Hard Electron Spectra and Polariza2on Proper2es of Rela2vis2c Jets Lukasz Stawarz ISAS/JAXA (Japan)
Outline Radio Galaxies (M 87) FSRQs BL Lacs Large- Scale Quasar Jets X- ray Binaries (Cyg X- 1) Broad- band observa-ons and polarimetry of jet sources constraining electron spectra and hence par-cle accelera-on processes in rela-vis-c ou:lows
M87 Jet LS et al. 06 Cheung, Harris & LS 07 HST- 1 knot in M87 jet: nozzle of a reconfinement shock?
Superluminal Blob Ejec2on Cheung, Harris & LS 07
HST- 1 Flare Harris et al. 09, 11, 12 Perlman et al. 11 Kollgaard et al. 90
Standing Shock Perlman et al. 11: par2cle accelera2on in a standing shock, with cooling from both par2cle aging and the relaxa2on of the compression
TeV Emission of M87:??? Abramowski et al. 12 [H.E.S.S., VERITAS, MAGIC, Fermi- LAT, ++] (Raue & LS)
Luminous Blazars (FSRQs) 3C 279 Abdo et al. 10 [Fermi- LAT, ++], Hayashida et al. 12
Low- Energy Electrons Sikora, LS, et al. 09 IGR J22517+2217 (Lanzuisi et al. 12) Flat (s e < 2.0) low- energy (E e < Γ sh m p c 2 ) electron spectra consistent with accelera2on by resonant absorp2on of cyclotron waves emiged by the ions reflected from rela2vis2c, perpendicular shock (Hoshino et al. 92, Amato & Arons 06)
High- Energy Electrons E 2 dn/de [erg cm -2 s -1 ] 10-8 10-9 10-10 10-11 First flare Inter-flare Second flare 3C 454.3 (flaring) 10 3 10 4 10 5 Energy [MeV] Tanaka, LS et al. 11 PKS 1222+216 Spectral breaks consistent with either intrinsic breaks in high- energy segments of electron con2nua, or with the annihila2on of the GeV photons on H- I and He- II Lyman recombina2on con2nuum and line emission inside the zone of the highest ioniza2on of the broad line region, within 0.1 pc (see Poutanen & Stern 10).
DSA in Rela2vis2c Regime Diffusive rela2vis2c shock accelera2on: variety of PLs and BPLs depending on the shock condi2ons, like magne2c field configura2on, turbulence spectrum, shock magne2za2on and velocity (Niemiec & Ostrowski 04, Sironi & Spitkovsky 09, 11)
Rapid Variability Saito, LS et al. 13: flux doubling 2mescale <1h implies very compact emission region size <0.01 pc in PKS 1510-089
TeV Emission of FSRQs:??? Tanaka, LS et al. 11, Tavecchio et al. 11 Aleksic et al. 11 [MAGIC, Fermi- LAT]
Low- luminosity Blazars (BL Lacs) the flattest synchrotron spectrum α = - 1/3 the corresp. (Th. regime) SSC spectrum α = - 1/3 Katarzynski et al. 06
Minimum Electron Energies Combined UV to X- ray data support the idea of very high electron minimum Lorentz factors in BL Lacs, E/m e c 2 10 3 3 10 5 High electron minimum Lorentz factors can help to explain the problem of inverse Compton catastrophe and high brightness temperature of BL Lacs (Tsang & Kirk 07) This may indicate the dominant role of turbulent electron accelera2on in rela2vis2c jets of BL Lacs (e.g., Katarzynski et al. 06, LS & Petrosian 08, Asano et al. 14) 1ES 0347 121 (Tanaka, LS et al. 14) γ min = 2 10 4
Turbulent Accelera2on q=2 (Jones 70, Schlickeiser 84, Bogdan & Schlickeiser 1985, Park & Petrosian 95, LS & Petrosian 08)
Slow and Inefficient? same scaling! Jones 94, Petrosian 12
Standard Shock Spectrum E 2 N(E) non- rela2vis2c shocks Γ sh m e c 2 GeV TeV E
Electron Spectra in FSRQs E 2 N(E) proton- mediated rela2vis2c shocks? Fermi- LAT spectra flat hard X- ray spectra (no Bulk- Compton in sox X- rays) Γ sh m e c 2 GeV TeV E
Electron Spectra in BL Lacs E 2 N(E) rela2vis2c turbulence? UV to X- ray spectra flat (EBL- corrected) γ- ray spectra ( Compton- catastrophe limit) Γ sh m e c 2 GeV TeV E
Broad- Band Polarimetry 2.0 1.5 1.0 s 1.5, a 0.5 s 2.0, a 1.0 s 2.5, a 1.5 maximum polariza-on degree log Ν'FΝ' 0.5 0.0 0.5 1.0 12 13 14 15 16 17 18 19 1.0 0.9 0.8 0.7 0.6 s 1.5, a 0.5 s 2.0, a 1.0 s 2.5, a 1.5 log Ν' Hz 0.5 12 13 14 15 16 17 18 log Ν' Hz γ min = 10 3 γ max = 10 5 γ eq = 3 10 4 Β = 1G E. Angelakis: higher synchrotron cut- offs/flaher electron spectra in gamma- ray quiet sample?
Large- Scale Quasar Jets 3C 273 - Jester et al. 02/07, Uchiyama et al. 06 UV emission is polarized, thus synchrotron in origin, implying that X- rays are also due to synchrotron emission of a flat- spectrum high- energy electron popula2on (as originally proposed in LS & Ostrowski 02, LS et al. 04)
Large- Scale Quasar Jets PKS 1136 135 Cara et al. 13 γ min = 3 10 6
TeV Flares of BL Lacs:??? Aharonian et al. 07/09 [H.E.S.S.]: TeV variability of BL Lac- type blazar PKS 2155-304 with flux doubling 2mescale t var ~ 200 s
Quiescent Blazar Spectra Mrk 501 Abdo et al. [Fermi- LAT, MAGIC, VERITAS, ++] 11 (Paneque & LS) Are such fits meaningful at all?
Cyg X- 1 Zdziarski, LS, Pijanka, & Sikora 14 (arxiv:1307.1309) Zdziarski, Pijanka, Sikora, & LS 14 (arxiv:1403.4768) from H. Odaka
Broad- band spectra of Cyg X- 1 jets in a hard state of the source, evaluated self- consistently assuming injec2on of fresh electrons from compact accelera2on regions distributed within the en2re ou}low, and subsequent electron energy losses (adiaba2c and radia2ve, including SYN, SSC, BBC, XC, with all the anisotropy, orbital, KN, and pair produc2on effects taken into account)
d EF E d lnξ 1 0.1 0.01 0.001 10 4 10 5 10 6 a 10 6 0.001 1 1000 10 6 E ev
1 d EF E d lnξ 0.01 10 4 10 6 c 10 6 0.001 1 1000 10 6 E ev
100 d EF E d lnξ 1 0.01 10 4 10 6 b 10 6 0.001 1 1000 10 6 E ev
d EF E d lnξ 100 1 radio! 0.01 10 4 10 6 opt. thin b 10 6 0.001 1 1000 10 6 E ev LP > 50% @ >200keV LP < 5% @5GHz
TeV Emission of Cyg X- 1:???
Conclusions Variety of electron spectra formed in rela2vis2c jets (PLs, BPLs, UM?) High minimum electron energies/very flat low- energy segments in electron spectra! Variety of par2cle accelera2on processes involved (shocks, turbulence, reconnec2on?) A role of a broad- band polarimetry Flaring vs. quiescence jet emission; problema2c TeV flares