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Markarian 421 with MAGIC telescope. Daniel Mazin for the MAGIC Collaboration Max-Planck-Institut f ür Physik , M ünchen [email protected] 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

[email protected]

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

+ X-calibration of the instruments

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
ad