1 / 11

Naoki Isobe , Kazuo Makishima (RIKEN) Makoto Tashiro, Koichi Ito (Saitama-U),

The electron and magnetic field energies in the east lobe of the radio galaxy Fornax A, measured with XMM-Newton. Naoki Isobe , Kazuo Makishima (RIKEN) Makoto Tashiro, Koichi Ito (Saitama-U), Naoko Iyomoto (GSFC), Hidehiro Kaneda (JAXA). IC X-ray emission from lobes of radio galaxies.

grady-yang
Download Presentation

Naoki Isobe , Kazuo Makishima (RIKEN) Makoto Tashiro, Koichi Ito (Saitama-U),

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. The electron and magnetic field energies in the east lobe of the radio galaxy Fornax A, measured with XMM-Newton. Naoki Isobe, Kazuo Makishima (RIKEN) Makoto Tashiro, Koichi Ito (Saitama-U), Naoko Iyomoto (GSFC), Hidehiro Kaneda (JAXA) X-ray Universe 2005

  2. IC X-ray emission from lobes of radio galaxies 3C 452 (Isobe et al. 2001) Color : Chandra (0.3-7 keV) Contour : VLA radio image Energy densities in radio lobes ue > um Magnetic energy density um[erg cm-3] Croston et al. 2005 Isobe et al. 2005 Brunetti et al., Comastri et al., Grandi et al. Electron energy density ue [erg cm-3] CMB-boosted The IC X-rays is discovered from Fornax A with ASCA(Kaneda et al. 1995)and ROSAT(Fiegelson et al. 1995) X-ray Universe 2005

  3. 20 arcmin 108 kpc The radio galaxy Fornax A 1.5 GHz VLA image (Fomalont et al. 1989) ASCA image • Distance : 18.6 Mpc (Madore et al. 1999) • The 4th brightest radio source in the southern hemisphere. S2.7 GHz = 98 ± 1.5Jy (Ekers 1969) • Double-lobe morphology, without any bright hot spots and jets. • The dormant nucleus (Iyomoto et al. 1998. Kim & Fabianno 1999, Tashiro et al. in this session) • ue = um ? (Kaneda et al. 1995, Tashiro et al. 2001) X-ray Universe 2005

  4. 10 arcmin 54.1 kpc NGC 1316 XMM-Newton image of Fornax A (1) MOS image in 0.3 – 10 keV • A 60 ksec XMM-Newton observation of the east lobe. ⇒ GTI : 30 ksec for MOS. 0 ksec for PN (due to BGD contamination) • All the east lobe is within the FoV. • NGC 1316 locates at the FoV edge. • 59 sources are detected. • Integrated flux of detected sources is smaller than the ASCA flux. ⇒ diffuse emission X-ray Universe 2005

  5. XMM-Newton image of Fornax A (2) MOS image in 0.3 – 10 keV • BGD-subtracted (Read & Ponman 2003) • Source-removed, • Exposure corrected • 1 arcmin smoothing • The diffuse X-ray emissionfrom the east lobe is confirmed. • Diffuse X-ray emission is also detected, between the lobe and host galaxy. X-ray Universe 2005

  6. r = 2.5 arcmin (13.5 kpc) X-ray Spectrum outside of the lobe • Thermal emission kT = 0.77+0.07-0.12 keV (A = 0.3 Asolar fix) • Consistent with the ASCA result kT = 0.77+0.03-0.04 keV A = 0.11+0.06-0.04 (Iyomoto el al. 1998). X-ray Universe 2005

  7. r = 10 arcmin (54.1 kpc) X-ray spectrum of the east lobe • Power-low model. S1keV = 86+19-9 nJy aX = 0.62+0.24-0.16 • Consistent with the ASCA result. S1keV = 110±50 nJy aX = 0.7±0.9 (Kaneda et al. 1995) • Slightly harder than the synchrotron radio spectrum. aR = 0.9 ± 0.2 (Kaneda et al. 1995) X-ray Universe 2005

  8. IC X-rays from synchrotron electrons Spectral Energy Distribution aR = aX X-ray : East lobe S1keV = 86+19-9 nJy aX = 0.62+0.24-0.16 Radio : total S1.4GHz = 44 Jy aR = 0.68 ± 0.05 29.9 MHz 100 MHz : Finlay & Jones (1973) 408 MHz : Robertoson (1973) 843 MHz : Jones & McAdam (1992) 1.4 GHz : Ekers et al (1983) 2.7 GHz : Ekers (1969) 5.0 GHz : Kuhr et al. (1981) TotalEast Lobe West Lobe(ASCA) X-ray Universe 2005

  9. ∝ ueum Electron spectrum 　　∝ g2a+1 ∝ ue uCMB mG mG 10-13 erg cm-3 10-13 erg cm-3 1.55 1.23+0.08-0.06 0.60+0.08-0.06 3.0 ± 0.3 5.0+1.1-1.0 Beq BIC um ue ue/um 1.59 1.22 ± 0.07 0.59+0.08-0.06 2.6+0.3-0.2 4.4+1.1-0.9 Energetics in the lobes (1) East Lobe (XMM-Newton) West Lobe (ASCA, Tashiro et al. 2001) 10 arcmin (54.1 kpc) 44 Jy 0.68 ± 0.05 0.62 90 +8 -9 nJy 7.3 arcmin (Integration region) 50 Jy 0.68 ± 0.05 0.74 ± 0.26 100 ±10 nJy Radius S1.4GHz aR a1keV S1keV X-ray Universe 2005 (Harris and Grindlay 1979)

  10. Fornax A East lobe Energetics in the lobes (2) X-ray Universe 2005

  11. Summary • XMM-Newton confirmation of the IC X-ray emission from the east lobe of Fornax A. S1keV = 86+19-9 nJy, aX = 0.62+0.24-0.16 • Evaluation of electron and magnetic energy density. ue = (3.0 ± 0.3) x 10-13 erg cm-3 um = 0.60+0.08-0.06 x 10-14 erg cm-3 • Moderate electron dominance, even though the nucleus is dormant. ue/um～ 5 • The ue will evolve to the equipartition value in ～ Gyr (IC + Synchrotron cooling time scale ～ 2 x 108 yr x (g/104)-2. • The IC X-ray and synchrotron radio distribution seems different X-ray Universe 2005

More Related