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Particles and Fields in Lobes of Radio Galaxies

Particles and Fields in Lobes of Radio Galaxies. Naoki Isobe (NASDA, MAXI Mission) Makoto Tashiro (Saitama Univ.) Kazuo Makishima (Univ. of Tokyo) Hidehiro Kaneda, Naoko Iyomoto (ISAS). Jet. Hot Spot. Nucleus. Lobe. time-integrated information on past activities of the jets.

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Particles and Fields in Lobes of Radio Galaxies

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  1. Particles and Fieldsin Lobes of Radio Galaxies Naoki Isobe (NASDA, MAXI Mission) Makoto Tashiro (Saitama Univ.) Kazuo Makishima (Univ. of Tokyo) Hidehiro Kaneda, Naoko Iyomoto (ISAS)

  2. Jet Hot Spot Nucleus Lobe time-integrated information on past activities of the jets Lobes of Radio Galaxies Cygnus A (VLA 1.4 GHz) Huge electron and magnetic field energies

  3. ue : energy density of electrons um: energy density of magnetic fields V : Volume of the Lobe • X-ray Emission Inverse Compton (IC) Scattering by SR electrons of the Cosmic Microwave Background (CMB) photons Flux : FIC∝ ueuCMBV Index :aIC uCMB : energy density of CMB 4.1 x 10 –13 (1 + z) 4 erg cm-3 = aSR ue and um Emission from Lobes and Physical Parameters • Radio Emission Synchrotron Radiation (SR) Flux : FSR∝ ueumV Index : aSR Comparing FSR and FIC

  4. IC X-Rays aX = 0.74 ～aSR 20’ = 135 kpc Discovery of IC X-rays from Lobes • Fornax A (NGC 1316, Kaneda et al. 1995, Tashiro et al. 2001) ue=2 x 10-13 erg cm-3 um=4.6 x 10-13erg cm-3 (B=3 mG) Nearly Equipartition

  5. Discovery of IC X-rays from Lobes • Centaurus B (z = 0.01215, Tashiro et al. 1998) ue = 2.4 x 10-12erg cm-3 um = 3.8 x 10-13erg cm-3 (B～ 3 mG) 10 arcmin (140 kpc) Electron Dominant ue / um= 6.3 Color : GIS 1.5 -3 keV Contour : VLA 843 MHz (McAdam et al. 1991 )

  6. ASCA Results • 4C 73.08 (z = 0.0571) • NGC 612 (z = 0.0290) 5 arcmin = 300 kpc 5 arcmin = 160 kpc Color : 0.7 – 3 keV Contour : 843 MHz (Jones & McAdam 1992) Color : 0.5 – 2 keV Contour : 608 MHz ue = 1.7 x 10-13 erg cm-3 um = 4.8 x 10-15 erg cm-3 ue = 4.3 x 10-13 erg cm-3 um = 2.1 x 10-14 erg cm-3

  7. Chandra Results • 3C452 (z = 0.0811) • 3C427.1 (z=0.572) Color : 0.3 – 7 keV Contour : 1.4 GHz 2 arcmin = 160 kpc Color : 0.3–7 keV, Contour : 1.4 GHz 10 arcsec = 50 kpc (Isobe et al. 2002 ApJL) 2 arcmin = 80 kpc • Pictor A (z = 0.0351) 0.3 – 7 keV

  8. Chandra Results • 3C452 (z = 0.0811) Thermal Comp. kT～ 1 keV PL comp. aX = 0.65 ～aSR IC X-rays from the SR electrons

  9. Chandra Results • 3C452 (z = 0.0811) • 3C427.1 (z=0.572) Color : 0.3 – 7 keV Contour : 1.4 GHz 2 arcmin = 160 kpc ue=3.0x10-10 erg cm-3 um=7.4x10-12 erg cm-3 Color : 0.3–7 keV, Contour : 1.4 GHz 10 arcsec = 50 kpc ue=2.1 x 10-12 erg cm-3 um=7.7 x 10-14 erg cm-3 2 arcmin = 80 kpc • Pictor A (z = 0.0351) ue=4.6 x 10-12 erg cm-3 um=1.3 x 10-13 erg cm-3 0.3 – 7 keV

  10. XMM-Newton Results • 3C 98 (z = 0.0306) • Centaurus B Color : 0.3 – 10 keV Contour : 4.8 GHz 2 arcmin = 70 kpc ue=5.1 x 10-12 erg cm-3 um=1.7 x 10-13 erg cm-3 (Isobe et al. in preparation) (Tashiro et al. in preparation)

  11. Equipartition ue=um Small Lobes < 50 kpc ue= 100um um [erg cm-3] Large Lobes > 100 kpc ue> 10um ～ ue [erg cm-3] ue and um in Radio Lobes 100 mG 10 mG 1 mG ge = 103 – 105

  12. Equipartition ueV=umV Magnetic Energy :umV [1058 erg] ueV= 100umV Electron Energy : ueV [1058 erg] Total Energies in Radio Lobes ～2 orders ～2 orders

  13. Electron EnergyueV [1058 erg] Luminosity of NucleusLX [1040 erg s-1] Relation to the Nucleus –electron energy- ueV∝LX

  14. Magnetic EnergyumV [1058 erg] Luminosity of NucleusLX [1040 erg s-1] Relation to the Nucleus –magnetic field- umV seems independent of LX (nearly constant ?)

  15. Spatial Distribution of IC X-rays • Chandra Observation of 3C 452 Point Sources X-ray Profile relatively uniform Radio Profile rim-brightening

  16. FSR FIC ∝um Spatial Distribution of Physical Parameters Equipartition ue/um～100

  17. Spatial Distribution of Physical Parameters • Fornax A • Centaurus B um/uemap Radial Profile of IC X-rays and SR radio

  18. Summaries • With ASCA, Chandra and Newton, we have detected the IC X-rays from the lobes of numbers of radio galaxies, and accurately determined ueand um in these lobes. • ue tend to dominate umtypically an order of magnitude. • The electron energy, ueV, seems to be proportional to the nuclear luminosity, although the magnetic energy, umV seemsindependent. • In several lobes, the electrons are relatively uniformly distributed, although the magnetic fields seem to be compressed toward the edges of the lobes. • All of these results strongly indicates that the electrons (i.e. particles) pay more important roles in the formation of the jets, and/or the evolution of the radio galaxies/lobes.

  19. Please e-mail to isobe@oasis.tksc.nasda.go.jp

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