Variable Very-High-Energy Gamma-Ray Emission from the Microquasar LS I +61 303

Albert, J.; Aliu, E.; Anderhub, H.; Antoranz, P.; Armada, A.; Asensio, M.; Baixeras, C.; Barrio, J. A.; Bartelt, M.; Bartko, H.; Bastieri, D.; Bavikadi, S. R.; Bednarek, W.; Berger, K.; Bigongiari, C.; Biland, A.; Bisesi, Erica; Böck, R.; Bordas, P.; Bosch‐Ramon, V.; Bretz, T.; Britvitch, I.; Cámara, Miguel; Carmona, E.; Chilingarian, A.; Ciprini, S.; Coarasa, J. A.; Commichau, S.; Contreras, J. L.; Cortina, J.; Curtef, V.; Danielyan, V.; Dazzi, F.; Angelis, A. De; Reyes, R. de los; Lotto, B. De; Domingo-Santamaría, E.; Dorner, D.; Doro, M.; Errando, M.; Fagiolini, M.; Ferenc, D.; Fernández, E.; Firpo, R.; Flix, J.; Fonseca, M. V.; Font, L.; Fuchs, M.; Galante, N.; Garczarczyk, M.; Gaug, M.; Giller, M.; Göebel, F.; Hakobyan, D.; Hayashida, M.; Hengstebeck, T.; Höhne, D.; Hose, J.; Hsu, C. C.; Isar, P. G.; Jacoń, P.; Kalekin, O.; Kosyra, R.; Kranich, D.; Laatiaoui, M.; Laille, A.; Lenisa, T.; Liebing, P.; Lindfors, E.; Lombardi, S.; Longo, F.; López, J.; López, M.; Lorenz, E.; Lucarelli, F.; Majumdar, P.; Maneva, G.; Mannheim, K.; Mansutti, O.; Mariotti, M.; Martı́nez, M.; Mase, K.; Mazin, D.; Merck, C.; Meucci, M.; Meyer, M.; Miranda, J. M.; Mirzoyan, R.; Mizobuchi, S.; Moralejo, A.; Nilsson, K.; Oña-Wilhelmi, E.; Orduña, R.; Otte, A. N.; Oya, I.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Pasanen, M.; Pascoli, D.; Pauß, F.; Pavel, N.; Pegna, R.; Peršić, M.; Peruzzo, L.; Piccioli, A.; Pöller, M.; Pooley, G. G.; Prandini, E.; Raymers, A.; Rhode, W.; Ribó, M.; Rico, J.; Riegel, B.; Rissi, M.; Robert, A.; Romero, Gustavo E.; Rügamer, S.; Saggion, A.; Sánchez, A.; Sartori, P.; Scalzotto, V.; Scapin, V.; Schmitt, R.; Schweizer, T.; Shayduk, M.; Shinozaki, K.; Shore, S. N.; Sidro, N.; Sillanpää, A.; Sobczyńska, D.; Stamerra, A.; Stark, L. S.; Takalo, L. O.; Temnikov, P.; Tescaro, D.; Teshima, M.; Tonello, N.; Torres, A. de; Torres, D. F.; Turini, N.; Vankov, H.; Vitale, V.; Wagner, R. M.; Wibig, T.; Wittek, W.; Zanin, R.; Zapatero, J.

doi:10.1126/science.1128177

Cited by 405 publications

(376 citation statements)

References 32 publications

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“…It is asserted that if these events take place in a region of the orbit where a large fraction of stellar UV photons is present, gamma-ray emission can take place via inverse Compton scattering of energetic jet electrons off this photon population. Recently, the MAGIC collaboration has detected VHE gamma-ray emission between φ= 0.4 and 0.7, which is consistent with the previous multi-wavelength results [5].…”

Section: Ls I +6303 As a Vhe Emittersupporting

confidence: 80%

“…Upper limits were derived for all orbital phases and are shown in figure 3 in terms of flux from the Crab Nebula during the same observational period. While the limits derived for the orbital phases of 0.1→0.8 are less stringent than the ones derived in [5] the MAGIC result did not include any coverage in the phase bins of 0→0.1, and 0.8→1. The Whipple upper limits for these phase bins therefore serve as a constraint on the system emission in the phases in which it is most likely quiescent.…”

Section: Observational Resultsmentioning

confidence: 74%

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Whipple telescope observations of LS I +61 303: 2004–2006

