OBSERVATIONS OF THE UNIDENTIFIED GAMMA-RAY SOURCE TeV J2032+4130 BY VERITAS

Aliu, E.; Aune, T.; Behera, B.; Beilicke, M.; Benbow, W.; Berger, K.; Bird, R.; Buckley, J. H.; Bugaev, V.; Cardenzana, J. V.; Cerruti, M.; Chen, X.; Ciupik, L.; Connolly, Michael; Cui, Wei; Duke, C.; Dumm, J.; Errando, M.; Falcone, A.; Federici, S.; Feng, Q.; Finley, J. P.; Fortin, P.; Fortson, L.; Furniss, A.; Galante, N.; Gillanders, G. H.; Griffin, S.; Griffiths, S.; Grube, J.; Gyuk, G.; Hanna, D.; Holder, J.; Hughes, G.; Humensky, T. B.; Kaaret, Philip; Kargaltsev, Oleg; Kertzman, M.; Khassen, Y.; Kieda, D.; Krawczynski, H.; Lang, M. J.; Madhavan, A. S.; Maier, G.; Majumdar, P.; McCann, A.; Moriarty, P.; Mukherjee, R.; Nieto, D.; Bhróithe, A. O'Faoláin De; Ong, R. A.; Otte, A. N.; Pandel, D.; Perkins, J. S.; Pohl, M.; Popkow, A.; Prokoph, H.; Quinn, J.; Ragan, K.; Rajotte, Jean-François; Reyes, Luis; Reynolds, P. T.; Richards, G.; Roache, E.; Sembroski, G. H.; Skole, C.; Staszak, D.; Telezhinsky, I.; Theiling, M.; Tucci, J. V.; Tyler, J.; Varlotta, A.; Vincent, S.; Wakely, S. P.; Weekes, T. C.; Weinstein, A. J.R.; Welsing, R.; Williams, D. A.; Zitzer, B.

doi:10.1088/0004-637x/783/1/16

Cited by 65 publications

(60 citation statements)

References 41 publications

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“…A possible TeV counterpart of this binary system, TeV J2032+4130, was one of the first sources ever detected at TeV energies and the first TeV source with no obvious counterpart at other wavelengths (Aharonian et al 2002). The source, however, exhibits a steady TeV flux with no evidence of periodic behaviour and was at first suggested to be the evolved pulsar wind nebula of PSR J2032+4127 (Aliu et al 2014, and references therein). The recent discovery that the pulsar is in a ∼ 30 year orbit around MT91 213, and is expected to pass through periastron by the end of 2017, challenges the current interpretation (Lyne et al 2015;Ho et al 2017).…”

Section: Introductionmentioning

confidence: 93%

Gamma–Gamma Absorption in the γ-ray Binary System PSR B1259-63/LS 2883

Sushch

Soelen

2017

ApJ

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The observed TeV light curve from the γ-ray binary PSR B1259-63/LS 2883 shows a decrease in the flux at periastron which has not been fully explained by emission mechanisms alone. This observed decrease can, however, be explained by γγ absorption due to the stellar and disk photons. We calculate the γγ absorption in PSR B1259-63/LS 2883 taking into account photons from both the circumstellar disk and star, assuming the γ rays originate at the position of the pulsar. The γγ absorption due to the circumstellar disk photons produces a ≈ 14% decrease in the flux, and there is a total decrease of ≈ 52% (> 1 TeV) within a few days before periastron, accompanied by a hardening of the γ-ray photon index. While the γγ absorption alone is not sufficient to explain the full complexity of the H.E.S.S. γ-ray light curve it results in a significant decrease in the predicted flux, which is co-incident with the observed decrease. In addition, we have calculated an upper-limit on the γγ absorption, assuming that the emission is produced at the apex of the bow shock. Future observations with CTA during the 2021 periastron passage may be able to confine the location of the emission based on the degree of γγ absorption as well as measure the hardening of the spectrum around periastron.

