MAGIC reveals a complex morphology within the unidentified gamma-ray source HESS J1857+026

J Aleksic,S Ansoldi,L Antonelli,P Antoranz,A Babic,P Bangale,U Barres De Almeida,J A Barrio,J Becerra Gonzalez,W Bednarek,E Bernardini, A Biland,O Blanch,S Bonnefoy,G Bonnoli,F Borracci,T Bretz,Eusebio Cano Carmona,A Carosi,D Carreto Fidalgo,P Colin,E Colombo,J L Contreras,J Cortina,Stefano Covino,P Da Vela,F Dazzi,A De Angelis,G De Caneva,B De Lotto,C Delgado Mendez,M Doert,A Dominguez,D Dominis Prester,D Dorner,M Doro,S Einecke,D Eisenacher,D Elsaesser,E Farina, D Ferenc,M V Fonseca,L Font,K Frantzen,C Fruck,R J Garcia Lopez, M Garczarczyk,D Garrido Terrats,M Gaug,N Godinovic,A Gonzalez Munoz,S R Gozzini,D Hadasch,M Hayashida,J Herrera,A Herrero,D Hildebrand,J Hose,D Hrupec,W Idec,V Kadenius,H Kellermann,S Klepser,K Kodani,Y Konno,J Krause,H Kubo,J Kushida,A La Barbera,D Lelas,N Lewandowska,E Lindfors,S Lombardi,M Lopez,R Lopezcoto,A Lopezoramas,E Lorenz,Irene Albarran Lozano,M Makariev,K Mallot,G Maneva,N Mankuzhiyil,K Mannheim,L Maraschi,B Marcote,Mauro Giorgio Mariotti,M Martinez,D Mazin,U Menzel,M Meucci,J M Miranda,R Mirzoyan,A Moralejo,P Munaradrover,D Nakajima,A Niedzwiecki, K Nilsson,K Nishijima,Katsuhisa Noda,N Nowak,E De Ona Wilhelmi,R Orito, A K Overkemping,S Paiano,M Palatiello, D Paneque,R Paoletti,J M Paredes,X Paredesfortuny,S Partini,M Persic,F Prada,P G Prada Moroni,E Prandini,S Preziuso,I Puljak,R Reinthal,W Rhode,M Ribo,J Rico,J Rodriguez Garcia, S Ruegamer,A Saggion,T Saito,Keisuke Saito,K Satalecka,V Scalzotto,V Scapin,C Schultz,T Schweizer,Steven N Shore, A Sillanpaa,J Sitarek,I Snidaric,D Sobczynska,F Spanier,V Stamatescu,A Stamerra,T Steinbring,J Storz,M Strzys,Siyuan Sun,T Suric,Leo O Takalo,Hideki Takami,F Tavecchio,P Temnikov,T Terzic,D Tescaro,M Teshima,J Thaele,O Tibolla,D F Torres,T Toyama,Aldo Treves,M Uellenbeck,P Vogler,R M Wagner,F Zandanel,R Zanin

ASTRONOMY & ASTROPHYSICS（2014）

引用 37|浏览4

暂无评分

摘要

Aims. HESS J1857+026 is an extended TeV gamma-ray source that was discovered by H. E. S. S. as part of its Galactic plane survey. Given its broadband spectral energy distribution and its spatial coincidence with the young energetic pulsar PSR J1856+0245, the source has been put forward as a pulsar wind nebula (PWN) candidate. MAGIC has performed follow-up observations aimed at mapping the source down to energies approaching 100 GeV in order to better understand its complex morphology. Methods. HESS J1857+026 was observed by MAGIC in 2010, yielding 29 h of good quality stereoscopic data that allowed us to map the source region in two separate ranges of energy. Results. We detected very-high-energy gamma-ray emission from HESS J1857+026 with a significance of 12 sigma above 150 GeV. The differential energy spectrum between 100 GeV and 13 TeV is described well by a power law function dN/dE = N-0(E/1TeV)(-Gamma) with N-0 = (5.37 +/- 0.44(stat) +/- 1.5(sys)) X 10(-12) (TeV-1 cm(-2) s(-1)) and Gamma = 2.16 +/- 0.07(stat) +/- 0.15(sys), which bridges the gap between the GeV emission measured by Fermi-LAT and the multi-TeV emission measured by H.E.S.S.. In addition, we present a detailed analysis of the energy-dependent morphology of this region. We couple these results with archival multiwavelength data and outline evidence in favor of a two-source scenario, whereby one source is associated with a PWN, while the other could be linked with a molecular cloud complex containing an HII region and a possible gas cavity.

查看译文

关键词

acceleration of particles,gamma rays: ISM,ISM: clouds,HII regions,ISM: individual objects: HESS J1857+026,pulsars: individual: PSR J1856+0245

AI 理解论文

溯源树

样例

生成溯源树，研究论文发展脉络

Chat Paper

正在生成论文摘要