The 2010 M 87 VHE flare and its origin: the MWL picture Martin - PowerPoint PPT Presentation

The 2010 M 87 VHE flare and its origin: the MWL picture Martin Raue for the H.E.S.S., MAGIC, VERITAS, and Fermi/ LAT Collaborations and the M 87 MWL Monitoring Team “High Energy Phenomena in Relativistic Outflows III” Barcelona, June 27 - July 1, 2011 martin.raue@desy.de H E S S

Giant radio galaxy M 87 radio (VLA) radio (VLA) Distance: ~16 Mpc Central BH: M BH ~ 3-6 × 10 9 M ⊙ optical (HST) Jet angle: ~20-30° ~2 kpc (20’’) Outer radio lobes (0.2 x 0.2 deg) X-ray (Chandra) Highly structured inner jet (kpc) resolved in radio, optical, X-ray VHE emission (HEGRA ’99) Short-term VHE variability (H.E.S.S. 2005) e.g. Curtis (1918), Biretta et al. (1999), Gebhardt & Thomas (2009), Aharonian et al. (2003), Aharonian et al. (2005) 2

Origin of the VHE emission Dark matter annihilation ? CR in M 87 ? ? Intra-cluster gas ? Large scale jets Inner/Outer-jet ? ? Hadronic/Leptonic ? ? Knots? HST1? Vicinity of black hole ... E. A. Baltz et al. (2000), C. Pfrommer and T. A. Enßlin (2003), Stawarz et al. (2005), Georganopoulos, et al. (2005), J.-P . Lenain et al. (2008), A. Reimer et al. (2004), Neronov & Aharonian (2007), Rieger & Aharonian (2008), Barkov et al. (2010) 3

Origin of the VHE emission Dark matter annihilation ✖ ? CR in M 87 ✖ ? ? Intra-cluster gas ✖ ? Large scale jets ✖ Inner/Outer-jet ✔ ? ? Hadronic/Leptonic ? ? Knots? HST1? ( ✔ ) Short term VHE variability Vicinity of black hole ✔ (~days) places strong size ... constraints r < 5 × 10 15 δ cm E. A. Baltz et al. (2000), C. Pfrommer and T. A. Enßlin (2003), Stawarz et al. (2005), Georganopoulos, et al. (2005), J.-P . Lenain et al. (2008), A. Reimer et al. (2004), Neronov & Aharonian (2007), Rieger & Aharonian (2008), Barkov et al. (2010) 4

HST-1: flare (2005) HST-1 = First bright feature in the jet resolved by Hubble Cheung et al. 2009 Underwent major flux outburst in 2005 (X-ray, optical, radio) Contemporaneous VHE Harris et al. 2009 activity detected in 2005 Time scale different Sub-structure, super-luminal features 5

Core: VHE vs MWL (2008) 20 A 20 VHE instruments VERITAS ] -1 s MAGIC -2 cm H.E.S.S. 10 ] -1 -12 s [10 -2 cm 10 VHE Φ -12 0 [10 H.E.S.S., MAGIC, VERITAS, VHE 29 Jan 05 Feb 12 Feb Time Φ VLBA, & Chandra 0 VHE flares coincides with 4 B [keV/s] increased radio and X-ray flux Chandra (2-10 keV) 2 knot HST-1 nucleus X-ray in the core Φ 0 C VLBA (43 GHz) 2 2 Indication for emission from nucleus (r = 1.2 mas) peak flux density jet w/o nucleus (1.2-5.3 mas) vicinity of the SMBH 1.5 1.5 [Jy] [Jy] radio radio 1 1 Φ Φ 0.5 0.5 02 Apr 2007 02 Jul 2007 01 Oct 2007 01 Jan 2008 01 Apr 2008 Time Acciari et al. (2009) 6

2010 VHE monitoring campaign Joint VHE monitoring campaign MAGIC & VERITAS ToO: H.E.S.S., Chandra (D. Harris et al.) , 43 GHz VLBA (C. Walker et al.) 7

M 87 - 2010 VHE campaign PRELIMINARY 2. ATel - ToO 1. ATel - Mariotti et triggered - Ong & al. 2010 Mariotti 2010 ~80h observation time 8

M 87 - 2010 VHE flare Parameter Value Units Fit range 55290 - 55299 MJD τ rise 1 . 69 ± 0 . 30 d d τ decay 0 . 611 ± 0 . 080 d d t 0 55295 . 954 ± 0 . 094 MJD m − 2 s − 1 (2 . 01 ± 0 . 15) × 10 − 11 Φ 0 N ote . — χ 2 / d.o.f. = 10 . 02 / 11 with chance probability P = 0 . 53. 21 observations in 15 days Well described by 2 x exponential function PRELIMINARY Doubling time 0.6 ± 0.08 days 9

VHE flares from 2005 to 2010 2010 vs 2005 statistics in 2005 to low, but 2005 seems more extended 2010 vs 2008 2008 more erratic? Quantify PRELIMINARY 10

PRELIMINARY M 87 - MWL VHE lightcurve HE Instruments H.E.S.S., MAGIC, VERITAS, Fermi, Chandra, X-RAY HST, LT, VLBA, MOJAVE, VLA, EVN OPTICAL RADIO 11

PRELIMINARY M 87 - MWL Core & HST-1 lightcurve Core & HST-1 Instruments H.E.S.S., MAGIC, Core VERITAS, Fermi, Chandra, HST, LT, VLBA, MOJAVE, HST-1 VLA, EVN Components Core / HST-1 Core HST-1 Core Core Madrid et al. 2007 HST HST-1 Chandra 12

VHE vs radio core PRELIMINARY 13

VHE vs X-ray PRELIMINARY Poster by D. Harris et al. 14

VHE vs HE/O/... Fermi Steady source (marginal variable?) HST / LT HST-1 flare 2005 LT: no strong activity in 2010 Radio HST-1 PRELIMINARY HST-1 flare 2005 15

Optical polarimetry Poster by E. Perlmann et al. PRELIMINARY 16

Conclusions M 87 Nearby (16 Mpc) VHE radio galaxy with massive SMBH Short-term VHE variability ~1 day 2010 campaign VHE monitoring by MAGIC & VERITAS (ToO: H.E.S.S., Chandra, VLBA) VHE flare detected t d < 1 day (excellent sampling) NO rise in the 43 GHz radio core emission Enhanced X-ray core emission (Chandra) Origin of the VHE emission? No unique solution? 2005: HST-1? 2008: Core? 2010: ? .. but X-ray core (2008/10) Full paper in preparation 17