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Section: Introductionmentioning

confidence: 93%

Gamma–Gamma Absorption in the γ-ray Binary System PSR B1259-63/LS 2883

Sushch

Soelen

2017

ApJ

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“…Co-located with J2032 is the extended VHE gamma-ray source TeV J2032+4130, which has remained an unidentified object despite thirteen years of observations since its discovery. That TeV J2032+4130 is an extended galactic object at VHEs would typically implicate the presence of a PWN as suggested in [13], though this interpretation has been questioned due to the considerably hard VHE spectrum and the recently identified binary.…”

Section: Veritas Observations Of the Binary System Psr J2032+4127/mt9mentioning

confidence: 97%

Recent Galactic Science Results from VERITAS on Pulsar Searches, PSR J2032+4127, and HAWC Follow-Ups

Richards¹

2017

Proceedings of 7th International Fermi Symposium — PoS(IFS2017)

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VERITAS is a ground-based imaging atmospheric Cherenkov telescope array sensitive to very high energy (VHE, E > 100 GeV) gamma rays. VERITAS has detected VHE gamma-ray emission from nearly 60 astrophysical sources of varied source classes. One of the primary areas of research of VERITAS is the study of galactic particle accelerators, and among the classes of galactic objects investigated are pulsars, binary systems, and pulsar wind nebulae. In this contribution, recent results from VERITAS on the three aforementioned source classes will be presented, including: results from a search for pulsed emission from 14 young pulsars appearing in archival VERITAS data; observations of the binary system PSR J2032+4127/MT91 213, which is quickly approaching its periastron passage set to occur in 2017 November; and follow-up observations of new VHE gamma-ray sources detected by the HAWC observatory. These VERITAS observations will provide insight into the particle acceleration and radiation mechanisms at work in these galactic objects.7th Fermi Symposium 2017

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“…The HEGRA TeV γ-ray source (TeV J2032+4130 [7]) has the extension of ∼6', and the flux of 5% of the Crab Nebula [29,8,9,30,31]. The nature of the HEGRA TeV source remains unclear.…”

Section: Tev γ-Rays From the Binary Containing Psr 2032+4127mentioning

confidence: 99%

“…Those authors discuss the Inverse Compton (IC) γ-ray emission in the context of the wind collision model for the massive binary systems. The observations of the binary system PSR J2032+4127/MT91 213 in the TeV γ-ray energy range are expected to be more difficult since in the direction of this binary an extended, steady TeV γ-ray source (TeV J2032+4130) has been discovered [7] (and confirmed in [8,9]). Applying the available parameters of the binary system, PSR J2032+4127/MT91 213, we present detailed calculations of the GeV-TeV γ-ray radiation expected from this binary close to the periastron passage of the pulsar.…”

Section: Introductionmentioning

confidence: 99%

Gamma-rays from comptonization of stellar radiation in the binary system containing PSR J2032+4127 at its periastron passage

Bednarek¹,

Banasiński²

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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We calculate the high energy gamma-ray emission expected during the periastron passage of the pulsar PSR J2032+4127 which form extended binary system with the massive companion star MT91 213. The γ-ray emission is expected due to the comptonization of the stellar radiation by electrons accelerated at the pulsar wind and stellar wind collision shock. We apply the numerical code for the cascade process initiated by electrons in the anisotropic radiation from the companion star. We conclude that around the periastron passage of this binary system, the γ-ray emission at TeV energies can overcome the TeV emission observed from an extended source in this direction which is likely due to the pulsar wind nebula formed by the pulsar PSR J2032+4127. We discuss the conditions within the binary system for which such a point like TeV γ-ray source should appear in addition to the presently observed the extended TeV γ-ray source.

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OBSERVATIONS OF THE UNIDENTIFIED GAMMA-RAY SOURCE TeV J2032+4130 BY VERITAS

Cited by 65 publications

References 41 publications

Gamma–Gamma Absorption in the γ-ray Binary System PSR B1259-63/LS 2883

Gamma–Gamma Absorption in the γ-ray Binary System PSR B1259-63/LS 2883

Recent Galactic Science Results from VERITAS on Pulsar Searches, PSR J2032+4127, and HAWC Follow-Ups

Gamma-rays from comptonization of stellar radiation in the binary system containing PSR J2032+4127 at its periastron passage

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