Large-scale emission from FR I jets Pol Bordas with the - PowerPoint PPT Presentation

Large-scale emission from FR I jets Pol Bordas with the collaboration of V. Bosch-Ramon & M. Perucho Barcelona June 2011, miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III OUTLINE ● The FR I/II dichotomy ● FR jets/medium interaction ● Large scale emission in FR I jets ● Summary & conclusions miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III The FR I - FR II dichotomy Active galactic nuclei Radio-loud (~10%), eliptical Radio-quiet (~90%), spiral Jet stuck in matter 100 kpc scale jet Optically weak Optically strong Broad Broad Narrow L 178 > 2.5·10 26 W/Hz L 178 < 2.5·10 26 W/Hz Lines Lines Lines Radio weak Radio Interm. Seyfert I Seyfert II quasar quasar Radio quasar GPS/CSS FR II BL Lac radio galaxy SSRQ FSRQ HBLs LBLs FR I radio galaxy Blazar miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III The FR I - FR II dichotomy Active galactic nuclei Radio-loud (~10%), eliptical Radio-quiet (~90%), spiral Jet stuck in matter 100 kpc scale jet Optically weak Optically strong Broad Broad Narrow L 178 > 2.5·10 26 W/Hz L 178 < 2.5·10 26 W/Hz Lines Lines Lines Radio weak Radio Interm. Seyfert I Seyfert II quasar quasar Radio quasar GPS/CSS FR II BL Lac radio galaxy SSRQ FSRQ HBLs LBLs FR I radio galaxy Blazar “(...) radio sources were classified using the ratio (...) there is a sharp division in luminosity (r) of the distance between the regions of highest between the two classes; those with brightness to the total extent of the source luminosities at 178 MHz below 2 x 10 25 W/ measured from the lowest (energy) contour into Hz are nearly all of Class I, and those Class 1 (r < 0.5) and Class II (r > 0.5). above nearly all of Class II Fanaroff & Riley, 1974, MNRAS , 167, 31 miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III The FR I - FR II dichotomy Ledlow & Owen, 1996, AJ , 112, 9 Ghisellini & Celotti, 2001, A&A , 379, L1 miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III The FR I - FR II dichotomy fundamental differences ● jet composition: FR I → e + - e - plasma (Reynolds et al. 1996); FR II → e - - p plasma (Celotti et al. 1997) ● black hole spin (Blandford & Znajek 1977, Rees 1982, Meier 1999) ● jet power - accretion rate (Gopal-Krishna 1988, Blandford 1996, Ghisellini & Celotti 2001) ● jet magnetic field at large scales (|| to jet axis in FR II, ⊥ in FR I’s) interaction with the medium ● jet deceleration against the ambient gas (Begelman 1982; Gopal-Krishna & Wiita 1988, 2001) ● both FR I and II jets are relativistic near the core. FR I much slower at large distances (Bicknell 1995) ● jet bending is common in FR I, not in FR II ● observation of hybrid sources (Gopal-Krishna & Wiita 2000) miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III The FR I - FR II dichotomy 0131-36A IPOL 4885.100 MHZ NGC612AAA.ICLN.1 -36 42 DECLINATION (B1950) 43 44 45 46 47 01 32 00 31 45 30 15 RIGHT ASCENSION (B1950) Gopal-Krishna & Wiita, 2000, A&A . 363, 507 HYMORS: HYbrid MOrphology Radio Sources e.g. NGC 612: “ 5 GHz radio maps show that the eastern lobe has a bright hotspot near its outer edge (FR II type), whereas the western lobe exhibits a jet-like structure which widens steadily and fades into a diffuse radio plume (FR I) ” miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III FR jets/medium interaction Chandra HS Nucleus VLA image of 3C351 at 1.4 GHz with Chandra X- M87 as seen by Chandra plus with 8 GHz contours. ray contours superposed. From Brunetti et al. 2001, From Harris & Krawczynski, 2006, ARA&A . 