japanese historical records of snrs and suzaku observation of sn1006 2006/05/16 one millennium after...
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Japanese historical records of SNRs and SUZAKU observation
of SN10062006/05/16 One Millennium after SN 1006? @Hangzhou
Hiroya Yamaguchi (Kyoto Univ., Japan) Katsuji Koyama (Kyoto Univ.)
Junko Hiraga (RIKEN),
Aya Bamba (RIKEN)
国宝「明月記」(冷泉家時雨亭文庫)
My talk plan
• The Japanese historical records of SN1006 and other supernova remnants.
• Introduction of Japanese satellite “Suzaku”.
• Report of the Suzaku observation of SN1006.
• Summary
Historical record of SNRs
Astronomical records (auroras, eclipse, shooting star and etc.)were frequently appeared after 7th century.
The exchange between China and Japan was very active.
煬帝 Yang Di
聖徳太子 Shotoku-taishi(assistance of emperor)
遣隋使 (Kenzuishi)The mission to China
Astronomical knowledge and thought
Ancient China and Japan
In 12-13th century, Teika Fujiwara (Japanese noble and poet) collected the ancient astronomical records, and noted them in his diary “Meigetsuki (明月記)” .
藤原定家 Teika Fujiwara (1162-1241)
He started to write the diary when he was 19 years old, and continued for 56 years.
In those days, diaries had the role of the records of the ceremony, political affairs, and disasters.
Unusual astronomical phenomena (supernovae, eclipses, comets, and shooting stars) were believed as the predictions of famines, epidemics, and floods.
Japanese historical record of SNR“Meigetsuki” (This page was written in 11/8, 1230.)
「客星古現例」the ancient samples of “guest stars”.
Guest stars = comets, novae, and supernovae
8 7 6 5 4 3 2 1
SN10063C58
Crab Nebula
SN1006
Chandra image of SN1006
一條院 寛弘三年 四月二日 葵酉 夜以降 騎官中 有大客星 如螢惑 光明動耀 連夜正見南方 或云 騎陣将軍星本体 増変光
In the reign-period of Ichijo-In, April 2nd, 3rd year of Kanko (= May 1st, 1006), a great guest star appeared within
the constellation “Kikan” (=Imperial Guards). It was very bright like Mars, and visible in the southern sky every night. One possibility was the star of “Kijin-Shogun” (= Chariots and General) suddenly lighten?
騎陣将軍 (Kijin-Shogun) Lupusκ
騎官 (kikan)
Crab nebula
Chandra image of Crab
後冷泉院 天喜二年 四月中旬以降 丑時 客星觜参度 見東方 孛天関星 大如歳星
In the reign-period of Goreizei-In, after the middle of April, 2nd year of Tenki (= May-June, 1054), a guest star appeared
nearby “Shi” and “Shin” (= Orion) in eastern sky at 2:00. It shined near to the star of “Tenkan”, and its size was comparable to Jupiter.
觜 , 参 = Orion
天関 (Tenkan)Taurusζ
3C58
Chandra image of 3C58
高倉院 治承五年 六月廿五日 庚午 戌時 客星見北方 近王良 守伝舎星
In the reign-period of Takakura-In, June 25th, 5th year of Jisyou (= August 7th, 1181), a guest star appeared in northern sky at 20:00. It was near to the star of “Oh-Ryo” (= real person’s name of ancient China) and “Densya”.
王良 (Oh-Ryo)Cassiopeiaβ
伝舎 (Densya) = Camelopardalis
Kyoto Gyoen
Reizei-ke
Kamo river
Kyoto Univ.
Very near ! (~ 2km)
“Meigetsuki” was designated as a national treasure in 2000.
It is preserved by Reizei-ke (冷泉家) , descendant of Teika Fujiwara.
Introduction of Suzaku
Introduction of SuzakuThe 5th Japanese X-ray astronomical satellite.
It was launched on July 10th 2005.
Suzaku is “Red Chinese Phoenix”, the protector God of the South. The wall painting of Suzaku
in “Kitora” tomb
朱雀 (Suzaku)
Instrument
XRT (X-Ray Telescope)Large effective area 450cm2 @1.5keV per 1 unit
XIS (X-ray Imaging Spectrometer)Improved X-ray CCD with high efficiency
and good energy resolutionLow BackgroundEnergy band : 0.2-12keV
HXD (Hard X-ray Detector)Wide energy band Si-PIN (8-50keV) & Scintillator (50-600keV)Non-imaging detector, but low background
XRT
XIS
HXD
XIS4 units3 Front-illuminated (FI) CCD high efficiency for hard X-ray‥1 Back-illuminated (BI) CCD high efficiency for soft X-ray‥
XRT
SensorAE/TCE
to DP
MPU
PPU
PPU
Bonnet
Base
DE
XRT
XIS
FI CCDBI CCD
Quantum Efficiency of XIS
Suzaku XIS-FISuzaku XIS-BI
Spectra of E0102-72
XIS
O VII
O VIII
Ne IX
Ne X
Comparison of efficiency and energy resolutions
XISComparison of background levels
BGD spectra normalized by solid angle of FOV and effective area
Suzaku XIS-FISuzaku XIS-BIXMM EPIC-MOSXMM EPIC-pn
Suzaku observationof SN1006
Cosmic ray acceleratorKoyama et al. (1995) discovered synchrotron X-ray from the shell of SN1006.
