A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Periastron Observations of TeV Gamma-Ray Emission from a Binary System with a 50-year Period
Tekijät: Abeysekara AU, Benbow W, Bird R, Brill A, Brose R, Buckley JH, Chromey AJ, Daniel MK, Falcone A, Finley JP, Fortson L, Furniss A, Gent A, Gillanders GH, Hanna D, Hassan T, Hervet O, Holder J, Hughes G, Humensky TB, Kaaret P, Kar P, Kertzman M, Kieda D, Krause M, Krennrich F, Kumar S, Lang MJ, Lin TTY, Maier G, Moriarty P, Mukherjee R, O'Brien S, Ong RA, Otte AN, Park N, Petrashyk A, Pohl M, Pueschel E, Quinn J, Ragan K, Richards GT, Roache E, Sadeh I, Santander M, Schlenstedt S, Sembroski GH, Sushch I, Tyler J, Vassiliev VV, Wakely SP, Weinstein A, Wells RM, Wilcox P, Wilhelm A, Williams DA, Williamson TJ, Zitzer B, Acciari VA, Ansoldi S, Antonelli LA, Engels AA, Baack D, Babic A, Banerjee B, de Almeida UB, Barrio JA, Gonzalez JB, Bednarek W, Bernardini E, Berti A, Besenrieder J, Bhattacharyya W, Bigongiari C, Biland A, Blanch O, Bonnoli G, Busetto G, Carosi R, Ceribella G, Cikota S, Colak SM, Colin P, Colombo E, Contreras JL, Cortina J, Covino S, D'Elia V, Da Vela P, Dazzi F, De Angelis A, De Lotto B, Delfino M, Delgado J, Di Pierro F, Espinera ED, Dominguez A, Prester DD, Dorner D, Doro M, Einecke S, Elsaesser D, Ramazani VF, Fattorini A, Fernandez-Barral A, Ferrara G, Fidalgo D, Foffano L, Fonseca MV, Font L, Fruck C, Galindo D, Gallozzi S, Lopez RJG, Garczarczyk M, Gasparyan S, Gaug M, Giammaria P, Godinovic N, Guberman D, Hadasch D, Hahn A, Herrera J, Hoang J, Hrupec D, Inoue S, Ishio K, Iwamura Y, Kubo H, Kushida J, Kuvezdic D, Lamastra A, Lelas D, Leone F, Lindfors E, Lombardi S, Longo F, Lopez M, Lopez-Oramas A, Fraga BMD, Maggio C, Majumdar P, Makariev M, Mallamaci M, Maneva G, Manganaro M, Mannheim K, Maraschi L, Mariotti M, Martinez M, Masuda S, Mazin D, Minev M, Miranda JM, Mirzoyan R, Molina E, Moralejo A, Moreno V, Moretti E, Munar-Adrover P, Neustroev V, Niedzwiecki A, Rosillo MN, Nigro C, Nilsson K, Ninci D, Nishijima K, Noda K, Nogues L, Nothe M, Paiano S, Palacio J, Paneque D, Paoletti R, Paredes JM, Pedaletti G, Penil P, Peresano M, Persic M, Moroni PGP, Prandini E, Puljak I, Garcia JR, Rhode W, Ribo M, Rico J, Righi C, Rugliancich A, Saha L, Sahakyan N, Saito T, Satalecka K, Schweizer T, Sitarek J, Snidaric I, Sobczynska D, Somero A, Stamerra A, Strzys M, Suric T, Tavecchio F, Temnikov P, Terzic T, Teshima M, Torres-Alba N, Tsujimoto S, van Scherpenberg J, Vanzo G, Acosta MV, Vovk I, Will M, Zaric D, Zaric D
Kustantaja: IOP PUBLISHING LTD
Julkaisuvuosi: 2018
Journal: Astrophysical Journal Letters
Tietokannassa oleva lehden nimi: ASTROPHYSICAL JOURNAL LETTERS
Lehden akronyymi: ASTROPHYS J LETT
Artikkelin numero: ARTN L19
Vuosikerta: 867
Sivujen määrä: 8
ISSN: 2041-8205
eISSN: 2041-8213
DOI: https://doi.org/10.3847/2041-8213/aae70e
Verkko-osoite: http://iopscience.iop.org/article/10.3847/2041-8213/aae70e
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/36685513
We report on observations of the pulsar/Be star binary system PSR J2032+4127/MT91 213 in the energy range between 100 GeV and 20 TeV with the Very Energetic Radiation Imaging Telescope Array and Major Atmospheric Gamma Imaging Cherenkov telescope arrays. The binary orbit has a period of approximately 50 years, with the most recent periastron occurring on 2017 November 13. Our observations span from 18 months prior to periastron to one month after. A new point-like gamma-ray source is detected, coincident with the location of PSR J2032+4127/MT91 213. The gamma-ray light curve and spectrum are well characterized over the periastron passage. The flux is variable over at least an order of magnitude, peaking at periastron, thus providing a firm association of the TeV source with the pulsar/Be star system. Observations prior to periastron show a cutoff in the spectrum at an energy around 0.5 TeV. This result adds a new member to the small population of known TeV binaries, and it identifies only the second source of this class in which the nature and properties of the compact object are firmly established. We compare the gamma-ray results with the light curve measured with the X-ray Telescope on board the Neil Gehrels Swift Observatory and with the predictions of recent theoretical models of the system. We conclude that significant revision of the models is required to explain the details of the emission that we have observed, and we discuss the relationship between the binary system and the overlapping steady extended source, TeV J2032+4130.
Ladattava julkaisu This is an electronic reprint of the original article. |  |
