Periastron Observations of TeV Gamma-Ray Emission from a Binary System with a 50-year Period
Ramazani VF; Acciari VA; Maraschi L; Lamastra A; Giammaria P; Hahn A; Prester DD; Paoletti R; Besenrieder J; Colin P; Noda K; Bonnoli G; Ishio K; Sitarek J; Maneva G; Moreno V; Saito T; Schlenstedt S; Babic A; Berti A; Mukherjee R; Bird R; Gent A; Guberman D; Fernandez-Barral A; Saha L; Neustroev V; Font L; Chromey AJ; Biland A; Pueschel E; Longo F; Tavecchio F; Garcia JR; Hughes G; Gaug M; Delfino M; Paredes JM; Moretti E; Manganaro M; Snidaric I; Dorner D; Ferrara G; Zitzer B; Satalecka K; Puljak I; Krennrich F; Antonelli LA; Nigro C; Furniss A; Bigongiari C; Wilcox P; Busetto G; Doro M; Bernardini E; Lin TTY; Lopez RJG; Hrupec D; Majumdar P; Molina E; Williamson TJ; Sembroski GH; Fidalgo D; Covino S; Fattorini A; Peresano M; Espinera ED; Barrio JA; Daniel MK; Niedzwiecki A; Kertzman M; Da Vela P; Hassan T; Righi C; Kaaret P; Carosi R; Cortina J; Nogues L; Sushch I; Lopez M; Bhattacharyya W; Garczarczyk M; Prandini E; Brose R; Hadasch D; Gallozzi S; Pohl M; Kar P; Fonseca MV; Fruck C; Blanch O; Park N; Gillanders GH; Santander M; Godinovic N; Penil P; Kumar S; Nothe M; Mirzoyan R; Richards GT; Paiano S; Roache E; Ninci D; Leone F; Contreras JL; Ceribella G; Mazin D; Colombo E; Kushida J; Inoue S; Nishijima K; Mannheim K; Williams DA; Strzys M; Moroni PGP; Lelas D; Sobczynska D; Buckley JH; Abeysekara AU; Weinstein A; Vassiliev VV; van Scherpenberg J; Iwamura Y; Persic M; Suric T; Fortson L; Vanzo G; Tsujimoto S; Palacio J; Wilhelm A; Petrashyk A; Delgado J; Bednarek W; Kubo H; Rhode W; Vovk I; Stamerra A; Makariev M; Teshima M; Miranda JM; Ansoldi S; Schweizer T; Munar-Adrover P; Elsaesser D; De Angelis A; Kieda D; Pedaletti G; Engels AA; Wells RM; Wakely SP; Foffano L; Tyler J; Banerjee B; Hoang J; Sadeh I; Holder J; Somero A; Cikota S; Ribo M; De Lotto B; Paneque D; Brill A; Lang MJ; Baack D; Torres-Alba N; de Almeida UB; Falcone A; Einecke S; Lindfors E; Rugliancich A; Will M; Galindo D; Dominguez A; Kuvezdic D; Temnikov P; Fraga BMD; Lombardi S; Colak SM; Krause M; Herrera J; Maier G; Lopez-Oramas A; Otte AN; Gonzalez JB; Gasparyan S; Rosillo MN; Masuda S; Moralejo A; Finley JP; Dazzi F; Maggio C; Benbow W; Hanna D; Minev M; Ong RA; Terzic T; Zaric D; Mariotti M; D'Elia V; Ragan K; Di Pierro F; Mallamaci M; Quinn J; Acosta MV; Hervet O; Martinez M; Sahakyan N; Humensky TB; Moriarty P; O'Brien S; Nilsson K; Rico J
Periastron Observations of TeV Gamma-Ray Emission from a Binary System with a 50-year Period
Ramazani VF
Acciari VA
Maraschi L
Lamastra A
Giammaria P
Hahn A
Prester DD
Paoletti R
Besenrieder J
Colin P
Noda K
Bonnoli G
Ishio K
Sitarek J
Maneva G
Moreno V
Saito T
Schlenstedt S
Babic A
Berti A
Mukherjee R
Bird R
Gent A
Guberman D
Fernandez-Barral A
Saha L
Neustroev V
Font L
Chromey AJ
Biland A
Pueschel E
Longo F
Tavecchio F
Garcia JR
Hughes G
Gaug M
Delfino M
Paredes JM
Moretti E
Manganaro M
Snidaric I
Dorner D
Ferrara G
Zitzer B
Satalecka K
Puljak I
Krennrich F
Antonelli LA
Nigro C
Furniss A
Bigongiari C
Wilcox P
Busetto G
Doro M
Bernardini E
Lin TTY
Lopez RJG
Hrupec D
Majumdar P
Molina E
Williamson TJ
Sembroski GH
Fidalgo D
Covino S
Fattorini A
Peresano M
Espinera ED
Barrio JA
Daniel MK
Niedzwiecki A
Kertzman M
Da Vela P
Hassan T
Righi C
Kaaret P
Carosi R
Cortina J
Nogues L
Sushch I
Lopez M
Bhattacharyya W
Garczarczyk M
Prandini E
Brose R
Hadasch D
Gallozzi S
Pohl M
Kar P
Fonseca MV
Fruck C
Blanch O
Park N
Gillanders GH
Santander M
Godinovic N
Penil P
Kumar S
Nothe M
Mirzoyan R
Richards GT
Paiano S
Roache E
Ninci D
Leone F
Contreras JL
Ceribella G
Mazin D
Colombo E
Kushida J
Inoue S
Nishijima K
Mannheim K
Williams DA
Strzys M
Moroni PGP
Lelas D
Sobczynska D
Buckley JH
Abeysekara AU
Weinstein A
Vassiliev VV
van Scherpenberg J
Iwamura Y
Persic M
Suric T
Fortson L
Vanzo G
Tsujimoto S
Palacio J
Wilhelm A
Petrashyk A
Delgado J
Bednarek W
Kubo H
Rhode W
Vovk I
Stamerra A
Makariev M
Teshima M
Miranda JM
Ansoldi S
Schweizer T
Munar-Adrover P
Elsaesser D
De Angelis A
Kieda D
Pedaletti G
Engels AA
Wells RM
Wakely SP
Foffano L
Tyler J
Banerjee B
Hoang J
Sadeh I
Holder J
Somero A
Cikota S
Ribo M
De Lotto B
Paneque D
Brill A
Lang MJ
Baack D
Torres-Alba N
de Almeida UB
Falcone A
Einecke S
Lindfors E
Rugliancich A
Will M
Galindo D
Dominguez A
Kuvezdic D
Temnikov P
Fraga BMD
Lombardi S
Colak SM
Krause M
Herrera J
Maier G
Lopez-Oramas A
Otte AN
Gonzalez JB
Gasparyan S
Rosillo MN
Masuda S
Moralejo A
Finley JP
Dazzi F
Maggio C
Benbow W
Hanna D
Minev M
Ong RA
Terzic T
Zaric D
Mariotti M
D'Elia V
Ragan K
Di Pierro F
Mallamaci M
Quinn J
Acosta MV
Hervet O
Martinez M
Sahakyan N
Humensky TB
Moriarty P
O'Brien S
Nilsson K
Rico J
IOP PUBLISHING LTD
Julkaisun pysyvä osoite on:
https://urn.fi/URN:NBN:fi-fe2021042720185
https://urn.fi/URN:NBN:fi-fe2021042720185
Tiivistelmä
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.
Kokoelmat
- Rinnakkaistallenteet [19207]