Study of Cosmic Electrons and Positrons with MAGIC

Study of cosmic electrons and positrons with MAGIC

Kathrin Mallot 1 Introduction Motivation

2 MAGIC The Experiment The e± spectrum with MAGIC

3 Future work Working on Data Working on Simulations

4 Outlook

Kathrin Mallot 2/18 e−-spectrum with MAGIC Introduction Motivation Cosmic Rays

Energies and rates of the cosmic-ray particles

CAPRICE AMS 100 protons only BESS98 Ryan et al. Grigorov • covers almost 12 orders of JACEE Akeno magnitude in energy all-particle Tien Shan -2 MSU ) 10 electrons KASCADE -1

15 s CASA-BLANCA • knee at ≈ 3 × 10 eV -1 DICE

sr HEGRA

-2 positrons CasaMia 18 Tibet • ankle at ≈ 3 × 10 eV 10-4 Fly Eye Haverah Yakutsk AGASA • composition: HiRes 98% nuclei and 2% electrons 10-6 antiprotons dN/dE (GeV cm 2 • nuclei composed of: E 87% protons, 12% helium 10-8 nuclei and heavier nuclei.

10-10 100 102 104 106 108 1010 1012 Ekin (GeV / particle) Kathrin Mallot 3/18 e−-spectrum with MAGIC Introduction Motivation The case of the electrons

• spans only 3 orders of magnitude • high energetic ﬂux bigger than predicted • ATIC-bump • HESS data may indicate further rise in ﬂux at TeV range

Kathrin Mallot 4/18 e−-spectrum with MAGIC MAGIC The Experiment

MAGIC

Kathrin Mallot 5/18 e−-spectrum with MAGIC MAGIC The Experiment The Telescopes

Situated at 2200 m.a.s.l. in Roque de los Muchachos Observatory, La Palma

• 2 IACT with 17m diameter dishes • Energy range: 50 GeV to 50TeV • very fast positioning • high sensitivity

Kathrin Mallot 6/18 e−-spectrum with MAGIC MAGIC The Experiment IACT: Imaging Atmospheric Cherenkov Telescope

Kathrin Mallot 7/18 e−-spectrum with MAGIC MAGIC The e± spectrum with MAGIC Measuring diﬀuse ﬂux

Problems: • Standard analysis does not work • No direction based cuts • No background measurements possible

New analysis developed: • based on “hadronness” of event • MC used for background simulation • Work done at MAGIC shows comparable, but not as good, results on point sources. • Only working analysis for diﬀuse ﬂux

Kathrin Mallot 8/18 e−-spectrum with MAGIC MAGIC The e± spectrum with MAGIC What is hadronness

• Hadronness is the likelihood for an event to be hadronic. • Based on the length and width of the light cone hitting the telescope • Assigned by random forest trained with MC electrons and protons

Kathrin Mallot 9/18 e−-spectrum with MAGIC MAGIC The e± spectrum with MAGIC Current results

Electron positron flux ] 2 GeV -1 sr -1 s -2

102 )/dE [m + HEAT +e - Emulsion chambers AMS-01

d(e PPB-BETS ×

3 H.E.S.S. low energy

E H.E.S.S. high energy ATIC Fermi-LAT low energy 10 Fermi-LAT high energy Pamela e- PRELIMINARY MAGIC

10 102 103 Energy [GeV]

Kathrin Mallot 10/18 e−-spectrum with MAGIC Future work Working on Data Data Analysis in the MAGIC collaboration

Things that need to be done:

• Cross check the current electron spectrum • Expand the current electron spectrum to higher energies if possible • Improve statistics of the data • Improve statistics of the MC used as background • Study the uncertainties in the analysis. • Reﬁne the analysis

Things I have already worked on or started to work on:

• Cross check the current electron spectrum • Expand the current electron spectrum to higher energies if possible • Improve statistics of the MC used as background

Kathrin Mallot 11/18 e−-spectrum with MAGIC Future work Working on Simulations Theoretical interpretations

• Still vague, only a general idea • Work on SUSY DM theories • identify remaining parameter space for MSSM compatible with measurements of • combined electron and positron spectrum • electron/positron ratio • and proton/antiproton ratio. • Crossreference with MSSM parameter space still allowed by LHC • identify two or more such models and compute the electron spectrum in the TeV range

Kathrin Mallot 12/18 e−-spectrum with MAGIC Future work Working on Simulations Predictions for MAGIC

Will try to answer these questions:

• How far can MAGIC extend the spectrum in best case? • Can MAGIC differentiate between the models considered? • What would be the improvement needed on statistical and systematic errors to see the difference? • How much observation time would be needed by MAGIC to differentiate between the models?

Kathrin Mallot 13/18 e−-spectrum with MAGIC Outlook CTA

A look at the next generation: CTA

Kathrin Mallot 14/18 e−-spectrum with MAGIC Outlook CTA What is CTA

• Next Generation of IACT • Array composed of several diﬀerent sized telescopes • Energy range from 100GeV to 100 TeV • Bigger ﬁeld of view • Operational in 2018

Kathrin Mallot 15/18 e−-spectrum with MAGIC Outlook CTA Work to be done in the CTA group

• Create MC electron data for CTA. • Study sensitivity for electrons of the diﬀerent CTA layouts. • Study goodness of separation of electrons from γ and protons in CTA. • Predict observation time needed to create an electron spectrum comparable to MAGIC’s. • Evaluate Energy range for CTA’s electron spectrum. • Predict whether or not CTA will be able to distinguish between the diﬀerent theoretic models studied.

Kathrin Mallot 16/18 e−-spectrum with MAGIC The End Outlook

• Cosmic electrons are a very active ﬁeld in Astrophysics.

• Many experiments are expected to publish (further) results in this area in the next few years: FERMI, AMS-02, MAGIC...

• Origin of the electron surplus unknown

• notable discrepancies between DM-theory and astrophysical-theory are expected just beyond the currently measured energy range.

• CTA is expected to further expand energy range when operational.

Kathrin Mallot 17/18 e−-spectrum with MAGIC The End Conclusion

• Working on measuring the e±-spectrum. • e±-spectrum “anomaly” could be sign of Dark Matter. • Future work will include theoretical and experimental work. • Interesting results from MAGIC and other experiments expected within the next 2-3 years.

THE END

Kathrin Mallot 18/18 e−-spectrum with MAGIC