Smith

Atkins

Bradbury

et al. 2007

Astrophys Space Sci

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Section: Ls I +6303 As a Vhe Emittersupporting

confidence: 80%

Section: Observational Resultsmentioning

confidence: 74%

Whipple telescope observations of LS I +61 303: 2004–2006

Smith

Atkins

Bradbury

et al. 2007

Astrophys Space Sci

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“…In fact, some sources observed by the Energetic Gamma Ray Experiment Telescope (EGRET) have already been suggested to be associated with high mass X-ray binaries (HMXBs): A0535+26 (Romero et al 2001), LS I +61 • 303 (Kniffen et al 1997), Cyg X-3 (Mori et al 1997), LS 5039 (Paredes et al 2000). Moreover, very high energy γ-ray emission was recently detected from the microquasars LS 5039 (Aharonian et al 2005a) and LS I +61 • 303 (Albert et al 2006), and from the colliding wind Be-pulsar system PSR B1259-63 (Aharonian et al 2005b).…”

Section: Introductionmentioning

confidence: 99%

Very high energy γ-ray emission from X-ray transients during major outbursts

Orellana

Romero

Pellizza

et al. 2007

A&A

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Context. Some high mass X-ray binaries (HMXB) have been recently confirmed as γ-ray sources by ground based Cherenkov telescopes. In this work, we discuss the γ-ray emission from X-ray transient sources formed by a Be star and a highly magnetized neutron star. This kind of systems can produce variable hadronic γ-ray emission through the mechanism proposed by Cheng and Ruderman, where a proton beam accelerated in the pulsar magnetosphere impacts the transient accretion disk. We choose as case of study the best known system of this class: A0535+26. Aims. We aim at making quantitative predictions about the very high-energy radiation generated in Be-X ray binary systems with strongly magnetized neutron stars. Methods. We study the gamma-ray emission generated during a major X-ray outburst of a HMXB adopting for the model the parameters of A0535+26. The emerging photon signal from the disk is determined by the grammage of the disk that modulates the optical depth. The electromagnetic cascades initiated by photons absorbed in the disk are explored, making use of the so-called "Approximation A" to solve the cascade equations. Very high energy photons induce Inverse Compton cascades in the photon field of the massive star. We implemented Monte Carlo simulations of these cascades, in order to estimate the characteristics of the resulting spectrum. Results. TeV emission should be detectable by Cherenkov telescopes during a major X-ray outburst of a binary formed by a Be star and a highly magnetized neutron star. The γ-ray light curve is found to evolve in anti-correlation with the X-ray signal.

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“…3EG J2016+3657 [15], (2) PWN, suggested both from studying the Crab offpulse emission [16], as well as from numerous positional coincidences between energetic pulsars and unidentified gamma-ray sources, and (3) Microquasars, as impressively confirmed by the detection of LS5039 with H.E.S.S. [17] (possible associated with 3EG J1824-1514) and LSI 61 • 303 with MAGIC [18] (possible associated with 3EG J0241+6103). Since the H.E.S.S.…”

Section: Contributed To the Multi-messenger Approach To Unidentified mentioning

confidence: 84%

Demystifying an unidentified EGRET source by VHE gamma-ray observations

Reimer

Funk

2007

The Multi-Messenger Approach to High-Energy Gamma-Ray Sources

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In a novel approach in observational highenergy gamma-ray astronomy, observations carried out by imaging atmospheric Cherenkov telescopes provide necessary templates to pinpoint the nature of intriguing, yet unidentified EGRET gamma-ray sources. Using GeV-photons detected by CGRO EGRET and taking advantage of high spatial resolution images from H.E.S.S. observations, we were able to shed new light on the EGRET observed gamma-ray emission in the Kookaburra complex, whose previous coverage in the literature is somewhat contradictory. 3EG J1420-6038 very likely accounts for two GeV gamma-ray sources (E > 1 GeV), both in positional coincidence with the recently reported pulsar wind nebulae (PWN) by HESS in the Kookaburra/Rabbit complex. PWN associations at VHE energies, supported by accumulating evidence from observations in the radio and X-ray band, are indicative for the PSR/plerionic origin of spatially coincident, but still unidentified Galactic gamma-ray sources from EGRET. This not only supports the already suggested connection between variable, but unidentified low-latitude gamma-ray sources with pulsar wind nebulae (3EG J1420-6038 has been suggested as PWN candidate previoulsy), it also documents the ability of resolving apparently confused EGRET sources by connecting the GeV emission as measured from a large-aperture space-based gamma-ray instrument with narrow field-of-view but superior spatial resolution observations by ground-based atmospheric Cherenkov tele-

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Variable Very-High-Energy Gamma-Ray Emission from the Microquasar LS I +61 303

Cited by 405 publications

References 32 publications

Whipple telescope observations of LS I +61 303: 2004–2006

Whipple telescope observations of LS I +61 303: 2004–2006

Very high energy γ-ray emission from X-ray transients during major outbursts

Demystifying an unidentified EGRET source by VHE gamma-ray observations

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