1. Japanese historical records of SNRs and SUZAKU observation of SN1006 2006/05/16 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）

2. 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

3. Historical record of SNRs

4. 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

5. 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.

6. 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 SN1006 3C58 Crab Nebula

7. 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)

8. 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

9. 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

10. 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.

11. Introduction of Suzaku

12. The 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)

13. Instrument XRT (X-Ray Telescope) Large effective area 450cm 2 @1.5keV per 1 unit XIS (X-ray Imaging Spectrometer) Improved X-ray CCD with high efficiency and good energy resolution Low Background Energy 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

14. XIS 4 units 3 Front-illuminated (FI) CCD ‥ high efficiency for hard X-ray 1 Back-illuminated (BI) CCD ‥ high efficiency for soft X-ray XRT XIS FI CCD BI CCD Quantum Efficiency of XIS

15. Suzaku XIS-FI Suzaku XIS-BI Spectra of E0102-72 XIS O VII O VIII Ne IX Ne X Comparison of efficiency and energy resolutions

16. XIS Comparison of background levels BGD spectra normalized by solid angle of FOV and effective area Suzaku XIS-FI Suzaku XIS-BI XMM EPIC-MOS XMM EPIC-pn

17. Suzaku observation of SN1006

18. Cosmic ray accelerator Koyama 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’

19. Thermal X-ray from SNRs We 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 ( ～ 10 7 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/kT e ) ・ n e n p V Line: I z ∝ n e n z V n e = electron density,n p = proton density n z = ion density, V = volume of emission region

20. Thermal X-ray from SNRs He-like ion H-like ion Ionization He-like H-like Fully ionized 1 10 100 10 3 10 4 Electron temperature (eV) Oxygen ionization fraction vs. electron temp. Non-equilibrium ionization (NEI) At low density, T e ≠ T z Ionization equilibrium requires ～ 10 3 years ! He-like H-like Fully ionized 10 6 10 7 10 8 10 9 10 10 10 11 10 12 n e t (cm -3 s) Oxygen ionization fraction vs. n e t (for kT e =1.5keV) Higher temperature Higher density Higher ionized state Neutral

21. 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 source 2 pointing for background Extract spectrum from whole northeast region.

22. Spectra of whole NE region Black : XIS-BI Red : 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

23. 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 !

24. 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 ??

25. Spectral analysis of NE region We 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

26. He-O line vs. hard X-ray emission Northern rim Eastern rim Inner region Consistent with imaging analysis !

27. H-O line vs. hard X-ray emission Northern rim Eastern rim Inner region Similar distribution to He-O vs. hard X-ray

28. 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

29. More detailed analysis and discussion He-O H-O Northern rim Eastern rim Inner region Black: N H =1x10 21 cm -2 Red: N H =2x10 21 cm -2 Blue: N H =3x10 21 cm -2 H-O/He-O ～ 0.2 in all regions ! High Temp. High Density kT e vs. n e t (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

30. More detailed analysis and discussion Black: Northern rim Red: Eastern rim Γ ～ 2.7 Γ ～ 3.1 Higher energy electrons exist in Northern rim ? E max ∝ V ∝ ρ -1/5 Low density → High shock speed → High acceleration efficiency Non-thermal emission Future work Quantitative decision of temperature, density, and maximum energy of accelerated electrons by spectral fitting with precise response of XIS.

31. 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?

33. HXD Comparison of background levels BGD spectra normalized by effective area 1Crab RXTE-PCA/HEXTE BeppoSAX-PDS Suzaku HXD-PIN/GSO Energy (keV) 10 100 500 Counts sec -1 keV -1 cm -2

34. Discussions Density of ISM ? ‥ Line intensity ∝ ρ 2 ‥ Radius ∝ ρ -1/3 r north > r east (Rothenflug et al. 2004) Line Non-thermal North rim weak intense hard East rim intense intense soft Inner region middle weak VLA (1518MHz) image of SN1006