radio galaxy elliptical fanaroff-riley type i “misaligned” bl lac (~ 60 ) distance 3.5 mpc...
TRANSCRIPT
Radio galaxyEllipticalFanaroff-Riley type I“Misaligned” BL Lac (~ 60)Distance 3.5 Mpc
Parameter Value
(J2000) 201.3650633
(J2000) -43.0191125
Galaxy Size 18 14 arcmin
Radio Source size 8 4 degrees
Distance 3.5 Mpc
Apparent Magnitude 7.96 mag
Total galaxy mass (41) 1011 M
Outer radio lobe 250 kpc
Inner radio lobe 5 kpc
Inner radio jet 1.35 kpc
Relativistic nuclear jet 1.65 pc
Radio core 0.008 pc
Dust lane radius 7 kpc
Optical image of Centaurus A (ESO/MPG 2.2-m telescope with WFI)
Outer lobes (408MHz) (20o20o, Haslman 1982 )
Outer lobes 6.9cm(4.75GHz) (5o9o, Junkes 1993)
Blue : Radio jetRed : COWhite : Atomic hydrogen gasYellow : shell(32’ 32’, Charmandaris 2000)
30 kpc ~ 0.3
Image size = 15 14 arcmin
RadioVLA(6cm)4.9GHz
Far infraredIRAS60-100m
Mid infraredSpitzer3.6 to 8m
VisibleDSS405-645nm
Near infrared2MASS1.2-2.17m
UltravioletGALEX130-300nm
Gamma
CANGAROO-III Angular resolution
X-rayChandra1-3 keV
0.25o
Oneeventresolution
10% of galaxies AGN
AGN - Time variation (1000sec) - It is 100 or more times brighter than the stars of the whole galaxy. - A massive black hole (MBH) as its nuclei
10% of AGN Jet (Blazar)
Jet - Super luminal motion - Radio lobe - Hot spot - Knot
Unified model of AGN
Cen A 60°
• Double-peaked structure= synchrotron + inverse Compton(Synchrotron Self-Compton model)
HBL
LBL
1~IC
sync
L
L
ray
Same cut as Crab ( L > 0.9 ) 2 distribution
Integral Flux 2- upper limit
7% Crab FluxOur flux limit is 10 times lower than previous results.
Possibility on HBL assumption
1~/
10~/ 8
sc
sc
LL
1580/1/ sc LL
Typical AGN model
But Cen A…
syncsync
B
sync
sync
ssc
UcRL
U
U
L
L
424
1
2
)12/(250
8/1
/3500580
/6~
2.0~
12
kpcRGB
BU
cceVUU
cceVU
kpcR
B
syncB
sync
IC peak
Synchrotron peak
Rad
io
Infr
ared
/ o p
t ica l X r
ay
Gam
ma
( MeV
) Gam
ma
( Te V
)
Relativistic beaming effect
Bai estimation
CANGAROO-III
Bai, J.M. et al 1999F(0.25-30TeV) = 6.410-9 erg cm-2 s-1 : BaiF(>530GeV) = 2.610-12 erg cm-2 s-1 : CANGAROO-III
The day-by-day results of Cen A observation
We cannot find any sign of bursts.
)/(
1)4/(3
22
MEd
d
M
dVvB
dE
dF
h
CDMqq
2nBv qq
The annihilation rate of the CDM can be written as
MdE
d
h /
1
The accelerator measurement on thefragmentation function
is limited to lower energy of such as 100 MeV. The gamma-ray flux is written
Cen A → Giant Galaxy 3.5 Mpc
Search for Gamma-rays from the Active radio galaxy Centaurus A with CAN
GAROO-III telescopes
We have observed the giant radio galaxy Centaurus A (Cen A) in the TeV energy region using the CANGAROOIIIstereoscopic system. The system has been in operation since 2004 and is an array of four Imaging Atmospheric
Cherenkov Telescopes (IACT) with about a 100 m spacing. The observations were carried out betweenMarch and April 2004. In total 20-hour data were obtained. No statistically significant gamma-ray signal has
been found above 530 GeV and we obtain an integral flux upper limit of 3.2 10-12 cm-2 sec-1 (2- level).This upper limit is less than 7 % of the gamma-ray flux from the Crab nebula. Although some groups reporteddetections of Cen A in the past, we give upper limits more than one-order of magnitude lower for this object.
S. Kabuki(a), R. Enomoto(b), M. Mori(b) and CANGAROO collaborators (a) Department of Physics, Graduate School of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan
(b) Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
Radio images of Centaurus A
Multiwavelength images of Centaurus A
Active Galactic Nuclei (AGN)
Synchrotron self-Compton model
Result of Analysis
Estimation of Flux (burst)
Upper limit on density of CDM
In this paper, we showed the result of the first stereoscopic observation ofCen A with CANGAROO-III telescopes. The observation period was from March 16 to April 19 2004 and the total observation time was 1197 min. We could not detect a TeV gamma-ray signal and the 2- upper limit was obtained to be 3.210-12 cm-2 sec-1 at energies greater than 530 GeV. This 2- upper limit corresponds to be approximately 7 %-Crab flux. This is an order of magnitude lower than past results. We derived physical parameters for an HBL model using our upper limits and multi-wavelength spectra. Assuming a volume of the emission region to be that defined by our angular resolution, we obtained a limit on the magneticfield: B > 210 G (R/12 kpc)-1. Even using a size of an order of a light year, it exceeds one Gauss, a situation which can be hardly understood. We conclude that Cen A is not classified as a normal HBL.
Conclusions
Blazar ~ 1/ ~ ~10
cos
Define beaming factor
The flux can be written as Fobs = 2+αF = p F.If we see Mrk501 at 60 degrees inclination like Cen A,with typical values, ~5 and p~3, the flux changes by p = 1.3×10-4 .If we assume Mrk501 is at the same distance of Cen A, (F Mrk501/F CenA)2 = (z Mrk501/z Cen A)2 = (0.034/0.0008)2 = 1.8104 Thus, even if its inclination is 60 degrees like Cen A, the gamma-ray signal could be detected.
The gamma-ray signal was undetectable. The problem of the inclination of the jet?
H.E.S.S. limit (Aharonian et al, 2005)
.