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すざくによる高銀緯 フェルミ未同定天体の X 線探査 (submitted to ApJ)

すざくによる高銀緯 フェルミ未同定天体の X 線探査 (submitted to ApJ). 2010/09/24 　日本天文学会　 2010 年　秋季年会　 @ 金沢大学. 前田洸登 （早大理工）. 片岡淳，中森健之（早大），真喜屋龍，戸谷友則（京大） 金井義和，河合誠之（東工大）， Lukasz Stawarz ，田中康之， 佐藤理江，高橋忠幸（ ISAS/JAXA ）， C. Cheung （ NASA/GSFC ）， D. Donato ， N. Gehrels （ CRESST ）， P. Saz Parkinson （ SCIPP ）. （ 271 sources ）.

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すざくによる高銀緯 フェルミ未同定天体の X 線探査 (submitted to ApJ)

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  1. すざくによる高銀緯フェルミ未同定天体のX線探査(submitted to ApJ) 2010/09/24　日本天文学会　2010年　秋季年会　@金沢大学 前田洸登 （早大理工） 片岡淳，中森健之（早大），真喜屋龍，戸谷友則（京大） 金井義和，河合誠之（東工大），Lukasz Stawarz，田中康之，佐藤理江，高橋忠幸（ISAS/JAXA），C. Cheung（NASA/GSFC），D. Donato，N. Gehrels（CRESST），P. Saz Parkinson（SCIPP）

  2. （271 sources） EGRET All-Sky Gamma-Ray Survey ( > 100MeV)Credit: EGRET team ●UnID : 170 sources CGRO/EGRET all-sky g-ray Survey

  3. 640 out of 1451 sources are still UnID

  4. Motivation of Suzaku observation • To survey a new-type g-ray source • Bright in the long term, but still unID • Extragalactic, but Not AGN • Source selection (3 months Fermi obs.) • BrightunID source (EGRET and 0FGL) • At high Galactic latitude (|b| > 10 [deg]) • No temporal variability

  5. Observed UnID Fermi/LAT Object 1FGL J1231.1-1410 1FGL J1311.7-3429 1FGL J1333.2+5056 |b|=10 [deg] 1FGL J2017.3+0603 Fermi/LAT Gamma-ray Image of 1-year Observation (100MeV - 300GeV)Credit: NASA/DOE/Fermi LAT Collaboration

  6. 1FGL J1231.1-1410 1FGL J1311.7-3429 Results of Suzaku Follow-up Observation 1FGL J1333.2+5056 1FGL J2017.3+0603 - Too much complicated- Run off the edge of FOV

  7. 1FGL J1231.1-1410 X-ray Image PSRJ1231-1411(P=3.68ms,d=0.4kpc) Dec.[deg] Suzaku XIS0+3 (0.4 - 10 keV)(NXB subtracted, exposure & vignetting corrected) • Brightest g-ray source of 4 unIDs • EGRET unID • (Radio) MSP PSRJ1231-1411 • Ransom et al. 2010 • X-ray position is consistent with g-ray & radio position R.A.[deg]

  8. X-ray Spectrum Analysis(Black:XIS0+3,Red:XIS1) Residuals remain(> 2 keV) improved wabs * blackbody wabs ( blackbody + powerlaw ) NH=0 consistent NH=0 consistent Γ ~ 1.8 kT ~ 0.16 keV Additional PL component is necessary! (significance level >99%)

  9. 1FGL J1231.1-1410nFn multi-wavelength SED Multi-wavelength SED of Geminga pulsarCredit:: D. J. Thompson (2004) Bright g-ray flux & blackbody + PL is similar to the spectral structure of Geminga pulsar

  10. 1FGL J1311.7-3429 X-ray Image (a) src A X-ray flare factor 10 20 ks • EGRET unID • Two X-ray sources Dec.[deg] (b) src B steady flux Suzaku XIS0+3 (0.4 - 10 keV)(NXB subtracted, exposure & vignetting corrected) R.A.[deg]

  11. 1FGL J1311.7-3429nFn multi-wavelength SED ? QHB (QSO Hosted Blazar) ?! No pulse detection (g-ray, radio)Remain uncertain (not typical blazar)

  12. 1FGL J2017.3+0603 X-ray Image Fermi unID (Radio) MSP PSR J2017+0603: Cognard et al. 2010 (P=2.9ms) g-ray pulsation CLASS J2017+0603:(z=1.74 blazar) Dec.[deg] Suzaku XIS0+3 (0.4 - 10 keV) (NXB subtracted, exposure & vignetting corrected) R.A.[deg]

  13. 1FGL J2017.3+0603nFn multi-wavelength SED CLASS J2017+0603 PSR J2017+0603

  14. Summary • Our Suzaku observation findings • 1FGL J1231.1-1410 : newly detected PL component of MSP • 1FGL J1311.7-3429 : detected variable X-ray source but still uncertain (QHB blazar?) • 1FGL J2017.3+0603 : only detected a blazar and not a pulsar in X-ray (give a pulsar upper-limit) • 1FGL J1333.2+5056 : too much complicated due to large localization error

  15. Next X-ray observations (AO-5) Coming Soon!

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