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MAGIC. Recent AGN Observations. The MAGIC Telescopes. Located at La Palma, altitude 2 200m First telescope in operation since 2004 Stereoscopic system in operation since 2009 moonlight and twilight observations. Single Telescope. Stereo System. MAGIC stereoscopic system.

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Recent AGN Observations

The magic telescopes
The MAGIC Telescopes

  • Located at La Palma, altitude 2 200m

  • First telescope in operation since 2004

  • Stereoscopic system in operation since 2009

  • moonlight

  • and twilight observations

Magic stereoscopic system
MAGIC stereoscopic system

  • Low energy threshold 50 GeV (25 GeV with sumtrigger): allows observations of distant universe and overlap with Fermi

  • FoV 3.5 degrees

  • Sensitivity 0.8% Crab in 50h (>250 GeV)

  • Angular resolution 0.07 degrees (>300GeV)

  • Energy resolution ~16% (E>300GeV)

Kva telescope
KVA Telescope

  • Tuorla is using remotely our KVA telescope which is located physically on La Palma, very close to MAGIC

Flat spectrum radio quasar 3c279
Flat-spectrum radio quasar 3C279

  • Most distant VHE gamma-ray emitter with z=0.536, discovered by MAGIC in 2006 (Albert et al. 2008, Science)

  • Re-observed in 2007 and 2009 (with MAGIC-I only), no new limits on EBL (the EBL modeling has improved greatly in past two-three years, it is not so much free parameter anymore), but interesting results for blazar physics.

  • Aleksić et al. 2011 A&A accepted [arXiv1101.2522]

3c 279 magic observations 2007 and 2009
3C 279 MAGIC observations 2007 and 2009

  • In January 2007 triggered by optical outburst

Tuorla blazar monitoring lightcurves available @

3c279 magic observations 2007 and 2009
3C279 MAGIC Observations 2007 and 2009

MAGIC observations

  • December 2008- April 2009 MAGIC observations: rather unfortunate timing

  • Resulted in non-detection, differential upperlimits:

Optically triggered discoveries
Optically triggered discoveries

  • In the past: Mrk180, 1ES1011+496, S50716+714; only for S50716+714 it was possible to show that during the optical outburst the VHE gamma-ray flux was higher than in previous MAGIC observations at low optical state.

  • Also 3C279 observations were triggered by high optical state, also some not-optically triggered discoveries have taken place in optical high state.

  • New ones: B3 2247+381 in October 2010 and ON 325 in January 2011

Bl lac object b3 2247 381
BL Lac object B3 2247+381

  • candidate BL Lac object at z=0.119

  • X-ray bright HBL=> good candidate for TeV emission

  • Added to Tuorla optical blazar monitoring program in 2006, first 4 years showed hardly any variability

  • Hard spectra in Fermi range: candidate TeV source

  • Optical outburst in autumn 2010, trigger to MAGIC in the end of September 2010

  • Swift ToO observations

Optically triggered discovery of vhe gamma ray emission from b3 2247 381
Optically triggered discovery of VHE gamma-ray emission from B3 2247+381

  • 9.3 hours of MAGIC observations resulted in the discovery of VHE gamma-ray emission from the source with 5 sigma

  • In total ~20 hours were collected

  • Flux ~2%Crab (below previous upper limit)

  • Paper in preparation

On325 1es1215 303
ON325 = 1ES1215+303 B3 2247+381

  • HBL at z=0.130 (or 0.237)

  • TeV blazar candidate from Costamante&Ghisellini (2002), appeared also in Fermi candidate list in 2010

  • Monitored in optical since 2003: has shown many fast optical flares

  • Has been previously observed with MAGIC (several times)

  • In high optical state in January 2011, triggered MAGIC and Swift observatons

Optically triggered discovery of vhe gamma ray emission from on 325
Optically triggered discovery of VHE gamma-ray emission from ON 325

