169 8555 3 4 1 e-mail: kataoka.jun@waseda.jp 606 8502 e-mail: totani@kuastro.kyoto-u.ac.jp 305 0801 1 1 e-mail: kunihito.ioka@kek.jp 50 5 X 1 10 10 2008 3 2,000 542 2012 9
5 2. 1 3 E 1 GeV E 10 GeV 1 2, 3 4 5 6 X 7 8 9 2 2 X 3 4 2.1 10, 11 3 1 1 GeV 10 GeV 1 GeV 10 9 10 GeV π 8 9 8 2 1.6 105 9 543
2 11 1.6 1 GeV E 2 GeV 2 GeV E 5 GeV 5 GeV E 10 GeV 10 GeV E 20 GeV 1 2 GeV, 2 5 GeV, 5 10 GeV, 10 20 GeV 11 10, 11 2.2 2 50, 20 5 dn/de E Γ Γ 2.0 1GeV 11 4 6 3 11 2 544 2012 9
3 1 5 GeV 11 a: b: A B A a C A a b 2.3 X 3 WMAP haze X North Polar Spur NPS WMAP haze WMAP Haze 2009 Planck 4 Planck NASA web 12 10 GeV ROSAT 1.5 kev X NASA 12 4 WMAP haze WMAP haze 12 X 1990 ROSAT 2 kev X X NPS Northern 105 9 545
Arc X X NPS 3. 3.1 11 X kt 2 kev 2,000 10 2 cm 3 3 10 54 55 erg km 10 7 5 3.2 30 1984 13 200 pc Galactic Center Lobe; GCL Bland-Hawthon 14 10 55 erg 1972 15 Scoville 16 Expanding Molecular Ring; EMR GCL 17 Bland-Hawthon 14 1 NPS 10 7 10 56 erg NPS 18 546 2012 9
5 24 3 NPS 30 30 Sgr A* 1996 19 X Sgr A* 300 Sgr B2 X X 300 Sgr A* 10 39 erg/s X Sgr A* X 10 100 20 21 105 9 547
3.3 400 Sgr A* X 300 10 6 10 55 erg 10 49 erg/ 1 M s / M s 22 0.1 M s / 1 Hα M82 Sgr A* Sgr A* RIAF radiatively inefficient accretion flow; 23 24 Sgr A* 1,000 1,000 10 49 erg/ X 10 100 X RIAF X 2 511 kev 511 kev Hα Sgr A* Sgr A* 1,000 Sgr A* Sgr A* Sgr A* Sgr A East 24 4. 4.1 548 2012 9
6 11 11 2 2 10 3.1 1 γ 2.0 2.5 6 1 GeV 25 WMAP haze 2 μg WMAP haze WMAP 6 γ 2.0 2.5 11 1 GeV 10 26 TeV 10 12 ev 105 9 549
TeV TeV CTA 5 4.2 27 π WMAP haze π 3.1 10 10 2 cm 3 π 140 MeV TeV CTA π IceCube 100 TeV 28 CTA 100 29 10 15 ev knee 10 18 ev ankle knee ankle IceCube 4.3 2 550 2012 9
2 26, 29 29 30 4.3 10 Cen A 200 31, 3 X 32 5. 3 3 1970 X 2 kev 2 X MAXI 2009 105 9 551
X CCD SSC GSC 0.5 kev 30 kev MAXI 2005 5 X 0.4 600 kev 7 8 6 2 kev X NPS X 2014 Astro-H 0.3 600 kev X X 10 kev X Hard X-ray Imager CTA Cherenkov Telescope Array CTA TeV 1 20 GeV 100 TeV 1,000 TeV 2 10 GeV CTA Meng Su 552 2012 9
12002 95, 373 2 2005 98, 680 3 Lukasz Stawarz, 2010 103, 486 4 2010 103, 374 5 2010 103, 438 62010 103, 324 72010 103, 430 8 2010 103, 366 9 2010 103, 494 10 Dobler G., et al., 2010, ApJ 717, 825 11 Su M., et al., 2010. ApJ 724, 1044 12 http://www.nasa.gov/mission_pages/planck/news/ planck20120213.html 13 Sofue Y., and Handa T., 1984, Nature 310, 568 14 Bland-Hawthorn J., Cohen M., 2003. ApJ 582, 246 15 Kaifu N., Kato T., Iguchi T., 1972, Nature 238, 105 16 Scoville N. Z., 1972, ApJ 175, L127 17 Sofue Y. 2000, ApJ 540, 224 18 2006 99, 582 19 Koyama K., et al., 1996, PASJ 48, 249 20 Murakami H., et al., 2000, ApJ 534, 283 21 Nobukawa M., Ryu S. G., Tsuru T. G., Koyama K., 2011, ApJ 739, L52 22 Matsunaga N., et al., Nature 477, 188 23 Narayan R., McClintock J. E., 2005, ApJ 623, 1017 24 Totani T., 2006, PASJ 58. 965 25 Chang J. et al., 2008, Nature 456, 362 26 Cheng K. S., et al., 2011, ApJ 731, L17 27 Crocker R. M., Aharonian F., 2011, Phys. Rev. Lett. 106, 101102 28 Lunardini C., Razzaque S., 2011, Phys. Rev. Lett. 108, 221102 29 Cheng K. S., et al., 2012. ApJ 746, 116 30 Mertsch P., Sarkar S., 2011, Phys. Rev. Lett. 107, 091101 31 Abdo A., et al., 2010, Science 328, 725 32 Pakull M. W., Soria R., Motch C., 2010, Nature 466, 209 Giant Gamma-Ray Bubbles Discovered with Fermi-LAT: Probing the Past Activity of Our Galactic Center Jun Kataoka Research Institute for Science and Engineering, Waseda University, 3 4 1 Okubo, Shinjuku-ku, Tokyo 169 8555, Japan Tomonori Totani Department of Astronomy, School of Science, Kyoto University, Sakyo-ku, Kyoto 606 8502, Japan Kunihito Ioka KEK Theory Center and the Graduate University for Advanced Studies, Oho, Tsukuba 305 0801, Japan Abstract: Fermi-LAT has discovered two giant gamma-ray bubbles, extending over 50 degrees above and below the Galactic center GC. The morphology is spatially correlated with WMAP haze, and the edges of the bubbles also line up with North Polar Spur in the ROSAT X-ray maps. We discuss possible episode of creating such giant bubbles with energy injection of the GC in the past. A very hard gamma-ray spectrum suggests these bubbles are likely site of high energy cosmic-ray acceleration. 105 9 553