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Markarian 421 with MAGIC telescope. Daniel Mazin for the MAGIC Collaboration Max-Planck-Institut f ür Physik , M ünchen mazin@mppmu.mpg.de. Outline. The MAGIC telescope AGN Markarian 421 Data sample Analysis status Conclusion / outlook. The MAGIC Telescope.

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Markarian 421 with magic telescope

Markarian 421 with MAGIC telescope

Daniel Mazin for the MAGIC Collaboration

Max-Planck-Institut für Physik, München

mazin@mppmu.mpg.de


Outline
Outline

  • The MAGIC telescope

  • AGN Markarian 421

  • Data sample

  • Analysis status

  • Conclusion / outlook


The magic telescope
The MAGIC Telescope

  • The largest imaging atmospheric Cherenkov Telescope with 236 m2 mirror surface

  • 3.5° FoV Camera with 576 high-QE PMT’s

  • Design optimized for:

    • Low energy threshold

      E = 30 GeV

    • Fast repositioning

      tp < 30 sec

Canarian Island La Palma,

2200 m asl


Agn markarian 421

Aimo Sillanpaa, NOT

AGN Markarian 421

  • Right Ascension11:04:27 (h:m:s)

    Declination: +38:12:32 (deg:m:s)

  • BL Lac object, z=0.030 (370 MLy)

  • Mass: 1.9 •108 M

  • First detected extragalactic TeV -ray source (Punch et al, 1992)

  • Many known flares, active in 2004

  • Well described by SSC models (e.g. Konopelko et al, ApJ,597:851)

  • Still many correlations not understood


Advantages of simultaneous observations

HEGRA, A&A,410,813

Advantages of simultaneous observations

  • One experiment: one decade in energy

  • Two experiments: two decades

  • Multiwavelength campaigns

  • Correlation studies

  • Change hardness during flares (Krennrich et al, ICRC 2003)

  • Light curves, look for fast flares

HEGRA, A&A,393,89



Magic data sample december 04
MAGIC data sample (December 04)

  • Triggered by RXTE and VERITAS (Dec 14)

  • After a few hours: MAGIC and HESS agreed to make simultaneous observations

  • Due to bad weather only 2 days of MAGIC data: 18 and 19 December


Comparison of mc predictions and data
Comparison of MC predictions and data

Good agreement between mc-gamma and excess events


Estimate of energy resolution

Log10(Etrue[GeV])

Log10(Eest[GeV])

Sigma[%]

(Eest-Etrue)/Etrue

Log10(Eest[GeV])

Estimate of energy resolution

  • SIZE (total number of PEs) simplest energy estimator

  • improve energy estimation including other image parameters

  • optimized estimator using Random Forest technique

  • 20% (30%) @ 1 TeV (100 GeV)


Mrk 421 false source plot

Number of excess events

39.19

Dec (deg)

38.69

38.19

Preliminary

37.69

Preliminary

11.14

11.10

11.07

11.04

11.00

RA (h)

Mrk 421: False source plot

  • For the whole data sample (3.7h):

    • After cuts: over 700 excess events

    • Point-like source ( < 0.15 deg )


Alpha plots
Alpha plots

18/12/05, <Zd>=48

18/12/05, <Zd>=12

  • For the 4 samples:

Clear signal

detection in all

of them

  • Energy range for this analysis:

    high zenith angle:

    250 GeV – 2 TeV

    low zenith angle:

    100 GeV – 1 TeV

19/12/05, <Zd>=51

19/12/05, <Zd>=21


Light curve x ray
Light curve (X-ray)

17-20 December 2004

18/12

19/12

  • X-rays: no significant variation

  • Optical data (KVA): quiescent state

Dec 04

Apr 04


Light curve gev magic
Light curve (GeV, MAGIC)

  • Low zenith angle points only, 20 min bins

  • No strong variations visible

  • Looks like we just missed the peak of the flare (weather!)

4004

4005

(mjd-49353)

  • Soon to come:

    • Energy spectrum and full light curve for the MAGIC data

    • Combined MAGIC – HESS data analysis


Conclusions outlook
Conclusions / Outlook

  • MAGIC clearly detected a flare of Markarian 421 in December 2004

  • Due to bad weather: too late for the peak of the flare

  • 3.7 hours of data: enough statistics to produce light curves and energy spectra  work in progress

  • Coordinated ground based Cherenkov telescopes observations going on

  • Almost full time coverage possible (CANGAROO, HESS, VERITAS, MAGIC)

  • Up to 3 decades in energy due to energy threshold and different zenith angle conditions



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