→ Indication of ~ 100TeV electrons
SNRs are cosmic ray accelerator !
Unsolved problem The environment of accelerating place ‥ Plasma temperature, density, and so on. Essential information to understand the acceleration mechanism.
Temperature 0.1 - 1 keV‥ We don’t know accurate value, Density 0.1 - 10 cm‥ -3 nor positional dependence.
Suzaku XIS-BI (high efficiency and good energy resolution) is the best instrument to resolve this problem !
ASCA image of SN1006
10’
Thermal X-ray from SNRsWe can get the information of temperature and density
from thermal X-ray spectrum of SNR !
Shock front of SNR heats the matter up to a temperature of a few keV ( ~ 107 K), and emits X-rays (bremsstrahlung and line emissions).
Electron temperature the shape of the bremsstrahlung continuum‥Density the flux of the continuum and the line emissions‥
Brems: I(ν) (hν)∝ -0.4 exp(-hν/kTe) ・ nenpVLine: Iz n∝ enzV
ne = electron density, np = proton densitynz = ion density, V = volume of emission region
Thermal X-ray from SNRs
He-like ion H-like ion
IonizationHe-like H-like Fully ionized
1 10 100 103 104
Electron temperature (eV)
Oxygen ionization fraction vs. electron temp.
Non-equilibrium ionization (NEI)
At low density, Te ≠ Tz
Ionization equilibrium requires ~ 103 years !
He-like H-like Fully ionized
106 107 108 109 1010 1011 1012
net (cm-3 s)
Oxygen ionization fraction vs. net (for kTe=1.5keV)
Higher temperatureHigher density Higher ionized state
Neutral
Neutral
XIS image of SN1006
XIS-BI 0.3 - 5.5 keV image
43.5ksec
62.4ksec
59.1ksec 61.6ksec
Suzaku observed SN1006 by 6pointing on 2005/9 and 2006/2.
4 pointing on source2 pointing for background
Extract spectrum from whole northeast region.
Spectra of whole NE region
Black : XIS-BIRed : average of 3 XIS-FIs
He-O
H-O
Non-thermal emission
Successfully divided oxygen lines and synchrotron component !
He-O band
3 - 5 keV band
Narrow band images of XIS-BI
He-O line band 3 - 5 keV band
Distributions of thermal plasma (line emission) and non-thermal electron (synchrotron emission) are different !
Narrow band images of XIS-BI
He-O line band 3 - 5 keV band
NE rim of SN1006
Easthern rim emits X-rays in the He-O band (soft thermal X-rays), and northern rim emits hard X-rays ??
Spectral analysis of NE regionWe divided NE region into 8x8 region, and extracted spectra from each square region.
Northern rim
Eastern rim
Inner region
Compared the fluxes of O lines and 3-5keV band.
Used region: in the YELLOW frame
He-O line vs. hard X-ray emission
Northern rim
Eastern rim
Inner region Consistent with imaging analysis !
H-O line vs. hard X-ray emission
Northern rim
Eastern rim
Inner region
Similar distribution to He-O vs. hard X-ray
Northern rim
Eastern rim
These regions are correspond to 2 Chandra filaments in NE shell.
Chandra image with Suzaku FOV.
Northern rim
Eastern rim
The first result: We distinguished the spectral properties of two filaments !
Chandra image of SN1006
Inner region
More detailed analysis and discussion
He-O
H-O
Northern rim
Eastern rimInner region
Black: NH=1x1021cm-2
Red: NH=2x1021cm-2
Blue: NH=3x1021cm-2
H-O/He-O ~ 0.2 in all regions !
High Temp.
Hig
h D
ens
ity
kTe vs. net (for H-O/He-O=0.2)
Line intensity: Eastern rim > Northern rim→ Density: Eastern rim > Northern rim
H-O/He-O ratio: Eastern rim = Northern rim→ Temperature: Eastern rim < Northern rim
More detailed analysis and discussion
Black: Northern rimRed: Eastern rim
Γ ~ 2.7
Γ ~ 3.1
Higher energy electrons exist in Northern rim ?
Emax ∝ V ρ∝ -1/5
Low density → High shock speed→ High acceleration efficiency
Non-thermal emission
Future workQuantitative decision of temperature, density, and maximum energy of accelerated electrons by spectral fitting with precise response of XIS.
Summary
• We observed SN1006 with Suzaku.
• We succeed to divide two oxygen lines from continuum spectrum.
• We discovered positional dependence of line intensities in the NE region of SN1006.
• E rim = High density and low temperature, N rim = low density and high temperature?
HXDComparison of background levelsBGD spectra normalized by effective area
1Crab
RXTE-PCA/HEXTEBeppoSAX-PDS
Suzaku HXD-PIN/GSO
Energy (keV)10 100 500
Cou
nts
sec-1
keV
-1 c
m-2
Discussions
Density of ISM ? ‥ Line intensity ρ∝ 2
‥ Radius ρ∝ -1/3
rnorth > reast (Rothenflug et al. 2004)
Line Non-thermalNorth rim weak intense hardEast rim intense intense softInner region middle weak
VLA (1518MHz)image of SN1006