Determining the TeV Gamma-Ray Emission Region in the Relativistic Jet of M87 using TeV and Radio Monitoring
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1 Determining the TeV Gamma-Ray Emission Region in the Relativistic Jet of M87 using TeV and Radio Monitoring R. M. Wagner Max-Planck-Institut für Physik, München and Excellence Cluster Origin and Structure of the Universe, Garching on behalf of the MAGIC, VERITAS, and H.E.S.S. Collaborations and the M87 43-GHz Monitoring Team
2 The Extragalactic TeV Sky Extragalactic VHE -ray sources (E >100 GeV) o M Mkn BL Lac Mkn NGC IC C 66A Mkn rwagner/sources/ 44 sources, mostly blazars Relativistically beamed gamma-ray emission Excepted by M87 (1999), Cen A (2008), M82, NGC 253 (2009), IC310, NGC 1275 (2010) o +90 W Comae NGC 253 o M AP Lib C 279 Cen A o Redshift z 2
3 The Giant Elliptical Radio Galaxy M87 Owen+00 (' 15 ) 80 kpc ( VLA Radio (90cm, Close-by radio galaxy: ( z= ) ~16.7 Mpc Radio structure: outflows and halo Jet angle: ~30 not a blazar! But inner region < 19 Central black hole very massive: M BH ~ M Gebhardt+Thomas09 Giant outer lobes, 0.2 x 0.2 deg relativistic particle population: Apparent superluminal motion in jet High radio polarization brightness temperature Unique laboratory to study blazar and jet physics 3
4 The Relativistic Plasma Jet of M87 Highly structured jet: knots resolved in radio, optical and X-rays Jet is variable: flares in radio, optical and X-rays ( VLA ) radio X-ray/optical/radio knots: concentrated structures... shocks? Radio/optical: similar polarization synchrotron emission X-ray: spectrum with α= synchrotron emission? ( HST ) optical ~2 kpc Inner jet: superluminal motion (~2c) => relativistic particle population Variability time-scales: weeks to months to years ( Chandra ) X-ray Wilson&Young02 4
5 The Relativistic Plasma Jet of M87 Highly structured jet: knots resolved in radio, optical and X-rays Jet is variable: flares in radio, optical and X-rays ( VLA ) radio X-ray/optical/radio knots: concentrated structures... shocks? Radio/optical: similar polarization synchrotron emission X-ray: spectrum with α= synchrotron emission? ( HST ) optical ~2 kpc Inner jet: superluminal motion (~2c) => relativistic particle population Variability time-scales: weeks to months to years ( Chandra ) X-ray Predictions of VHE γ-ray and UHECR particle emission 4 Wilson&Young02
6 The Relativistic Plasma Jet of M87 Highly structured jet: knots resolved in radio, optical and X-rays Jet is variable: flares in radio, optical and X-rays ( VLA ) radio X-ray/optical/radio knots: concentrated structures... shocks? Radio/optical: similar polarization synchrotron emission X-ray: spectrum with α= synchrotron emission? ( HST ) optical ~2 kpc Inner jet: superluminal motion (~2c) => relativistic particle population Harris+09 Variability time-scales: weeks to months to years ( Chandra ) X-ray Predictions of VHE γ-ray and UHECR particle emission 4 Wilson&Young02
7 M87 at Very High Energies >4σ excess seen by HEGRA in σ detection by H.E.S.S 2003/4, Aharonian+06 5
8 M87 at Very High Energies >4σ excess seen by HEGRA in σ detection by H.E.S.S 2003/4, Signal confirmed by MAGIC and VERITAS Day-scale flares 2005 H.E.S.S., 2008 MAGIC Aharonian+06 5
9 M87 at Very High Energies >4σ excess seen by HEGRA in σ detection by H.E.S.S 2003/4, Signal confirmed by MAGIC and VERITAS Day-scale flares 2005 H.E.S.S., 2008 MAGIC Variations on timescales of months Aharonian+06 5
10 M87 at Very High Energies >4σ excess seen by HEGRA in σ detection by H.E.S.S 2003/4, Signal confirmed by MAGIC and VERITAS Day-scale flares 2005 H.E.S.S., 2008 MAGIC Variations on timescales of months Detected by Fermi 08/09 Aharonian+06 5
11 M87 at Very High Energies >4σ excess seen by HEGRA in σ detection by H.E.S.S 2003/4, Signal confirmed by MAGIC and VERITAS Day-scale flares 2005 H.E.S.S., 2008 MAGIC Variations on timescales of months Detected by Fermi 08/09 Energy spectrum stable hard: α= GeV to 20 TeV Aharonian+06 5
12 The Origin of the VHE Emission? Possible mechanism/ sites for VHE emission Dark matter annihilation Cosmic Rays in M 87 Intra-cluster gas Large-scale jets Inner/Outer-jet (Hadronic/Leptonic) Knots? HST1? Vicinity of black hole... ( VLA ) radio ( HST ) optical ~2 kpc ( Chandra ) X-ray Wilson&Young02 6
