Modulated high-energy gamma-ray emission from the microquasar Cygnus X-3
(176)
Abdo, A A
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Ackermann, M
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Ajello, M
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Giordano, F
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Grondin, M H
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Grove, J E
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Guiriec, S
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Hanabata, Y
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Harding, A K
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Hayashida, M
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Hays, E
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Hill, A B
z
Hjalmarsdotter, L
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Horan, D
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Hughes, R E
l
Jackson, M S
e,ai
Johannesson G
c
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u,ae
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Kocian, M L
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Kuss, M
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Latronico, L
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Lemoine Goumard, M
aa,ab
Longo, F
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Loparco, F
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Lovellette, M N
a
Lubrano, P
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Madejski, G M
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Makeev, A
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Marchand, L
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Marelli, M
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Max Moerbeck, W
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Omodei, N
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Ong, R A
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Ormes, J F
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Paneque, D
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Parent, D
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Pelassa, V
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Pepe, M
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Pesce Rollins, M
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Piron, F
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Pooley, G
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Porter, T A
at
Pottschmidt, K
u
Raino S
o,p
Rando, R
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Ray, P S
a
Razzano, M
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Rea, N
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Readhead, A
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Reimer, A
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Reimer, O
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Richards, J L
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Rochester, L S
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Rodriguez, J
g
Rodriguez, A Y
s
Romani, R W
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Ryde, F
e,ai
Sadrozinski, H F W
at
Sander, A
l
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at
Sgro C
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Siskind, E J
aw
Smith, D A
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Smith, P D
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Spinelli, P
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g
Stevenson, M
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a
Suson, D J
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Thayer, J B
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Thompson, D J
u
Tibaldo, L
g,j,k
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ay
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Tramacere, A
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Uchiyama, Y
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Vasileiou, V
u,ae
Vilchez, N
al
Vitale, V
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Waite, A P
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Wang, P
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Wilms, J
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Winer, B L
l
Wood, K S
a
Ylinen, T
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Ziegler, M
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note
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The orbital modulation on its own does not limit the size of the emitting region to the size of the binary orbit, because the orbital period could be imprinted on the emission occurring further out. However, the interpretation of the modulation as inverse Compton scattering off stellar photons requires the high-energy electrons to be within the system.
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72149111875
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The gamma rays in the Fermi energy range are unaffected by Compton scattering in the stellar wind or by pair production on the stellar UV photons.
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note
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The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and the Department of Energy in the United States; CEA/Institut de Recherches sur les lois Fondamentales de l'Univers and l'Institut National de Physique Nucléaire et de Physique des Particules/CNRS in France; the Agenzia Spaziale Italiana and Istituto Nazionale di Fisica Nucleare in Italy; the Ministry of Education, Culture, Sports, Science and Technology, National Laboratory for High Energy Physics (KEK), and Japan Aerospace Exploration Agency in Japan; and the K. A. Wallenberg Foundation, Swedish Research Council and National Space Board in Sweden. Additional support from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France for science analysis during the operations phase is also gratefully acknowledged. J.C. is a Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation. G.D. and A.B.H. are funded by contract ERC-StG-200911 from the European Community.
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