Skip to main navigation Skip to search Skip to main content

TeV Emission of Galactic Plane Sources with HAWC and H.E.S.S.

  • H. Abdalla
  • , F. Aharonian
  • , F. Ait Benkhali
  • , E. O. Angüner
  • , C. Arcaro
  • , C. Armand
  • , T. Armstrong
  • , H. Ashkar
  • , M. Backes
  • , V. Baghmanyan
  • , V. Barbosa Martins
  • , A. Barnacka
  • , M. Barnard
  • , Y. Becherini
  • , D. Berge
  • , K. Bernlöhr
  • , B. Bi
  • , M. Böttcher
  • , C. Boisson
  • , J. Bolmont
  • M. De Bonyde Lavergne, M. Breuhaus, R. Brose, F. Brun, P. Brun, M. Bryan, M. Büchele, T. Bulik, T. Bylund, S. Caroff, A. Carosi, T. Chand, S. Chandra, A. Chen, G. Cotter, M. Curyło, J. Damascene Mbarubucyeye, I. D. Davids, J. Davies, C. Deil, J. Devin, L. Dirson, A. Djannati-Ataï, A. Dmytriiev, A. Donath, V. Doroshenko, L. Dreyer, C. Duffy, J. Dyks, K. Egberts, F. Eichhorn, S. Einecke, G. Emery, J. P. Ernenwein, K. Feijen, S. Fegan, A. Fiasson, G. Fichet De Clairfontaine, G. Fontaine, S. Funk, M. Füßling, S. Gabici, Y. A. Gallant, G. Giavitto, L. Giunti, D. Glawion, J. F. Glicenstein, D. Gottschall, M. H. Grondin, J. Hahn, M. Haupt, G. Hermann, J. A. Hinton, W. Hofmann, C. Hoischen, T. L. Holch, M. Holler, M. Hörbe, D. Horns, D. Huber, M. Jamrozy, D. Jankowsky, F. Jankowsky, I. Jung-Richardt, E. Kasai, M. A. Kastendieck, K. Katarzyński, U. Katz, D. Khangulyan, B. Khélifi, S. Klepser, W. Kluźniak, Nu Komin, R. Konno, K. Kosack, D. Kostunin, M. Kreter, G. Lamanna, A. Lemière, M. Lemoine-Goumard, J. P. Lenain, F. Leuschner, C. Levy, T. Lohse, I. Lypova, J. Mackey, J. Majumdar, D. Malyshev, D. Malyshev, V. Marandon, P. Marchegiani, A. Marcowith, A. Mares, G. Martí-Devesa, R. Marx, G. Maurin, P. J. Meintjes, M. Meyer, A. M.W. Mitchell, R. Moderski, L. Mohrmann, A. Montanari, C. Moore, P. Morris, E. Moulin, J. Muller, T. Murach, K. Nakashima, A. Nayerhoda, M. De Naurois, H. Ndiyavala, J. Niemiec, L. Oakes, P. O'Brien, H. Odaka, S. Ohm, L. Olivera-Nieto, E. De Ona Wilhelmi, M. Ostrowski, M. Panter, S. Panny, R. D. Parsons, G. Peron, B. Peyaud, Q. Piel, S. Pita, V. Poireau, A. Priyana Noel, D. A. Prokhorov, H. Prokoph, G. Pühlhofer, M. Punch, A. Quirrenbach, S. Raab, R. Rauth, P. Reichherzer, A. Reimer, O. Reimer, Q. Remy, M. Renaud, F. Rieger, L. Rinchiuso, C. Romoli, G. Rowell, B. Rudak, V. Sahakian, S. Sailer, H. Salzmann, D. A. Sanchez, A. Santangelo, M. Sasaki, J. Schäfer, F. Schüssler, H. M. Schutte, U. Schwanke, M. Seglar-Arroyo, M. Senniappan, A. S. Seyffert, N. Shafi, J. N.S. Shapopi, K. Shiningayamwe, R. Simoni, A. Sinha, H. Sol, A. Specovius, S. Spencer, M. Spir-Jacob, Stawarz, L. Sun, R. Steenkamp, C. Stegmann, S. Steinmassl, C. Steppa, T. Takahashi, T. Tavernier, A. M. Taylor, R. Terrier, J. H.E. Thiersen, D. Tiziani, M. Tluczykont, L. Tomankova, C. Trichard, M. Tsirou, R. Tuffs, Y. Uchiyama, D. J. Van Der Walt, C. Van Eldik, C. Van Rensburg, B. Van Soelen, G. Vasileiadis, J. Veh, C. Venter, P. Vincent, J. Vink, H. J. Völk, Z. Wadiasingh, S. J. Wagner, J. Watson, F. Werner, R. White, A. Wierzcholska, Yu Wun Wong, A. Yusafzai, M. Zacharias, R. Zanin, D. Zargaryan, A. A. Zdziarski, A. Zech, S. J. Zhu, A. Zmija, J. Zorn, S. Zouari, N. Żywucka, A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velézquez, K. P. Arunbabu, D. Avila Rojas, E. Belmont-Moreno, S. Y. Benzvi, C. Brisbois, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño De León, E. De La Fuente, C. De León, R. Diaz Hernandez, J. C. Díaz-Vélez, B. L. Dingus, M. A. Duvernois, M. Durocher, R. W. Ellsworth, K. Engel, C. Espinoza, K. L. Fan, M. Fernández Alonso, N. Fraija, A. Galván-Gámez, D. Garcia, J. A. García-González, F. Garfias, G. Giacinti, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, B. Hona, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, A. Jardin-Blicq, V. Joshi, D. Kieda, W. H. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, R. López-Coto, K. Malone, O. Martinez, I. Martinez-Castellanos, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, F. Salesa Greus, A. Sandoval, M. Schneider, H. Schoorlemmer, J. Serna-Franco, A. J. Smith, R. W. Springer, P. Surajbali, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, T. Weisgarber, E. Willox, H. Zhou
  • University of Namibia
  • Dublin Institute for Advanced Studies
  • Max-Planck-Institut für Kernphysik
  • Russian-Armenian University
  • Aix-Marseille Université
  • North-West University
  • LTHE (UMR 5564 CNRS/IRD/Université de Grenoble)
  • University of Oxford
  • Université Paris-Saclay
  • Institute for Nuclear Physics
  • c/o DESY
  • Jagiellonian University
  • Linnaeus University, Växjö
  • University of Tübingen
  • LUTH - Laboratoire de l'Univers et de ses Theories
  • Sorbonne Université
  • University of Amsterdam
  • Friedrich-Alexander University (FAU) Erlangen-Nürnberg and Universitätsklinikum Erlangen
  • University of Warsaw
  • University of the Witwatersrand, Johannesburg
  • Astroparticule and Cosmol APC
  • Universität Hamburg
  • University of Leicester
  • Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences
  • University of Potsdam
  • University of Adelaide
  • Laboratoire Univers et Particules de Montpellier
  • Univ. Bordeaux
  • University of Innsbruck
  • Landessternwarte Heidelberg
  • Nicolaus Copernicus University
  • Rikkyo University
  • Humboldt-Universität zu Berlin
  • University of the Free State
  • University of Tokyo
  • Yerevan Physics Institute
  • MST-8, Los Alamos National Laboratory
  • Universidad Nacional Autónoma de México
  • Universidad Autónoma de Chiapas
  • Universidad Michoacana de San Nicolás de Hidalgo
  • University of Rochester
  • University of Maryland
  • Instituto Nacional de Astrofísica Óptica y Electrónica (INAOE)
  • Benemerita Universidad Autonoma de Puebla
  • Universidad de Guadalajara
  • University of Wisconsin-Madison
  • Pennsylvania State University
  • Tecnologico de Monterrey
  • University of Utah
  • Michigan Technological University
  • Chulalongkorn University
  • National Astronomical Research Institute of Thailand
  • Michigan State University
  • Universidad Politécnica de Pachuca
  • University of Padova
  • Instituto Politécnico Nacional
  • University of New Mexico
  • Universidad Autónoma del Estado de Hidalgo
  • Instituto de Ciencias Nucleares de la UNAM
  • Stanford University
  • University of Valencia
  • Shanghai Jiao Tong University

