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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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magic

MAGIC

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 @ http://users.utu.fi/kani/1m

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
  • 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
  • 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
  • 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?
  • 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
  • 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: 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
  • 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
  • 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
  • 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
  • MAGIC-HESS-VERITAS joint effort
  • Coverage 120h / 50nights
  • HST-1 very unlikely source of the emission
summary and outlook
Summary and outlook
  • 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!
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