13 The Origin of the VHE Emission? Possible mechanism/ sites for VHE emission Dark matter annihilation Cosmic Rays in M 87 Intra-cluster gas Large-scale jets Inner/Outer-jet (Hadronic/Leptonic) Knots? HST1? Vicinity of black hole... ( VLA ) radio ( HST ) optical ~2 kpc Further observations to: ( Chandra ) X-ray confirm short-term VHE variability determine location of VHE emission 6 Wilson&Young02
14 The 2008 Campaign: VHE Instruments VERITAS MAGIC HESS H.E.S.S., MAGIC, & VERITAS collected >120 h of data from Jan to Jul
15 The Imaging Air Cherenkov Technique Extended Air Shower initiated in atmosphere Detect the Cherenkov radiation from charged particles in EAS A mirror reflects and concentrates the light An image of the shower formed in a photomultiplier camera km Cherenkov light cone ~ 1 o 120 m
16 The Imaging Air Cherenkov Technique Extended Air Shower initiated in atmosphere Detect the Cherenkov radiation from charged particles in EAS A mirror reflects and concentrates the light An image of the shower formed in a photomultiplier camera Gamma event Hadron event km Cherenkov light cone 120 m ~ 1 o Hadrons (background) dominate over gammas (signal). They must be rejected statistically in the analysis
17 The 2008 Campaign: Further Instruments VLBA observations at 43 GHz Walker+09 Resolution: 0.21x0.43 mas (30x60 Rs) Scale: <pc direct vicinity of the BH Movie project: 13 obs. in 2007, every three weeks; 14 obs. in 2008, every 5 days Chandra observations in X-rays since 2002 Harris+07, 08, 09 Scale: kpc inner jet Every 6 weeks 9
18 The 2008 Joint VHE Campaign Coordinated observations: VERITAS/MAGIC/H.E.S.S. plus 5 Chandra pointings in 2008 Coverage: 120h, 50 nights Outburst in February 2008 (2 weeks after a MAGIC trigger, ( HST-1 X-ray low-state of Confirmed short-term variability ( Chandra ) X-ray Core HST-1 Knot A HST-1 very low Science 325 (2009) 444 Core flux peaks all-time high HST-1: unlikely source of VHE emission 10
19 VHE/Radio Collaboration Reveals... VLBA Monitoring of the M87 jet at 43 GHz,( 2007/8 ) Walker et al. mas Resolution: 0.43x Schwarzschild radii ( pc = 0.37 mas (1 mas = Science 325 (2009) 444 VHE Gamma-Rays X-Rays Radio Jet 30 x 60 R S VHE flare accompanied by radio flare from BH vincinity 11
20 VHE/Radio Collaboration Reveals... VLBA Monitoring of the M87 jet at 43 GHz,( 2007/8 ) Walker et al. mas Resolution: 0.43x Schwarzschild radii ( pc = 0.37 mas (1 mas = Science 325 (2009) 444 VHE Gamma-Rays X-Rays Radio R.C. Walker et al. Jet 30 x 60 R S VHE flare accompanied by radio flare from BH vincinity 11
21 VHE/Radio Collaboration Reveals... Science 325 (2009)
22 VHE/Radio Collaboration Reveals... Science 325 (2009)
23 VHE/Radio Collaboration Reveals... Science 325 (2009) 444 Science 325 (2009) 444 SOM Time-dependent electron injection into slow outer sheath ~VHE flux 12
24 M87 in VHE γ-rays: What did we learn? First non-blazar emitting VHE γ-rays: Misaligned blazar, AGN unification? TeV alone: Upper limit on VHE extension 14 kpc location unknown TeV alone: Short-term variability: Excludes models Constrains size of emitting region (R < 5x10 15 δ cm, ~100 R schw ) TeV alone: Hard energy spectra: modeling, emission mechanism Radio/TeV connection: Strong indication First experimental evidence: charged particles accelerated in BH vicinity 13
25 M87 in VHE γ-rays: What did we learn? First non-blazar emitting VHE γ-rays: Misaligned blazar, AGN unification? TeV alone: Upper limit on VHE extension 14 kpc location unknown TeV alone: Short-term variability: Excludes models Constrains size of emitting region (R < 5x10 15 δ cm, ~100 R schw ) TeV alone: Hard energy spectra: modeling, emission mechanism Radio/TeV connection: Strong indication First experimental evidence: charged particles accelerated in BH vicinity Key question: origin/(location) of the TeV emission 13
