THE SPECTRUM AND MORPHOLOGY OF THE FERMI BUBBLES

被引：240

作者：

Ackermann, M. ^{[1
]}

Albert, A. ^{[2
,3
]}

Atwood, W. B. ^{[4
,5
]}

Baldini, L. ^{[6
]}

Ballet, J. ^{[7
]}

Barbiellini, G. ^{[8
,9
]}

Bastieri, D. ^{[10
,11
]}

Bellazzini, R. ^{[6
]}

Bissaldi, E. ^{[12
,13
]}

Blandford, R. D. ^{[2
,3
]}

Bloom, E. D. ^{[2
,3
]}

Bottacini, E. ^{[2
,3
]}

Brandt, T. J. ^{[14
]}

Bregeon, J. ^{[15
]}

Bruel, P. ^{[16
]}

Buehler, R. ^{[1
]}

Buson, S. ^{[10
,11
]}

Caliandro, G. A. ^{[2
,3
,17
]}

Cameron, R. A. ^{[2
,3
]}

Caragiulo, M. ^{[18
]}

Caraveo, P. A. ^{[19
]}

Cavazzuti, E. ^{[20
]}

Cecchi, C. ^{[21
,22
]}

Charles, E. ^{[2
,3
]}

Chekhtman, A. ^{[23
]}

Chiang, J. ^{[2
,3
]}

Chiaro, G. ^{[11
]}

Ciprini, S. ^{[20
,24
]}

Claus, R. ^{[2
,3
]}

Cohen-Tanugi, J.

Conrad, J. ^{[25
,26
,27
]}

Cutini, S. ^{[20
]}

D'Ammando, F. ^{[28
,29
]}

de Angelis, A. ^{[30
,31
]}

de Palma, F. ^{[18
]}

Dermer, C. D. ^{[32
]}

Digel, S. W.

Di Venere, L. ^{[33
]}

do Couto e Silva, E. ^{[3
]}

Drell, P. S. ^{[2
,3
]}

Favuzzi, C. ^{[33
]}

Ferrara, E. C. ^{[14
]}

Focke, W. B. ^{[2
,3
]}

Franckowiak, A. ^{[2
,3
]}

Fukazawa, Y. ^{[34
]}

Funk, S. ^{[2
,3
]}

Fusco, P. ^{[18
,33
]}

Gargano, F. ^{[18
]}

Gasparrini, D. ^{[20
,24
]}

Germani, S. ^{[21
,22
]}

机构：

[1] DESY, D-15738 Zeuthen, Germany

[2] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA

[3] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA

[4] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA

[5] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA

[6] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy

[7] Univ Paris Diderot, CNRS, CEA Saclay, CEA IRFU,Lab AIM,Serv Astrophys, F-91191 Gif Sur Yvette, France

[8] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy

[9] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy

[10] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

[11] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy

[12] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy

[13] Univ Trieste, I-34127 Trieste, Italy

[14] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[15] Univ Montpellier 2, IN2P3, CNRS, Lab Univ & Particules Montpellier, Montpellier, France

[16] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France

[17] CIFS, I-10133 Turin, Italy

[18] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy

[19] INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy

[20] ASI, Sci Data Ctr, I-00133 Rome, Italy

[21] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy

[22] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy

[23] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA

[24] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Roma, Italy

[25] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden

[26] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden

[27] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden

[28] INAF, Ist Radioastron, I-40129 Bologna, Italy

[29] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy

[30] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy

[31] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy

[32] Div Space Sci, Naval Res Lab, Washington, DC 20375 USA

[33] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy

[34] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan

[35] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy

[36] Pontificia Univ Catolica Chile, Dipartimento Fis, Santiago, Chile

[37] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria

[38] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria

[39] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA

[40] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA

[41] CRESST, Greenbelt, MD 20771 USA

[42] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[43] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France

[44] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland

[45] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan

[46] CNRS, IRAP, F-31028 Toulouse 4, France

[47] Univ Toulouse, IRAP, UPS OMP, GAHEC, Toulouse, France

[48] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden

[49] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy

[50] Yale Univ, Dept Phys, Dept Astron, New Haven, CT 06520 USA

来源：

ASTROPHYSICAL JOURNAL | 2014年 / 793卷 / 01期

关键词：

astroparticle physics; cosmic rays; Galaxy: general; Galaxy: halo; gamma rays: diffuse background; methods: data analysis; LARGE-AREA TELESCOPE; COSMIC-RAY PROPAGATION; CONTINUUM GAMMA-RAYS; P-P INTERACTION; X-RAY; COMPTON-SCATTERING; EMISSION; MILKY; RADIATION; PARAMETERIZATION;

D O I：

10.1088/0004-637X/793/1/64

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Fermi bubbles are two large structures in the gamma-ray sky extending to 55 degrees above and below the Galactic center. We analyze 50 months of Fermi Large Area Telescope data between 100MeV and 500 GeV above 10 degrees in Galactic latitude to derive the spectrum and morphology of the Fermi bubbles. We thoroughly explore the systematic uncertainties that arise when modeling the Galactic diffuse emission through two separate approaches. The gamma-ray spectrum is well described by either a log parabola or a power law with an exponential cutoff. We exclude a simple power law with more than 7 sigma significance. The power law with an exponential cutoff has an index of 1.9 +/- 0.2 and a cutoff energy of 110 +/- 50 GeV. We find that the gamma-ray luminosity of the bubbles is 4.4(-0.9)(+2.4) x 10(37) erg s(-1). We confirm a significant enhancement of gamma-ray emission in the southeastern part of the bubbles, but we do not find significant evidence for a jet. No significant variation of the spectrum across the bubbles is detected. The width of the boundary of the bubbles is estimated to be 3.4(-2.6)(+3.7) deg. Both inverse Compton (IC) models and hadronic models including IC emission from secondary leptons fit the gamma-ray data well. In the IC scenario, synchrotron emission from the same population of electrons can also explain the WMAP and Planck microwave haze with a magnetic field between 5 and 20 mu G.

引用

页数：34

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