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Hard X-ray study of lobes of radio galaxy Fornax A Naoki Isobe (RIKEN/ Suzaku Help Desk) Makoto Tashiro, Hiromi Seta, Yuichi Yaji (Saitama Univ.) Keiko Matsuta, Hidehiro Kaneda (ISAS/JAXA), Kazuo Makishima (RIKEN/Univ.of Tokyo) etc. Radio Galaxy Fornax A

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hard x ray study of lobes of radio galaxy fornax a

Hard X-ray study of lobes of radio galaxy Fornax A

Naoki Isobe

(RIKEN/Suzaku Help Desk)

Makoto Tashiro, Hiromi Seta, Yuichi Yaji (Saitama Univ.)

Keiko Matsuta, Hidehiro Kaneda (ISAS/JAXA),

Kazuo Makishima (RIKEN/Univ.of Tokyo)etc.

Radio Galaxies in the Chandra Era

radio galaxy fornax a
Radio Galaxy Fornax A
  • Nearby radio galaxy (D = 18.6 Mpc)
  • The 1st source, from whichthe lobe IC X-ray emission was detected with ASCA and ROSAT(e.g., Kaneda et al. 1995)
  • The flux of IC X-ray emission indicate a magnetic field of 1.2 mG (Isobe et al. 2006) , which is slightly smaller than the field under the minimum energy condition (1.55mG).
  • The X-ray/radio distribution suggest a homogeneous electron and edge-strengthened magnetic field distributions (Tashiro et al. 2001) .

Color : ASCA (2-10 keV)

Contour : VLA 1.4 GHz

Radio Galaxies in the Chandra Era

radio galaxy fornax a3
Radio Galaxy Fornax A
  • Nearby radio galaxy (D = 18.6 Mpc)
  • The 1st source, from whichthe lobe IC X-ray emission was detected with ASCA and ROSAT(e.g., Kaneda et al. 1995)
  • The flux of IC X-ray emission indicate a magnetic field of 1.2 mG (Isobe et al. 2006) , which is slightly smaller than the field under the minimum energy condition (1.55mG).
  • The X-ray/radio distribution suggest a homogeneous electron and edge-strengthened magnetic field distributions (Tashiro et al. 2001) .

XMM-Newton Spectrum

of Fornax A east lobe

GX = 1.62 -0.15 +0.24

(Isobe et al. 2006)

Radio Galaxies in the Chandra Era

radio galaxy fornax a4
Radio Galaxy Fornax A
  • Nearby radio galaxy (D = 18.6 Mpc)
  • The 1st source, from whichthe lobe IC X-ray emission was detected with ASCA and ROSAT(e.g., Kaneda et al. 1995)
  • The flux of IC X-ray emission from the east lobe indicate a magnetic field of 1.2 mG (Isobe et al. 2006) , which is slightly smaller than the field under the minimum energy condition (1.55mG).
  • The X-ray/radio distribution suggest a homogeneous electron and edge-strengthened magnetic field distributions (Tashiro et al. 2001) .

ASCA (2-10 keV)

VLA 1.4 GHz

(Tashiro et al. 2001)

Radio Galaxies in the Chandra Era

what we have to do next

102

103

104

103

104

105

Lorents factor ge

What we have to do next

Spectral Energy Distribution

(Isobe et al. 2006)

  • The Lorents factor of radio electrons is larger than that of X-ray ones
  • It is important to detect radio/X-ray emission from electrons with the same Lorentz factor.
  • 2 options
    • low-frequency radio
    • Hard X-ray
  • Low-frequency radio observation is difficult.
  • Hard X-ray observation with Suzaku is the ideal tool.