26 M87 (non-simultaneous) SED Decelerated inner jet, Geoganopolous+05 Published before HESS 2005 flare x Does not describe hard TeV spectra well x Strong cutoff, but tunable? Hadronic: Synchrotron Proton Blazar Reimer+04 fit based on HEGRA detection x Fermi Range: Rather different slopes x Intrinsic cutoff at few TeV s -1 ] -2 dn/de [erg cm E Chandra (nucleus) Beilicke 2010 IJMPD19, Data non-simultaneous VLBA (43GHz) (2008) BH Magnetosphere, Neronov&Aharonian 2007 Data fit to HESS 2005 flare Takes place at the very BH vincinity compatible with TeV, Fermi, radio Individual blobs in the inner jet close to BH Lenain+08 Model fit to HESS zone SSC Abdo Fermi-LAT (2008/9) 9 10 MAGIC (2008) H.E.S.S. (2004 & 05) Inner jet, Spine- Sheath Tavecchio+08 x probably cannot explain radio 10 VERITAS (2007 ) Energy [ev] Partly published before TeV flaring was known in M87 13
27 2010 Campaign Joint VHE monitoring campaign by MAGIC & VERITAS ToO observations triggered by a VHE high state 1st trigger by MAGIC in 2010 Feb. (ATel #2431) Higher flux state, but no strong flare EVN (European VBLI Net) follow up observations Giovannini+ 2nd trigger by MAGIC & VERITAS in April (ATel #2542) H.E.S.S. started observation Apr. 9 and could confirm high state Full MWL campaign triggered Chandra (D. Harris), Swift (B. Giebels), RXTE, Fermi-LAT, VLBA (C.Walker et al.), EVN, optical polarimetry (U. Barres del Almeida) 15
28 M87: Importance of Results & Future Radio galaxy M 87 Laboratory to probe the origin of VHE emission from SMBH and relativistic jets 2008: H.E.S.S., MAGIC,VERITAS + VLBA, Chandra VHE flare detected, coinciding with rise in radio core and enhanced X-ray core flux Indication for origin of VHE emission very close to the SMBH (<100Rs) 2010: MAGIC,VERITAS, + ToO (H.E.S.S.,VLBA, Chandra,...) VHE high state (Feb) and flare (April) detected (ATel #2431,#2542) MWL campaign triggered (Radio, X-ray, optical polarimetry,...) Analysis ongoing TeV/radio connection: - TeV emission from BH vicinity - Important input for TeV modeling - Accretion & jet formation physics Future questions: - Can pattern be observed repeatedly? - TeV emission & radio core: How close to BH? - More detailed sampling of light curves - Other TeV sources: Similar pattern? 16
29 Do Optical Triggers Work? Mkn 180 ToO trigger MAGIC Collab., ApJ 648 (2006) L105 ApJ 667 (2007) L21 ApJ 704 (2009) L129 March h S=5.5 σ Optical light curves: KVA telescope, La Palma 1ES ToO trigger Flux [mjy] MAGIC MAGIC h S=6.2 σ March-May 2007 S S=6.8 σ April
30 A Continuing Success Story... B th Extragalactic TeV source Optical alerts: 12 alerts, 4 hits R-band flux (calibration star) TeV Discovery MAGIC Collab., ATel 2910 RFO released October 7, 2010 KVA Telescope for MAGIC elevated optical Aug h of observations Oct % Crab nebula (E>100 GeV) >5 standard deviations Triggered Swift-XRT 18
31 A Continuing Success Story... B th Extragalactic TeV source Optical alerts: 12 alerts, 4 hits R-band flux (calibration star) TeV Discovery MAGIC Collab., ATel 2910 RFO released October 7, 2010 KVA Telescope for MAGIC elevated optical Aug h of observations Oct % Crab nebula (E>100 GeV) >5 standard deviations Triggered Swift-XRT 18
32 Perseus Cluster 2008 MAGIC Coll., ApJ 710 (2010) 634 Upper limits on the gamma-ray emission constraining the emission produced by cosmic rays: CR-to-thermal pressure <4% for cluster core, <8% for entire cluster dark matter annihilation: limit consistent with boost factors of 10 4 central radio galaxy NGC1275, compatible with Fermi-LAT detection. Upper limit (E>100 GeV) F < 4.6 to 7.5 x cm 2 s 1 (Γ= 1.5 to 2.5) models with and without galaxies minimum γ flux for radio minihalo hadronic CR interaction with ambient cluster gas 24.4 hr observation during 2008 November and December. 19
33 NGC 1275 Discovered GeV E > 400 GeV MAGIC Collab., ATel 2916 released October 10, 2010 Fermi-LAT No signal >400 GeV from August h of observations 3% Crab nebula (E>100 GeV) 5.2 standard deviations 20
34 Beamed and Unbeamed Gamma-Rays from Galaxies Hotel Olos, Muonio (Lapland), Finland April 11-15, 2011 Local Organizing Committee A. Biland, E. Lindfors, S. Rodriguez, A. Sillanpää (chair), R. Wagner Scientific Organizing Committee C. Dermer, NRL, Washington D.C. t.b.c. A. Levinson, Tel Aviv University L. Maraschi, Brera Observatory A. Marscher, Boston University D. Paneque, MPI München & SLAC A. Reimer, Innsbruck University A. Sillanpää, Tuorla Observatory T. Totani, Kyoto University R. Wagner, MPI München (chair) S. Wagner, LSW Heidelberg t.b.c.
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