lifetime with a deep gamma-ray survey of the Perseus Galaxy Cluster with MAGICMAGIC and Finnish Centre of Astronomy with ESO Collaborations and INFN Consortium, Rome, Italy and Finnish MAGIC Consortium: Tuorla Observatory (V.A. Acciari et al.). Jun 28, 2018. 17 pp.arXiv:1806.11063

Constraining Dark Matter lifetime with a deep gamma-ray survey of the Perseus Galaxy Cluster with MAGICMAGIC and Finnish Centre of Astronomy with ESO Collaborations and INFN Consortium, Rome, Italy and Finnish MAGIC Consortium: Tuorla Observatory (V.A. Acciari et al.). Jun 28, 2018. 17 pp.arXiv:1806.11063

J(θmax

[GeV·cm ²]):⁻

1.5x10¹⁹Distance:

77.7Mpc

NEW!

NEW!


CONCLUSIONSCONCLUSIONS

● MAGIC → Possibility to work in different Physics fields● After 15 years, still very active collaboration (at least two new

member groups in the past year)● Articles published every month● Still space for improvement from the instrumental point of view● Wide variety of sources observed and more to observe● Accumulating time of observation to have more statistics

Let’s join MAGIC!


● The MAGIC collaboration opens a fraction of the observing program to external scientists

● Further details can be found here:

https://magic.mpp.mpg.de/outsiders/magicop/

● The next observing cycle spans from January 2019 to February 2020

NEWS!NEWS!

Thanks!Thanks!

MAGIC: from Astrophysics to Fundamental Physics ...

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