Radio Galaxies in the Chandra Era

the x ray observatory suzaku
The X-ray Observatory Suzaku

Suzaku

  • The 5th Japanese X-ray satellite, launched July 10, 2005. (about 3 years old.)
  • 2 X-ray detectors
    • XIS (X-ray Imaging Spectrometer)
      • 3 CCD cameras active

1 BI CCD (XIS1)

2 FI CCD (XIS0, 3)

      • 0.2 – 10 keV
      • Low background
      • Good energy resolution
    • HXD (Hard X-ray Detector)
      • Si-PIN diode

: 10 – 60 keV

      • GSO scintillator

: 60 – 300 keV

      • Wide energy band
      • low background

HXD

XIS

Radio Galaxies in the Chandra Era

suzaku observation of fornax a

HXD/PIN FoV

(FWHM)

Suzaku observation of Fornax A

XIS 0.5 – 10 keV

VLA 1.4 GHz (Fomalont et l 1989)

2 Suzaku exposures : Host Galaxy (40 ks) and West Lobe (80 ks)

Radio Galaxies in the Chandra Era

suzaku hxd pin spectrum
Suzaku HXD/PIN Spectrum

Comparison with Data & NXB

Comparison with Data & CXB

Data

NXB (Tuned)

NXB-Subtracted

NXB-Subtracted

CXB

(Boldt 1987)

2% of NXB

Hard X-ray signals from the west lobe

are significant up to 20 keV.

Radio Galaxies in the Chandra Era

wide band x ray spectrum of the west lobe
Wide-band X-ray spectrum of the west lobe

PL component

G = 1.82 ±0.22

S1keV = 137 -29 +32 nJy

0.2 keV

0.8 keV

Radio Galaxies in the Chandra Era

spectral energy distribution

ge =

4200

ge =

4200

Spectral Energy Distribution

GR= 1.68 ± 0.05

GX= 1.82 ± 0.22

Spectrum of the radio electrons is

connected to that of IC X-ray electrons

Radio Galaxies in the Chandra Era

physical quantities in lobes
Physical quantities in lobes

West Lobe

(Suzaku, This Work )

East Lobe

(XMM-Newton, Isobe et al. 2006)

R (arcmin)

(kpc)

S1.4GHz (Jy)

GR

GX

S1keV (nJy)

10

54.1

44 ±5.9

1.68 ± 0.05

1.62 -0.15 +0.24

90 +8 -9

12

64.9

74 ± 7.7

1.68 ± 0.05

1.82 ± 0.22

137 -29 +32

1.55

1.23 ± 0.07

0.61 ± 0.07

3.0 ± 0.3

5.0 ± 1.0

1.59

1.4 ± 0.1

0.78 ± 0.10

2.36 ± 0.25

3.0 ± 0.7

Bme (mG)

BIC (mG)

uB (10-13 erg cm-3)

ue (10-13 erg cm-3)

ue/um

Radio Galaxies in the Chandra Era

future perspective

103

104

105

GLAST Sensitivity

(5 s / 1year)

Cheung et al. 2006

Sambruna @ 1st GLAST Symp.

NeXT SXI/HXT

Future perspective

Radio Galaxies in the Chandra Era

summary
Summary
  • IC X-ray emission was detected up to 20 keV from the west lobe of Fornax A, with Suzaku HXD.
  • The X-ray spectrum of the west lobe is described with a PL model with G = 1.82±0.22 and S1keV = 137-29+34 nJy.
  • A comparison between the radio and X-ray fluxes gives B = 1.4±0.1 mG, which is slightly smaller than the minimum energy field Bme = 1.59 mG.
  • The X-ray photons of 20 keV corresponds to the electron Lorents factor of ge~ 5000. As a result, we have succeeded in connecting the electron spectra of synchrotron and IC emitting electrons.

Radio Galaxies in the Chandra Era

references
References
  • Kaneda et al. 1995 ApJ 453, L13
  • Iyomoto et al. 1998 ApJ 503, L31
  • Tashiro et al. 2001 ApJ 546, L19
  • Isobe et al. 2006 ApJ 645, 256

Radio Galaxies in the Chandra Era