2005/9/282005/9/28 X-ray Universe 2005X-ray Universe 2005 11

The electron and magnetic field The electron and magnetic field energies in the east lobe of the energies in the east lobe of the

radio galaxy Fornax A, radio galaxy Fornax A, measured with measured with XMM-NewtonXMM-Newton..

Naoki IsobeNaoki Isobe, , Kazuo Makishima (RIKEN)Kazuo Makishima (RIKEN)

Makoto Tashiro, Koichi Ito (Saitama-U),Makoto Tashiro, Koichi Ito (Saitama-U),

Naoko Iyomoto (GSFC), Hidehiro Kaneda (JAXA)Naoko Iyomoto (GSFC), Hidehiro Kaneda (JAXA)

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IC X-ray emission from lobes of radio galaxiesIC X-ray emission from lobes of radio galaxies3C 452 (Isobe et al. 2001) Color : Chandra (0.3-7 keV) Contour : VLA radio image

Energy densities in radio lobes

The IC X-rays is discovered from Fornax Awith ASCA (Kaneda et al. 1995) and ROSAT (Fiegelson et al. 1995)

Croston et al. 2005Isobe et al. 2005

Brunetti et al., Comastri et al., Grandi et al.

ue > um

CMB-boostedM

agn

etic

en

erg

y d

ensi

ty

um

[erg

cm

-3]

Electron energy density ue [erg cm-3]

2005/9/282005/9/28 X-ray Universe 2005X-ray Universe 2005 33

The radio galaxy Fornax A The radio galaxy Fornax A Distance : 18.6 MpcDistance : 18.6 Mpc (Madore et al. 1999)(Madore et al. 1999)

The 4The 4thth brightest radio s brightest radio source in the southern hource in the southern hemisphere.emisphere.

SS2.7 GHz2.7 GHz = 98 ± 1.5Jy = 98 ± 1.5Jy (Ekers 1969)(Ekers 1969)

Double-lobe morphologyDouble-lobe morphology, wi, without any bright hot spots athout any bright hot spots and jets.nd jets.

The dormant nucleusThe dormant nucleus (Iyomoto et al. 1998. Kim & Fabianno 199(Iyomoto et al. 1998. Kim & Fabianno 199

9, Tashiro et al. in this session)9, Tashiro et al. in this session)

uuee = = uumm ? ? (Kaneda et al. 1995, Tashiro et al. 2001)(Kaneda et al. 1995, Tashiro et al. 2001)

20 arcmin

108 kpc

1.5 GHz VLA image (Fomalont et al. 1989)ASCA image

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XMM-NewtonXMM-Newton image of Fornax A (1) image of Fornax A (1) A 60 ksec XMM-Newton oA 60 ksec XMM-Newton o

bservation of the east lobbservation of the east lobe. e.

⇒ ⇒ GTI GTI : 30 ksec for MOS: 30 ksec for MOS. . 0 ksec for PN 0 ksec for PN (due to BGD contamination)(due to BGD contamination) All the east lobe is within All the east lobe is within

the FoV.the FoV. NGC 1316 locates at the FNGC 1316 locates at the F

oV edge.oV edge. 59 sources59 sources are detected. are detected. Integrated flux of detected Integrated flux of detected

sources is smaller than thsources is smaller than the e ASCAASCA flux. flux.

MOS image in 0.3 – 10 keV

10 arcmin

54.1 kpc

⇒ ⇒ diffuse emissiondiffuse emission

NGC 1316

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XMM-NewtonXMM-Newton image of Fornax A (2) image of Fornax A (2)

The The diffuse X-ray diffuse X-ray emissionemission from the east from the east lobelobe is confirmed. is confirmed.

Diffuse X-ray emission Diffuse X-ray emission is also detected, is also detected, between the lobe and between the lobe and host galaxy.host galaxy.

