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Diffuse Galactic gamma-ray emission with H.E.S.S

Abramowski, A.; Aharonian, F.; Ait Benkhali, F.; Akhperjanian, A.G.; Angüner, E.O.; Backes, M.; Balenderan, S.; Balzer, A.; Barnacka, A.; Becherini, Y.; Becker Tjus, J.; Berge, D.; Bernhard, S.; Bernlöhr, K.; Birsin, E.; Biteau, J.; Böttcher, M.; Boisson, C.; Bolmont, J.; Bordas, P.; Bregeon, J.; Brun, F.; Brun, P.; Bryan, M.; Bulik, T.; Carrigan, S.; Casanova, S.; Chadwick, P.M.; Chakraborty, N.; Chalme-Calvet, R.; Chaves, R.C.G.; Chrétien, M.; Colafrancesco, S.; Cologna, G.; Conrad, J.; Couturier, C.; Cui, Y.; Davids, I.D.; Degrange, B.; Deil, C.; deWilt, P.; Djannati-Ataï, A.; Domainko, W.; Donath, A.; Drury, L. O'C.; Dubus, G.; Dutson, K.; Dyks, J.; Dyrda, M.; Edwards, T.; Egberts, K.; Eger, P.; Espigat, P.; Farnier, C.; Fegan, S.; Feinstein, F.; Fernandes, M.V.; Fernandez, D.; Fiasson, A.; Fontaine, G.; Förster, A.; Füßling, M.; Gabici, S.; Gajdus, M.; Gallant, Y.A.; Garrigoux, T.; Giavitto, G.; Giebels, B.; Glicenstein, J.F.; Gottschall, D.; Grondin, M.-H.; Grudzińska, M.; Hadasc...

