Characterising the VHE diffuse emission in the central 200 parsecs of our Galaxy with H.E.S.S

H. Abdalla , A. Abramowski , F. Aharonian , F. Ait Benkhali , A.G. Akhperjanian , T. Andersson , E.O. Angüner , M. Arakawa , M. Arrieta (1) , P. Aubert (2) , M. Backes , A. Balzer , M. Barnard , Y. Becherini , J. Becker Tjus , D. Berge , S. Bernhard , K. Bernlöhr , R. Blackwell , M. Böttcher , C. Boisson (1) , J. Bolmont (3) , S. Bonnefoy , P. Bordas , J. Bregeon (4) , F. Brun (5) , P. Brun (6) , M. Bryan , M. Büchele , T. Bulik , M. Capasso , J. Carr (7) , S. Casanova , M. Cerruti (3) , N. Chakraborty , R.C.G. Chaves (4) , A. Chen , J. Chevalier (2) , M. Coffaro , S. Colafrancesco , G. Cologna , B. Condon (5) , J. Conrad , Y. Cui , I.D. Davids , J. Decock (6) , B. Degrange (8) , C. Deil , J. Devin (4) , P. Dewilt , L. Dirson , A. Djannati-Ataï (9) , W. Domainko , A. Donath , L.O'C. Drury , K. Dutson , J. Dyks , T. Edwards , K. Egberts , P. Eger , J.-P. Ernenwein (7) , S. Eschbach , C. Farnier , S. Fegan (8) , M.V. Fernandes , A. Fiasson (2) , G. Fontaine (8) , A. Förster , S. Funk , M. Füssling , S. Gabici (9) , Y.A. Gallant (4) , T. Garrigoux , G. Giavitto , B. Giebels (8) , J.F. Glicenstein (6) , D. Gottschall , A. Goyal , M.-H. Grondin (5) , J. Hahn , M. Haupt , J. Hawkes , G. Heinzelmann , G. Henri (10) , G. Hermann , J.A. Hinton , W. Hofmann , C. Hoischen , T.L. Holch , M. Holler , D. Horns , A. Ivascenko , H. Iwasaki , A. Jacholkowska (3) , M. Jamrozy , M. Janiak , D. Jankowsky , F. Jankowsky , M. Jingo , T. Jogler , L. Jouvin (9) , I. Jung-Richardt , M.A. Kastendieck , K. Katarzyński , M. Katsuragawa , U. Katz , D. Kerszberg (3) , D. Khangulyan , B. Khélifi (9) , J. King , S. Klepser , D. Klochkov , W. Kluźniak , D. Kolitzus , Nu. Komin , K. Kosack (6) , S. Krakau , M. Kraus , P.P. Krüger , H. Laffon (5) , G. Lamanna (2) , J. Lau , J.-P. Lees (2) , J. Lefaucheur (1) , V. Lefranc (6) , A. Lemière (9) , M. Lemoine-Goumard (5) , J.-P. Lenain (3) , E. Leser , T. Lohse , M. Lorentz (6) , R. Liu , R. López-Coto , I. Lypova , V. Marandon , Alexandre Marcowith (4) , C. Mariaud (8) , R. Marx , G. Maurin (2) , N. Maxted , M. Mayer , P.J. Meintjes , M. Meyer , A.M.W. Mitchell , R. Moderski , M. Mohamed , L. Mohrmann , K. Morå , E. Moulin (6) , T. Murach , S. Nakashima , M. de Naurois (8) , F. Niederwanger , J. Niemiec , L. Oakes , P. O'Brien , H. Odaka , S. Ohm , M. Ostrowski , I. Oya , M. Padovani (4) , M. Panter , R.D. Parsons , N.W. Pekeur , G. Pelletier (10) , C. Perennes (3) , P.-O. Petrucci (10) , B. Peyaud (6) , Q. Piel (2) , S. Pita (9) , H. Poon , D. Prokhorov , H. Prokoph , G. Pühlhofer , M. Punch (9) , A. Quirrenbach , S. Raab , R. Rauth , A. Reimer , O. Reimer , Matthieu Renaud (4) , R. de Los Reyes , S. Richter , F. Rieger , C. Romoli , G. Rowell , B. Rudak , C.B. Rulten (1) , V. Sahakian , S. Saito , D. Salek , D.A. Sanchez (2) , A. Santangelo , M. Sasaki , R. Schlickeiser , F. Schüssler (6) , A. Schulz , U. Schwanke , S. Schwemmer , M. Seglar-Arroyo (6) , M. Settimo (3) , A.S. Seyffert , N. Shafi , I. Shilon , R. Simoni , H. Sol (1) , F. Spanier , G. Spengler , F. Spies , R. Steenkamp , C. Stegmann , K. Stycz , I. Sushch , T. Takahashi , J.-P. Tavernet (3) , T. Tavernier (9) , A.M. Taylor , R. Terrier (9) , L. Tibaldo , D. Tiziani , M. Tluczykont , C. Trichard (7) , N. Tsuji , R. Tuffs , Y. Uchiyama , D.J. van Der Walt , C. van Eldik , C. van Rensburg , B. van Soelen , George Vasileiadis (4) , J. Veh , C. Venter , A. Viana , P. Vincent (3) , J. Vink , F. Voisin , H.J. Völk , T. Vuillaume (2) , Z. Wadiasingh , S.J. Wagner , P. Wagner , R.M. Wagner , R. White , A. Wierzcholska , P. Willmann , A. Wörnlein , D. Wouters (6) , R. Yang , D. Zaborov (8) , M. Zacharias , R. Zanin , A.A. Zdziarski , A. Zech (1) , F. Zefi (8) , A. Ziegler , N. Żywucka