MOS image in 0.3 – 10 keV BGD-subtracted (Read & Ponman 2003) Source-removed, Exposure corrected 1 arcmin smoothing

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X-ray Spectrum outside of the lobeX-ray Spectrum outside of the lobe

Thermal emissionThermal emission

kTkT = 0.77 = 0.77+0.07+0.07-0.12-0.12 keV keV

((AA = 0.3 = 0.3 AAsolarsolar fix) fix)

Consistent with the Consistent with the ASCA resultASCA result

kTkT = 0.77 = 0.77+0.03+0.03-0.04-0.04 keV keV

A = 0.11A = 0.11+0.06+0.06-0.04-0.04

(Iyomoto el al. 199(Iyomoto el al. 1998).8).

r = 2.5 arcmin (13.5 kpc)

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X-ray spectrum of the east lobeX-ray spectrum of the east lobe Power-low model.Power-low model. SS1keV1keV = 86 = 86+19+19

-9-9 nJy nJy XX = 0.62 = 0.62+0.24+0.24

-0.16-0.16

Consistent with the Consistent with the ASCA result.ASCA result.

SS1keV1keV = 110±50 nJy = 110±50 nJy XX = 0.7±0.9 = 0.7±0.9

(Kaneda et al. 1995)(Kaneda et al. 1995)

Slightly harder than Slightly harder than the synchrotron radithe synchrotron radio spectrum.o spectrum.

RR = 0.9 ± 0.2 = 0.9 ± 0.2 (Kaneda et al. 1995)(Kaneda et al. 1995)

r = 10 arcmin (54.1 kpc)

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Spectral Energy DistributionSpectral Energy Distribution

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)

Total East Lobe West Lobe(ASCA)

X-ray : East lobe S1keV = 86+19

-9 nJy X = 0.62+0.24

-0.16

Radio : total S1.4GHz = 44 Jy R = 0.68 ± 0.05

R = X

IC X-rays from synchrotron electrons

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Energetics in the lobes (1)Energetics in the lobes (1)

Radius

S1.4GHz

R

1keV

S1keV

10 arcmin (54.1 kpc)44 Jy0.68 ± 0.050.6290 +8 -9 nJy

East Lobe(XMM-Newton)

West Lobe(ASCA, Tashiro et al. 2001)

7.3 arcmin (Integration region)

50 Jy0.68 ± 0.050.74 ± 0.26100 ±10 nJy

Beq

BIC

um

ue

ue/um

1.551.23+0.08

-0.06 0.60+0.08

-0.06

3.0 ± 0.35.0+1.1

-1.0

G G10-13 erg cm-3 10-13 erg cm-3

1.591.22 ± 0.07 0.59+0.08

-0.06

2.6+0.3-0.2

4.4+1.1-0.9

Electron spectrum

　　∝ 2+1

∝ ue um

∝ ue uCMB

(Harris and Grindlay 1979)

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Energetics in the lobes (2)Energetics in the lobes (2)

Fornax AEast lobe

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SummarySummary XMM-Newton confirmation of the XMM-Newton confirmation of the IC X-ray emissionIC X-ray emission from from

the east lobe of Fornax A. the east lobe of Fornax A.

SS1keV1keV = 86 = 86+19+19-9-9 nJy, nJy, XX = 0.62 = 0.62+0.24+0.24

-0.16-0.16 Evaluation of electron and magnetic energy density. Evaluation of electron and magnetic energy density.

uuee = (3.0 ± 0.3) x 10 = (3.0 ± 0.3) x 10-13-13 erg cm erg cm-3-3

uumm = 0.60 = 0.60+0.08+0.08-0.06-0.06 x 10 x 10-14-14 erg cm erg cm-3-3

Moderate Moderate electron dominanceelectron dominance, even though the nucleus i, even though the nucleus is dormant. s dormant.

uuee//uumm ～ ～ 55

The The uuee will evolve to the equipartition value in will evolve to the equipartition value in ～ ～ GyrGyr (IC (IC + Synchrotron cooling time scale + Synchrotron cooling time scale ～ ～ 2 x 102 x 1088 yr x ( yr x (-2-2..

The IC X-ray and synchrotron radio distribution seems diThe IC X-ray and synchrotron radio distribution seems differentfferent