Deeper H.E.S.S. observations of Vela Junior (RX J0852.04622): Morphology studies and resolved spectroscopy

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 , Agnès Balzer , M. Barnard , Y. Becherini , J. Becker Tjus , D. Berge , S. Bernhard , K. Bernlöhr , R. Blackwell , M. Böttcher , C. Boisson (1) , J. Bolmont (3) , 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. Chalme-Calvet (3) , R. C. G. Chaves , A. Chen , J. Chevalier (2) , M. Chrétien (3) , 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 , M. Gajdus , Y. Gallant , T. Garrigoux , G. Giavitto , B. Giebels (8) , J.F. Glicenstein , D. Gottschall , A. Goyal , M.-H. Grondin (5) , J. Hahn , M. Haupt , J. Hawkes , G. Heinzelmann , G. Henri (10) , G. Hermann , O. Hervet (1) , J.A. Hinton , W. Hofmann , C. Hoischen , M. Holler (8) , 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) , Michel Kieffer (3) , 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 , 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 , Emmanuel Moulin (6) , T. Murach , S. Nakashima , M. de Naurois , F. Niederwanger , J. Niemiec , L. Oakes , P. O’brien , H. Odaka , S. Öttl , S. Ohm , M. Ostrowski , I. Oya , M. Padovani , M. Panter , R. D. Parsons , M Paz Arribas , 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 , A. Reimer , O. Reimer , Matthieu Renaud (4) , R. de Los Reyes , S. Richter , F. Rieger , C. Romoli , G. Rowell , B. Rudak , C. 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 , Ł Stawarz , 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 , G. Vasileiadis (8) , J. Veh , C. Venter , A. Viana , P. Vincent (3) , J. Vink , F. Voisin , H. J. Völk , T. Vuillaume (2) , Z. Wadiasingh , S. Wagner (9) , P. Wagner , R.M. Wagner , R. White , A. Wierzcholska , P. Willmann , A. Wörnlein , D. Wouters (6) , R. Yang , V. Zabalza , 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

Aims. We study γ-ray emission from the shell-type supernova remnant (SNR) RX J0852.0−4622 to better characterize its spectral properties and its distribution over the SNR. Methods. The analysis of an extended High Energy Spectroscopic System (H.E.S.S.) data set at very high energies (E > 100 GeV) permits detailed studies, as well as spatially resolved spectroscopy, of the morphology and spectrum of the whole RX J0852.0−4622 region. The H.E.S.S. data are combined with archival data from other wavebands and interpreted in the framework of leptonic and hadronic models. The joint Fermi-LATH .E.S.S. spectrum allows the direct determination of the spectral characteristics of the parent particle population in leptonic and hadronic scenarios using only GeV-TeV data. Results. An updated analysis of the H.E.S.S. data shows that the spectrum of the entire SNR connects smoothly to the high-energy spectrum measured by Fermi-LAT. The increased data set makes it possible to demonstrate that the H.E.S.S. spectrum deviates significantly from a power law and is well described by both a curved power law and a power law with an exponential cutoff at an energy of E cut = (6.7±1.2 stat ±1.2 syst) TeV. The joint Fermi-LATH .E.S.S. spectrum allows the unambiguous identification of the spectral shape as a power law with an exponential cutoff. No significant evidence is found for a variation of the spectral parameters across the SNR, suggesting similar conditions of particle acceleration across the remnant. A simple modeling using one particle population to model the SNR emission demonstrates that both leptonic and hadronic emission scenarios remain plausible. It is also shown that at least a part of the shell emission is likely due to the presence of a pulsar wind nebula around PSR J0855−4644. A FITS image of the region of interest and two text files describing the H.E.S.S. spectrum of RX J0852.0-4622 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via

Domaines: Planète et Univers [physics]; Astrophysique [astro-ph]; Phénomènes cosmiques de haute energie [astro-ph.HE]

H. Abdalla, A. Abramowski, F. Aharonian, F. Ait Benkhali, A. G. Akhperjanian, et al.. Deeper H.E.S.S. observations of Vela Junior (RX J0852.04622): Morphology studies and resolved spectroscopy. Astronomy and Astrophysics - A&A, 2018, 612, pp.A7. ⟨10.1051/0004-6361/201630002⟩. ⟨hal-02410561⟩