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We present the results of the most comprehensive survey of the Galactic plane in very high-energy (VHE) γ-rays, including a public release of Galactic sky maps, a catalog of VHE sources, and the discovery of 16 new sources of VHE γ-rays. The High Energy Spectroscopic System (H.E.S.S.) Galactic plane survey (HGPS) was a decade-long observation program carried out by the H.E.S.S. I array of Cherenkov telescopes in Namibia from 2004 to 2013. The observations amount to nearly 2700 h of quality-selected data, covering the Galactic plane at longitudes from ℓ = 250° to 65° and latitudes |b|≤ 3°. In addition to the unprecedented spatial coverage, the HGPS also features a relatively high angular resolution (0.08° ≈ 5 arcmin mean point spread function 68% containment radius), sensitivity (≲1.5% Crab flux for point-like sources), and energy range (0.2-100 TeV). We constructed a catalog of VHE γ-ray sources from the HGPS data set with a systematic procedure for both source detection and characterization of morphology and spectrum. We present this likelihood-based method in detail, including the introduction of a model component to account for unresolved, large-scale emission along the Galactic plane. In total, the resulting HGPS catalog contains 78 VHE sources, of which 14 are not reanalyzed here, for example, due to their complex morphology, namely shell-like sources and the Galactic center region. Where possible, we provide a firm identification of the VHE source or plausible associations with sources in other astronomical catalogs. We also studied the characteristics of the VHE sources with source parameter distributions. 16 new sources were previously unknown or unpublished, and we individually discuss their identifications or possible associations. We firmly identified 31 sources as pulsar wind nebulae (PWNe), supernova remnants (SNRs), composite SNRs, or gamma-ray binaries. Among the 47 sources not yet identified, most of them (36) have possible associations with cataloged objects, notably PWNe and energetic pulsars that could power VHE PWNe.
;Brun, P.;Bryan, M.;Büchele, M.;Bulik, T.;Capasso, M.;Carrigan, S.;Caroff, S.;Carosi, A.;Casanova, S.;Cerruti, M.;Chakraborty, N.;Chaves, R. C. G.
;Chen, A.;Chevalier, J.;Colafrancesco, S.;Condon, B.;Conrad, J.;Davids, I. D.;Decock, J.;Deil, C.
;Devin, J.;deWilt, P.;Dirson, L.;Djannati-Ataï, A.;Domainko, W.;Donath, A.
;Drury, L. O. 'C.;Dutson, K.;Dyks, J.;Edwards, T.;Egberts, K.;Eger, P.;Emery, G.;Ernenwein, J. -P.;Eschbach, S.;Farnier, C.;Fegan, S.;Fernandes, M. V.;Fiasson, A.;Fontaine, G.;Förster, A.;Funk, S.;Füßling, M.;Gabici, S.;Gallant, Y. A.;Garrigoux, T.;Gast, H.;Gaté, F.;Giavitto, G.;Giebels, B.;Glawion, D.;Glicenstein, J. F.;Gottschall, D.;Grondin, M. -H.;Hahn, J.;Haupt, M.;Hawkes, J.;Heinzelmann, G.;Henri, G.;Hermann, G.;Hinton, J. A.;Hofmann, W.;Hoischen, C.;Holch, T. L.;Holler, M.;Horns, D.;Ivascenko, A.;Iwasaki, H.;Jacholkowska, A.;Jamrozy, M.;Jankowsky, D.;Jankowsky, F.;Jingo, M.;Jouvin, L.;Jung-Richardt, I.;Kastendieck, M. A.;Katarzyński, K.;Katsuragawa, M.;Katz, U.;Kerszberg, D.;Khangulyan, D.;Khélifi, B.;King, J.;Klepser, S.;Klochkov, D.;Kluźniak, W.;Komin, Nu.;Kosack, K.;Krakau, S.;Kraus, M.;Krüger, P. P.;Laffon, H.;Lamanna, G.;Lau, J.;Lees, J. -P.;Lefaucheur, J.;Lemière, A.;Lemoine-Goumard, M.;Lenain, J. -P.;Leser, E.;Lohse, T.;Lorentz, M.;Liu, R.;López-Coto, R.;Lypova, I.;Marandon, V.