Diffuse Galactic gamma-ray emission with H.E.S.S Thumbnail


A. Abramowski

F. Aharonian

F. Ait Benkhali

A.G. Akhperjanian

E.O. Angüner

M. Backes

S. Balenderan

A. Balzer

A. Barnacka

Y. Becherini

J. Becker Tjus

D. Berge

S. Bernhard

K. Bernlöhr

E. Birsin

J. Biteau

M. Böttcher

C. Boisson

J. Bolmont

P. Bordas

J. Bregeon

F. Brun

P. Brun

M. Bryan

T. Bulik

S. Carrigan

S. Casanova

N. Chakraborty

R. Chalme-Calvet

R.C.G. Chaves

M. Chrétien

S. Colafrancesco

G. Cologna

J. Conrad

C. Couturier

Y. Cui

I.D. Davids

B. Degrange

C. Deil

P. deWilt

A. Djannati-Ataï

W. Domainko

A. Donath

L. O'C. Drury

G. Dubus

K. Dutson

J. Dyks

M. Dyrda

T. Edwards

K. Egberts

P. Eger

P. Espigat

C. Farnier

S. Fegan

F. Feinstein

M.V. Fernandes

D. Fernandez

A. Fiasson

G. Fontaine

A. Förster

M. Füßling

S. Gabici

M. Gajdus

Y.A. Gallant

T. Garrigoux

G. Giavitto

B. Giebels

J.F. Glicenstein

D. Gottschall

M.-H. Grondin

M. Grudzińska

D. Hadasch

S. Häffner

J. Hahn

J. Harris

G. Heinzelmann

G. Henri

G. Hermann

O. Hervet

A. Hillert

J.A. Hinton

W. Hofmann

P. Hofverberg

M. Holler

D. Horns

A. Ivascenko

A. Jacholkowska

C. Jahn

M. Jamrozy

M. Janiak

F. Jankowsky

I. Jung-Richardt

M.A. Kastendieck

K. Katarzyński

U. Katz

S. Kaufmann

B. Khélifi

M. Kieffer

S. Klepser

D. Klochkov

W. Kluźniak

D. Kolitzus

Nu Komin

K. Kosack

S. Krakau

F. Krayzel

P.P. Krüger

H. Laffon

G. Lamanna

J. Lefaucheur

V. Lefranc

A. Lemière

M. Lemoine-Goumard

J.-P. Lenain

T. Lohse

A. Lopatin

C.-C. Lu

V. Marandon

A. Marcowith

R. Marx

G. Maurin

N. Maxted

M. Mayer

T.J.L. McComb

J. Méhault

P.J. Meintjes

U. Menzler

M. Meyer

A.M.W. Mitchell

R. Moderski

M. Mohamed

K. Morâ

E. Moulin

T. Murach

M. de Naurois

J. Niemiec

S.J. Nolan

L. Oakes

H. Odaka

S. Ohm

B. Opitz

M. Ostrowski

I. Oya

M. Panter

R.D. Parsons

M. Paz Arribas

N.W. Pekeur

G. Pelletier

P.-O. Petrucci

B. Peyaud

S. Pita

H. Poon

G. Pühlhofer

M. Punch

A. Quirrenbach

S. Raab

I. Reichardt

A. Reimer

O. Reimer

M. Renaud

R. de los Reyes

F. Rieger

C. Romoli

S. Rosier-Lees

G. Rowell

B. Rudak

C.B. Rulten

V. Sahakian

D. Salek

D.A. Sanchez

A. Santangelo

R. Schlickeiser

F. Schüssler

A. Schulz

U. Schwanke

S. Schwarzburg

S. Schwemmer

H. Sol

F. Spanier

G. Spengler

F. Spies

Ł Stawarz

R. Steenkamp

C. Stegmann

F. Stinzing

K. Stycz

I. Sushch

J.-P. Tavernet

T. Tavernier

A.M. Taylor

R. Terrier

M. Tluczykont

C. Trichard

K. Valerius

C. van Eldik

B. van Soelen

G. Vasileiadis

J. Veh

C. Venter

A. Viana

P. Vincent

J. Vink

H.J. Völk

F. Volpe

M. Vorster

T. Vuillaume

S.J. Wagner

P. Wagner

R.M. Wagner

M. Ward

M. Weidinger

Q. Weitzel

R. White

A. Wierzcholska

P. Willmann

A. Wörnlein

D. Wouters

R. Yang

V. Zabalza

D. Zaborov

M. Zacharias

A.A. Zdziarski

A. Zech

H.-S. Zechlin

Y. Fukui

H.E.S.S. Collaboration


Diffuse γ-ray emission is the most prominent observable signature of celestial cosmic-ray interactions at high energies. While already being investigated at GeV energies over several decades, assessments of diffuse γ-ray emission at TeV energies remain sparse. After completion of the systematic survey of the inner Galaxy, the H.E.S.S. experiment is in a prime position to observe large-scale diffuse emission at TeV energies. Data of the H.E.S.S. Galactic Plane Survey are investigated in regions off known γ-ray sources. Corresponding γ-ray flux measurements were made over an extensive grid of celestial locations. Longitudinal and latitudinal profiles of the observed γ-ray fluxes show characteristic excess emission not attributable to known γ-ray sources. For the first time large-scale γ-ray emission along the Galactic plane using imaging atmospheric Cherenkov telescopes has been observed. While the background subtraction technique limits the ability to recover modest variation on the scale of the H.E.S.S. field of view or larger, which is characteristic of the inverse Compton scatter-induced Galactic diffuse emission, contributions of neutral pion decay as well as emission from unresolved γ-ray sources can be recovered in the observed signal to a large fraction. Calculations show that the minimum γ-ray emission from π0 decay represents a significant contribution to the total signal. This detection is interpreted as a mix of diffuse Galactic γ-ray emission and unresolved sources.

Journal Article Type Article
Publication Date Dec 15, 2014
Deposit Date Apr 15, 2015
Publicly Available Date Apr 22, 2015
Journal Physical Review D
Print ISSN 1550-7998
Electronic ISSN 1550-2368
Publisher American Physical Society
Peer Reviewed Peer Reviewed
Volume 90
Issue 12
Public URL
Related Public URLs


Published Journal Article (534 Kb)

Copyright Statement
Reprinted with permission from the American Physical Society: Physical Review D 90, 122007 © 2014 by the American Physical Society. Readers may view, browse, and/or download material for temporary copying purposes only, provided these uses are for noncommercial personal purposes. Except as provided by law, this material may not be further reproduced, distributed, transmitted, modified, adapted, performed, displayed, published, or sold in whole or part, without prior written permission from the American Physical Society.

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