44, 463 ApJ , 561,L157 miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III FR jets/medium interaction Hot Spots entrainment FR II FR I of external material cocoon cocoon shell shell contact disrupted jet discontinuity miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III rest-mass density FR II jets/medium interaction: numerical simulations ● jet composition, whether e + - e - or e - - p plasma does not affect strongly the propagation of FR II jets plasma ● Relativistic jets may be very efficient in reheating the ICM → cooling flow problem rest-mass density temperature Perucho et al. (in preparation) Scheck et al. 2002, MNRAS , 331, 615 miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III FR II jets/medium interaction: analytical models bow shock reverse shock reconfnement shock 6 7 FR II z reconf 45 46 -25 g cm ρ 0 d -β -3 ρ ; ρ 0 ≈ 2 x med [ med shocked jet l b - β FR II med cocoon FR II r b med med med med med med med miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III FR II jets/medium interaction: non-thermal emission lobe lobe shell shell ● strong photon fields: UV disk , IR torus , NIR host-galaxy ● moderately powerful jets (L jet ~10 45 erg cm -2 s -1 ) ● evolution through source size: R 1 = 1 to 100 kpc lobe ● fixed magnetic field = 10 -5 G ● spectral aging shell ● One zone model for each t source Ito et al. 2011, ApJ , 730, 120 miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III FR I jets/medium interaction: numerical simulations Perucho & Martí, 2007, MNRAS , 382, 526 miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III FR I jets/medium interaction: numerical simulations shell pressure shell density cocoon pressure cocoon density Perucho & Martí, 2007, MNRAS , 382, 526 miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III FR I jets/medium interaction: radiative model miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III FR I jets/medium interaction: radiative model Bordas, Bosch-Ramon & Perucho, 2011, MNRAS . 412, 1229 miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III FR I jets/medium interaction: radiative model μ-waves VHE γ-rays HE γ-rays HE γ-rays optical μ-waves X-rays optical X-rays o radio i UV d IR UV a IR r 42 42 10 10 5 yr 5 yr t src = 10 t src = 10 shell 6 yr 6 yr t src = 3 x 10 t src = 3 x 10 41 41 10 10 8 yr 8 yr t src = 10 t src = 10 RH cocoon cocoon 40 40 10 10 -1 ) -1 ) Av log ν L ν (erg s log ν L ν (erg s 39 39 10 10 38 38 10 10 37 37 10 10 36 36 10 9 10 11 10 13 10 17 10 19 10 21 10 23 10 27 10 29 10 10 15 10 25 10 7 31 9 11 13 15 17 19 21 10 10 10 10 10 10 10 10 10 log ν (Hz) log ν (Hz) Bordas, Bosch-Ramon & Perucho, 2011, MNRAS . 412, 1229 miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III FR I jets/medium interaction: radiative model 44 44 10 10 Radio X-rays 43 43 10 10 42 42 10 10 -1 ) -1 ) log L 1-10 keV (erg s log L 5GHz (erg s 41 41 10 10 40 40 10 10 39 39 10 10 shell cocoon 38 38 10 10 total 37 37 10 10 5 6 7 8 5 6 7 8 10 10 10 10 10 10 10 10 log t src (yr) log t src (yr) 44 44 10 10 HE γ -rays VHE γ -rays 43 43 10 10 42 42 10 10 -1 ) -1 ) log L 0.1-100 GeV (erg s log L >100 GeV (erg s 41 41 10 10 40 40 10 10 39 39 10 10 38 38 10 10 37 37 10 10 5 6 7 8 5 6 7 8 10 10 10 10 10 10 10 10 log t src (yr) log t src (yr) Bordas, Bosch-Ramon & Perucho, 2011, MNRAS . 412, 1229 miércoles 29 de junio de 2011

Large-scale emission in FR I jets Pol Bordas, HEPRO III FR I jets/medium interaction: radiative model ● Bolometric thermal emission increases with time: despite shell density and bow shock velocity decrease, t thermal > t src . Peak of thermal emission shifted to lower energies as t src increases ● Radio : fluxes up to 10 -12 (d/100 Mpc) -2 erg cm -2 s -1 (~few Jy) in a region of ~10 arcmin - 3C 31: F 5GHz = 3 × 10 40 erg/s, Andernach et al. 1992) - 3C 15: F 5GHz ~ 10 -14 erg cm -2 s -1 (d = 300 Mpc) ● X-rays : thermal : Fluxes ~10 -13 erg cm -2 s -1 for t src = 10 8 yrs. Hard X-rays in more compact regions (~1 arcmin) along the jet apex; soft X-rays from the whole shell. non-thermal: cocoon dominates in our model, though limb brightening effects may make the shell brighter (Cen A?) - X-ray fluxes at the level of those reported, e.g., for 3C 15 (Kataoka et al. 2003) ● HE gamma-rays : ν L ν ~10 39 -40 erg/s for t src = 10 7-8 yrs, Γ ph ≈ 2.3 - Cen A by Fermi: ~ 10 -11 erg cm 2 s -1 => ~10 40 erg/s (d = 3 Mpc). - Distant sources --> higher non-thermal efficiencies/L jet but enough angular resolution? ● VHE gamma-rays : ν L ν ~10 37 - a few × 10 38 erg/s for t src = 10 7 -10 8 yrs - steep spectrum above ~1 TeV; faint extended flux => long t obs required ! - angular resoultions at ~arcmin (=> CTA?) miércoles 29 de junio de 2011