1 LUTH (UMR_8102) - Laboratoire Univers et Théories
2 LAPP - Laboratoire d'Annecy de Physique des Particules
3 LPNHE (UMR_7585) - Laboratoire de Physique Nucléaire et de Hautes Énergies
4 LUPM - Laboratoire Univers et Particules de Montpellier
5 CENBG - Centre d'Etudes Nucléaires de Bordeaux Gradignan
6 IRFU - Institut de Recherches sur les lois Fondamentales de l'Univers
7 CPPM - Centre de Physique des Particules de Marseille
8 LLR - Laboratoire Leprince-Ringuet
9 APC (UMR_7164) - AstroParticule et Cosmologie
10 IPAG - Institut de Planétologie et d'Astrophysique de Grenoble

The diffuse very high-energy (VHE; >100 GeV) γ-ray emission observed in the central 200 pc of the Milky Way by H.E.S.S. was found to follow dense matter distribution in the central molecular zone (CMZ) up to a longitudinal distance of about 130 pc to the Galactic centre (GC), where the flux rapidly decreases. This was initially interpreted as the result of a burst-like injection of energetic particles 104 yr ago, but a recent more sensitive H.E.S.S. analysis revealed that the cosmic-ray (CR) density profile drops with the distance to the centre, making data compatible with a steady cosmic PeVatron at the GC. In this paper, we extend this analysis to obtain, for the first time, a detailed characterisation of the correlation with matter and to search for additional features and individual γ-ray sources in the inner 200 pc. Taking advantage of 250 h of H.E.S.S. data and improved analysis techniques, we perform a detailed morphology study of the diffuse VHE emission observed from the GC ridge and reconstruct its total spectrum. To test the various contributions to the total γ-ray emission, we used an iterative 2D maximum-likelihood approach that allows us to build a phenomenological model of the emission by summing a number of different spatial components. We show that the emission correlated with dense matter covers the full CMZ and that its flux is about half the total diffuse emission flux. We also detect some emission at higher latitude that is likely produced by hadronic collisions of CRs in less dense regions of the GC interstellar medium. We detect an additional emission component centred on the GC and extending over about 15 pc that is consistent with the existence of a strong CR density gradient and confirms the presence of a CR accelerator at the very centre of our Galaxy. We show that the spectrum of full ridge diffuse emission is compatible with that previously derived from the central regions, suggesting that a single population of particles fills the entire CMZ. Finally, we report the discovery of a VHE γ-ray source near the GC radio arc and argue that it is produced by the pulsar wind nebula candidate G0.13−0.11.Key words: gamma rays: general / gamma rays: ISM / Galaxy: center / cosmic rays† Deceased.

Mots clés: gamma rays: general; gamma rays: ISM; Galaxy: center; cosmic rays

Domaines: Astrophysique [astro-ph]

H. Abdalla, A. Abramowski, F. Aharonian, F. Ait Benkhali, A.G. Akhperjanian, et al.. Characterising the VHE diffuse emission in the central 200 parsecs of our Galaxy with H.E.S.S. Astronomy and Astrophysics - A&A, 2018, 612, pp.A9. ⟨10.1051/0004-6361/201730824⟩. ⟨hal-01815286⟩