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Title: The spectrum and morphology of the Fermi bubbles
Authors: M. Ackermann
A. Albert
W. B. Atwood
L. Baldini
J. Ballet
G. Barbiellini
D. Bastieri
R. Bellazzini
E. Bissaldi
R. D. Blandford
E. D. Bloom
E. Bottacini
T. J. Brandt
J. Bregeon
P. Bruel
R. Buehler
S. Buson
G. A. Caliandro
R. A. Cameron
M. Caragiulo
P. A. Caraveo
E. Cavazzuti
C. Cecchi
E. Charles
A. Chekhtman
J. Chiang
G. Chiaro
S. Ciprini
R. Claus
J. Cohen-Tanugi
J. Conrad
S. Cutini
F. D'Ammando
A. De Angelis
F. De Palma
C. D. Dermer
S. W. Digel
L. Di Venere
E. Do Couto E Silva
P. S. Drell
C. Favuzzi
E. C. Ferrara
W. B. Focke
A. Franckowiak
Y. Fukazawa
S. Funk
P. Fusco
F. Gargano
D. Gasparrini
S. Germani
N. Giglietto
F. Giordano
M. Giroletti
G. Godfrey
G. A. Gomez-Vargas
I. A. Grenier
S. Guiriec
D. Hadasch
A. K. Harding
E. Hays
J. W. Hewitt
X. Hou
T. Jogler
G. Jóhannesson
A. S. Johnson
W. N. Johnson
T. Kamae
J. Kataoka
J. Knödlseder
D. Kocevski
M. Kuss
S. Larsson
L. Latronico
F. Longo
F. Loparco
M. N. Lovellette
Deutsche Elektronen-Synchrotron
Kavli Institute for Particle Astrophysics and Cosmology
Santa Cruz Institute for Particle Physics
Istituto Nazionale di Fisica Nucleare, Roma
Institut de Recherche sur les Lois Fondamentales de l'Univers
Universita degli Studi di Trieste
Istituto Nazionale Di Fisica Nucleare, Sezione di Padova
Universita degli Studi di Padova
NASA Goddard Space Flight Center
Laboratoire Univers et Particules de Montpellier
Laboratoire Leprince-Ringuet
Consorzio Interuniversitario per la Fisica Spaziale (CIFS)
INAF Istituto di Astrofisica Spaziale e Fisica Cosmica, Milan
Agenzia Spaziale Italiana
Universita degli Studi di Perugia
George Mason University, Fairfax Campus
Osservatorio Astronomico di Roma
Stockholms universitet
Oskar Klein Centre for Cosmoparticle Physics
Kungl. Vetenskapsakademien
Istituto Di Radioastronomia, Bologna
Alma Mater Studiorum Universita di Bologna
Universita degli Studi di Udine
Naval Research Laboratory
Universita degli Studi di Bari
Hiroshima University
Pontificia Universidad Catolica de Chile
Medizinische Universitat Innsbruck
University of Maryland, Baltimore County
Centre d'Etudes Nucleaires de Bordeaux Gradignan
University Science Institute Reykjavik
Waseda University
CNRS Centre National de la Recherche Scientifique
Universite de Toulouse
Yale University
University of Maryland
Mahidol University
University of California, Irvine
University of Denver
Max Planck Institut fur Physik (Werner-Heisenberg-Institut)
Keywords: Earth and Planetary Sciences;Physics and Astronomy
Issue Date: 20-Sep-2014
Citation: Astrophysical Journal. Vol.793, No.1 (2014)
Abstract: © 2014. The American Astronomical Society. All rights reserved. The Fermi bubbles are two large structures in the gamma-ray sky extending to 55° above and below the Galactic center. We analyze 50 months of Fermi Large Area Telescope data between 100 MeV and 500 GeV above 10° 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 7σ 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 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 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 μG.
ISSN: 15384357
Appears in Collections:Scopus 2011-2015

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