Research output: Contribution to journalArticlepeer-review

Abstract

The High Altitude Water Cherenkov (HAWC) observatory and the High Energy Stereoscopic System (H.E.S.S.) are two leading instruments in the ground-based very-high-energy γ-ray domain. HAWC employs the water Cherenkov detection (WCD) technique, while H.E.S.S. is an array of Imaging Atmospheric Cherenkov Telescopes (IACTs). The two facilities therefore differ in multiple aspects, including their observation strategy, the size of their field of view, and their angular resolution, leading to different analysis approaches. Until now, it has been unclear if the results of observations by both types of instruments are consistent: several of the recently discovered HAWC sources have been followed up by IACTs, resulting in a confirmed detection only in a minority of cases. With this paper, we go further and try to resolve the tensions between previous results by performing a new analysis of the H.E.S.S. Galactic plane survey data, applying an analysis technique comparable between H.E.S.S. and HAWC. Events above 1 TeV are selected for both data sets, the point-spread function of H.E.S.S. is broadened to approach that of HAWC, and a similar background estimation method is used. This is the first detailed comparison of the Galactic plane observed by both instruments. H.E.S.S. can confirm the γ-ray emission of four HAWC sources among seven previously undetected by IACTs, while the three others have measured fluxes below the sensitivity of the H.E.S.S. data set. Remaining differences in the overall γ-ray flux can be explained by the systematic uncertainties. Therefore, we confirm a consistent view of the γ-ray sky between WCD and IACT techniques.

Original languageEnglish
Article number6
JournalAstrophysical Journal
Volume917
Issue number1
DOIs
Publication statusPublished - 10 Aug 2021

Fingerprint

Dive into the research topics of 'TeV Emission of Galactic Plane Sources with HAWC and H.E.S.S.'. Together they form a unique fingerprint.

Cite this