;Malyshev, D.;Marcowith, A.;Mariaud, C.;Marx, R.;Maurin, G.;Maxted, N.;Mayer, M.;Meintjes, P. J.;Meyer, M.;Mitchell, A. M. W.;Moderski, R.;Mohamed, M.;Mohrmann, L.;Morå, K.;Moulin, E.;Murach, T.;Nakashima, S.;de Naurois, M.;Ndiyavala, H.;Niederwanger, F.;Niemiec, J.;Oakes, L.;O'Brien, P.;Odaka, H.;Ohm, S.;Ostrowski, M.;Oya, I.;Padovani, M.;Panter, M.;Parsons, R. D.;Paz Arribas, M.;Pekeur, N. W.;Pelletier, G.;Perennes, C.;Petrucci, P. -O.;Peyaud, B.;Piel, Q.;Pita, S.;Poireau, V.;Poon, H.;Prokhorov, D.;Prokoph, H.;Pühlhofer, G.;Punch, M.;Quirrenbach, A.;Raab, S.;Rauth, R.;Reimer, A.;Reimer, O.;Renaud, M.;de los Reyes, R.;Rieger, F.;Rinchiuso, L.;Romoli, C.;Rowell, G.;Rudak, B.;Rulten, C. B.;Safi-Harb, S.;Sahakian, V.;Saito, S.;Sanchez, D. A.;Santangelo, A.;Sasaki, M.;Schandri, M.;Schlickeiser, R.;Schüssler, F.;Schulz, A.;Schwanke, U.;Schwemmer, S.;Seglar-Arroyo, M.;Settimo, M.;Seyffert, A. S.;Shafi, N.;Shilon, I.;Shiningayamwe, K.;Simoni, R.;Sol, H.;Spanier, F.;Spir-Jacob, M.;Stawarz, Ł.;Steenkamp, R.;Stegmann, C.;Steppa, C.;Sushch, I.;Takahashi, T.;Tavernet, J. -P.;Tavernier, T.;Taylor, A. M.;Terrier, R.;Tibaldo, L.;Tiziani, D.;Tluczykont, M.;Trichard, C.;Tsirou, M.;Tsuji, N.;Tuffs, R.;Uchiyama, Y.;van der Walt, D. J.;van Eldik, C.;van Rensburg, C.;van Soelen, B.;Vasileiadis, G.;Veh, J.;Venter, C.;Viana, A.;Vincent, P.;Vink, J.;Voisin, F.;Völk, H. J.;Vuillaume, T.;Wadiasingh, Z.;Wagner, S. J.;Wagner, P.;Wagner, R. M.;White, R.;Wierzcholska, A.;Willmann, P.;Wörnlein, A.;Wouters, D.;Yang, R.;Zaborov, D.;Zacharias, M.;Zanin, R.;Zdziarski, A. A.;Zech, A.;Zefi, F.;Ziegler, A.;Zorn, J.;Żywucka, N.
2018-01-01
Abstract
We present the results of the most comprehensive survey of the Galactic plane in very high-energy (VHE) γ-rays, including a public release of Galactic sky maps, a catalog of VHE sources, and the discovery of 16 new sources of VHE γ-rays. The High Energy Spectroscopic System (H.E.S.S.) Galactic plane survey (HGPS) was a decade-long observation program carried out by the H.E.S.S. I array of Cherenkov telescopes in Namibia from 2004 to 2013. The observations amount to nearly 2700 h of quality-selected data, covering the Galactic plane at longitudes from ℓ = 250° to 65° and latitudes |b|≤ 3°. In addition to the unprecedented spatial coverage, the HGPS also features a relatively high angular resolution (0.08° ≈ 5 arcmin mean point spread function 68% containment radius), sensitivity (≲1.5% Crab flux for point-like sources), and energy range (0.2-100 TeV). We constructed a catalog of VHE γ-ray sources from the HGPS data set with a systematic procedure for both source detection and characterization of morphology and spectrum. We present this likelihood-based method in detail, including the introduction of a model component to account for unresolved, large-scale emission along the Galactic plane. In total, the resulting HGPS catalog contains 78 VHE sources, of which 14 are not reanalyzed here, for example, due to their complex morphology, namely shell-like sources and the Galactic center region. Where possible, we provide a firm identification of the VHE source or plausible associations with sources in other astronomical catalogs. We also studied the characteristics of the VHE sources with source parameter distributions. 16 new sources were previously unknown or unpublished, and we individually discuss their identifications or possible associations. We firmly identified 31 sources as pulsar wind nebulae (PWNe), supernova remnants (SNRs), composite SNRs, or gamma-ray binaries. Among the 47 sources not yet identified, most of them (36) have possible associations with cataloged objects, notably PWNe and energetic pulsars that could power VHE PWNe.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11582/318019
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simulazione ASN
Il report seguente simula gli indicatori relativi alla propria produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione. La simulazione si basa sui dati IRIS e sugli indicatori bibliometrici alla data indicata e non tiene conto di eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori. La simulazione può differire dall'esito di un’eventuale domanda ASN sia per errori di catalogazione e/o dati mancanti in IRIS, sia per la variabilità dei dati bibliometrici nel tempo. Si consideri che Anvur calcola i valori degli indicatori all'ultima data utile per la presentazione delle domande.
La presente simulazione è stata realizzata sulla base delle specifiche raccolte sul tavolo ER del Focus Group IRIS coordinato dall’Università di Modena e Reggio Emilia e delle regole riportate nel DM 589/2018 e allegata Tabella A. Cineca, l’Università di Modena e Reggio Emilia e il Focus Group IRIS non si assumono alcuna responsabilità in merito all’uso che il diretto interessato o terzi faranno della simulazione. Si specifica inoltre che la simulazione contiene calcoli effettuati con dati e algoritmi di pubblico dominio e deve quindi essere considerata come un mero ausilio al calcolo svolgibile manualmente o con strumenti equivalenti.
