2005/9/28 x-ray universe 2005 1 the electron and magnetic field energies in the east lobe of the...
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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]
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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