First 1ES1959+650 observations

with the MAGIC telescopeand comparison with Crab Nebula at 40 ZA

First 1ES1959+650 observations

with the MAGIC telescopeand comparison with Crab Nebula at 40 ZA

IntroductionData analyzedAnalysis methodPreliminary results

IntroductionData analyzedAnalysis methodPreliminary results

Nadia Tonello, Max-Planck-Insitut für Physik, MünchenNadia Tonello, Max-Planck-Insitut für Physik, München

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Nadia Tonello, MPI MunichNadia Tonello, MPI Munich 22

What is 1ES1959+650?

1998: First detection: Utah Seven Telescope Array

Weak sourceConfirmed in 2002 by WHIPPLE and HEGRA

Most interesting aspect: orphan flare in June 2002. Candidate source for south neutrino telescopes

Elliptical galaxyElliptical galaxy Active Galactic NucleusActive Galactic Nucleus z = 0.047z = 0.047 RA =19h59m59.8sRA =19h59m59.8s Dec = +65Dec = +6508'54''08'54''

Observability from La Palma:Observability from La Palma: May-October 35May-October 35-54-54 z.a. z.a.

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The MAGIC Telescope

Canary Island La Palma2200 m asl

Largest ImagingAir CherenkovTelescope for -ray astronomy

17 m mirror dish3.5 field of view576 high-QE PMTs

Design optimized for: low energy thresholdE = 30 GeV

fast repositioning tR<30 sec

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Imaging Air Cherenkov Telescopes

~ 10 kmParticleshower

~ 1o

Ch

eren

kov

ligh

t

~ 120 m

Gammaray Cherenkov light Image of

particle shower in telescope camera

reconstruct: arrival direction, energyreject hadron background

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Standard Analysis

hadron shower (background)

gamma shower

raw image cleaned image

Shower reconstructionand background rejection based on image shapeanalysis

Hillas parameters:Length, width, distance,alpha

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MAGIC raw dataSource Days Obs. Time ZA range Azimuth

1ES1959+650

September 06, 07October 07, 10,14,15,16,17

6 h 55 m4.4 M events

min = 35max = 47

min = -26max = 2

Crab Nebula

September13, 14, 15, 16,21,22,23

2 h 17 m1.7 M events

min = 35max = 46(selected)

min= 85max = 94

Off data September 8, 10, 11, 12, 13, 14, 16, 17

2 h 49 m2.3 M events

min = 35max = 46(selected)

min= 85max = 94

Cuts optimized on Crab Nebula and applied to 1ES1959 and Off dataCuts optimized on Crab Nebula and applied to 1ES1959 and Off data

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Signal above 2000 ph.

1ES 1959 + 650: Size >2000 phSignificance: 7.0 Excess events: 165

Crab Nebula: Size >2000 phSignificance: 26.4 Excess events: 529 ± 20

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Time analysis

Binning in about 2 h dataNo substantial variation of activity

Days Obs time Significance Excess Rate(phot/min)

September6,7

121 min 3.6 42.8 ± 11.8 0.35 ± 0.09

October 7,10,15

110 min 4.0 49.5 ± 12.3 0.45 ±0.11

October 16, 17

137 min 5.0 64.0 ± 12.8 0.46 ± 0.09

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X-ray light curve

Activity not particularly high

5 - 7 Sept

7 -17 Oct

RXTE mission day

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Optical light curve

Tuorla Observatory Blazar Monitoring Program

Quiescent state

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Crab-1ES1959 comparison

Same cuts applied to Crab and 1ES1959 for each size binSame cuts applied to Crab and 1ES1959 for each size bin

Size (ph) Significance Excess events

1000<S<2000 10.2 296 ± 29

2000<S<4000 18 258 ± 14

4000<S<8000 17.3 166 ± 10

8000<S<16000 4.8 71 ± 15

1000<S<2000 5.0 364 ± 73

2000<S<4000 4.9 87 ± 20

4000<S<8000 4.2 42 ± 10

8000<S<16000 1.5 29 ± 19

CR

AB

1ES

1959

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Crab-1ES1959 comparison

Excess events/(obs. time * size bin width)

43%

12%

9%

14%

Softer spectrum?

HEGRA System Results (2000-2001):94 h obs. Time.Energy threshold: 2TeVSignificance 5.4= 3.3 ±0.78% Crab flux

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1ES1959 has been observed with MAGIC for ~7 h. Crab and OFF data (~ 2h each) have been selected to match ZA range: 40 deg.

Data have been analyzed with cuts optimized on Crab.

We have a signal from 1ES1959+650 when We have a signal from 1ES1959+650 when there was no high activity in X-raysthere was no high activity in X-rays

No variation of state, observations are fragmented in time.

Comparison with Crab in size bins:

1ES1959 ~40% to ~10% of Crab, compatible with HEGRA System flux measurements at high energies.

Work in progress: Energy spectrum.

Conclusions