  • MAGIC ToO observations started on January 2nd 2011

  • 5.5 hours of MAGIC observations resulted in ~5sigma detection: ATel #3100

  • In total >20 hours were collected

  • Paper in preparation

Hbl 1es 0806 524
HBL 1ES 0806+524 ON 325

  • HBL at z=0.138

  • Candidate TeV blazar from the Costamante&Ghisellini list, detected by VERITAS in 2006-2008 with flux ~1.8%Crab, “little or no measurable variability” was found

  • Source was showing very prominent and very bright flare in the optical bands since October 2010

  • The MAGIC observations were finally accepted in February 2011

Optically triggered observation of 1es 0806 524
Optically triggered observation of 1ES 0806+524 ON 325

  • MAGIC observation on 24th of February (3.3hours) resulted in detection with >6sigma, preliminary analysis gives flux estimation of ~5.6% Crab

  • Observations on 23rd of February resulted in non-detection=> day scale variability

  • Analysis of the whole dataset (~20h) is ongoing

  • Also Swift observations were triggered, high X-ray state (ATel#3208)

Do optical triggers work
Do optical triggers work? ON 325

  • Yes, they do... at least most of the time and for most of the objects (many HBLs, some LBLs and 3C279)

  • But it is difficult to prove

  • And in best studied sources (like Mrk421 and PKS2155-304) the activity in these two energy regimes seems to be connected only “occasionally”.

Not optically triggered discovery magic j 2001 435
Not optically triggered discovery: MAGIC J 2001+435 ON 325

  • Was observed because was identified as one of the best candidates for VHE gamma-ray emission from the list of candidate sources

  • Is identified with MG4 J200112+4352, HBL at unknown redshift

  • Detected on one night only 16th July 2010

  • Announced with astronomers telegram #2753, paper in preparation

Best studied northern tev sources mrk421 mrk501 and m87
Best studied northern TeV sources: ON 325 Mrk421, Mrk501 and M87

  • Two near-by TeV blazars Mrk421 and Mrk501 (z=0.03), high energy peaking BL Lacs

  • The brightest TeV sources so obvious candidates for any deep study involving VHE gamma-ray energies

  • Long term monitoring with MAGIC and extensive MWL campaigns in Fermi era.

  • M87, the nearby radio galaxy

  • Long-term collaboration between MAGIC-HESS-VERITAS to monitor the source in VHE gamma-rays in coordination with other instruments from different wavebands (VLBA, X-rays)

Long term monitoring
Long-term monitoring ON 325

  • To study: un-biased statistics of different flux levels, spectral properties in different flux states, correlations with other wavelengths and determination of flare probabilities

  • Trigger ToOs (self-triggers, other IACTs, other wavelengths)

  • Sources to be monitored need to be bright: MAGIC has been regularly monitoring Mrk421, Mrk501 and 1ES1959+650 since 2006 (but observations since 2004)

Results for mrk421
Results for Mrk421 ON 325

  • The lightcurve has 119 daily averaged flux data points

  • Variable in short and long timescales

  • Clear correlation with X-rays

Hsu et al. 2009, ICRC, Lodz

The extensive mwls
The extensive MWLs ON 325

  • Despite the decades of study the spectral energy distributions were still rather poorly characterized

  • With Fermi on-board it is finally possible to study the full SED from radio to VHE gamma-rays

  • Extensive coordinated MWLs since 2009

Extensive mwl on m87 in 2008
Extensive MWL on M87 in 2008 ON 325

  • MAGIC-HESS-VERITAS joint effort

  • Coverage 120h / 50nights

  • HST-1 very unlikely source of the emission

Summary and outlook
Summary and outlook ON 325

  • The VHE gamma-ray emission from flat-spectrum radio quasars: fast variability (in time scale of days for 3C279 and in time-scale of ~10 minutes for PKS1222+216)

  • Optical triggers work well, although connection between optical to VHE gamma-ray high states is not proved yet.

  • Improved sensitivity has allowed new discoveries of sources: important for population studies

  • Extensive MWLs provide important insights into AGN jets

  • MAGIC stereoscopic system is performing well and we expect many more interesting results to come!