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

Abdalla, H.; Aharonian, F.; Ait Benkhali, F.; Anguner, E. O.; Arcaro, C.; Armand, C.; Armstrong, T.; Ashkar, H.; Backes, M.; Baghmanyan, V.; Barbosa Martins, V.; Barnacka, A.; Barnard, M.; Becherini, Y.; Berge, D.; Bernlohr, K.; Bi, B.; Bottcher, M.; Boisson, C.; Bolmont, J.; De Bonyde Lavergne, M.; Breuhaus, M.; Brose, R.; Brun, F.; Brun, P.; Bryan, M.; Buchele, M.; Bulik, T.; Bylund, T.; Caroff, S.; Carosi, A.; Chand, T.; Chandra, S.; Chen, A.; Cotter, G.; Curylo, M.; Damascene Mbarubucyeye, J.; Davids, I. D.; Davies, J.; Deil, C.; Devin, J.; Dirson, L.; Djannati-Atai, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Dreyer, L.; Duffy, C.; Dyks, J.; Egberts, K.; Eichhorn, F.; Einecke, S.; Emery, G.; Ernenwein, J. -P.; Feijen, K.; Fegan, S.; Fiasson, A.; Fichet De Clairfontaine, G.; Fontaine, G.; Funk, S.; Fussling, M.; Gabici, S.; Gallant, Y. A.; Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M. -H.; Hahn, J.; Haupt, M.; Hermann, G.; Hinton, J. A.; Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.; Horbe, M.; Horns, D.; Huber, D.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jung-Richardt, I.; Kasai, E.; Kastendieck, M. A.; Katarzynski, K.; Katz, U.; Khangulyan, D.; Khelifi, B.; Klepser, S.; Kluzniak, W.; Komin, N.; Konno, R.; Kosack, K.; Kostunin, D.; Kreter, M.; Lamanna, G.; Lemiere, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leuschner, F.; Levy, C.; Lohse, T.; Lypova, I.; Mackey, J.; Majumdar, J.; Malyshev, D.; Malyshev, D.; Marandon, V.; Marchegiani, P.; Marcowith, A.; Mares, A.; Marti-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Meyer, M.; Mitchell, A. M. W.; Moderski, R.; Mohrmann, L.; Montanari, A.; Moore, C.; Morris, P.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, K.; Nayerhoda, A.; De Naurois, M.; Ndiyavala, H.; Niemiec, J.; Oakes, L.; O'Brien, P.; Odaka, H.; Ohm, S.; Olivera-Nieto, L.; De Ona Wilhelmi, E.; Ostrowski, M.; Panter, M.; Panny, S.; Parsons, R. D.; Peron, G.; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V.; Priyana Noel, A.; Prokhorov, D. A.; Prokoph, H.; Puhlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.; Reichherzer, P.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Sahakian, V.; Sailer, S.; Salzmann, H.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Schafer, J.; Schussler, F.; Schutte, H. M.; Schwanke, U.; Seglar-Arroyo, M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shapopi, J. N. S.; Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Specovius, A.; Spencer, S.; Spir-Jacob, M.; Stawarz, L.; Sun, L.; Steenkamp, R.; Stegmann, C.; Steinmassl, S.; Steppa, C.; Takahashi, T.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Thiersen, J. H. E.; Tiziani, D.; Tluczykont, M.; Tomankova, L.; Trichard, C.; Tsirou, M.; Tuffs, R.; Uchiyama, Y.; Van Der Walt, D. J.; Van Eldik, C.; Van Rensburg, C.; Van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Volk, H. J.; Wadiasingh, Z.; Wagner, S. J.; Watson, J.; Werner, F.; White, R.; Wierzcholska, A.; Wong, Y. W.; Yusafzai, A.; Zacharias, M.; Zanin, R.; Zargaryan, D.; Zdziarski, A. A.; Zech, A.; Zhu, S. J.; Zmija, A.; Zorn, J.; Zouari, S.; Zywucka, N.; Albert, A.; Alfaro, R.; Alvarez, C.; Arteaga-Velezquez, J. C.; Arunbabu, K. P.; Avila Rojas, D.; Belmont-Moreno, E.; Benzvi, S. Y.; Brisbois, C.; Caballero-Mora, K. S.; Capistran, T.; Carraminana, A.; Casanova, S.; Cotti, U.; Cotzomi, J.; Coutino De Leon, S.; De La Fuente, E.; De Leon, C.; Diaz Hernandez, R.; Diaz-Velez, J. C.; Dingus, B. L.; Duvernois, M. A.; Durocher, M.; Ellsworth, R. W.; Engel, K.; Espinoza, C.; Fan, K. L.; Fernandez Alonso, M.; Fraija, N.; Galvan-Gamez, A.; Garcia, D.; Garcia-Gonzalez, J. A.; Garfias, F.; Giacinti, G.; Gonzalez, M. M.; Goodman, J. A.; Harding, J. P.; Hernandez, S.; Hona, B.; Huang, D.; Hueyotl-Zahuantitla, F.; Huntemeyer, P.; Iriarte, A.; Jardin-Blicq, A.; Joshi, V.; Kieda, D.; Lee, W. H.; Leon Vargas, H.; Linnemann, J. T.; Longinotti, A. L.; Luis-Raya, G.; Lopez-Coto, R.; Malone, K.; Martinez, O.; Martinez-Castellanos, I.; Martinez-Castro, J.; Matthews, J. A.; Miranda-Romagnoli, P.; Morales-Soto, J. A.; Moreno, E.; Mostafa, M.; Nayerhoda, A.; Nellen, L.; Newbold, M.; Nisa, M. U.; Noriega-Papaqui, R.; Omodei, N.; Peisker, A.; Perez Araujo, Y.; Perez-Perez, E. G.; Rho, C. D.; Rosa-Gonzalez, D.; Ruiz-Velasco, E.; Salesa Greus, F.; Sandoval, A.; Schneider, M.; Schoorlemmer, H.; Serna-Franco, J.; Smith, A. J.; Springer, R. W.; Surajbali, P.; Tollefson, K.; Torres, I.; Torres-Escobedo, R.; Turner, R.; Urena-Mena, F.; Villasenor, L.; Weisgarber, T.; Willox, E.; Zhou, H.

doi:10.3847/1538-4357/abf64b

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.