MAGIC Observations of the Unidentified γ-Ray Source TeV J2032+4130

Albert, J.; Aliu, E.; Anderhub, H.; Antoranz, P.; Baixeras, C.; Barrio, J. A.; Bartko, H.; Bastieri, D.; Becker, J.; Bednarek, W.; Berger, K.; Bigongiari, C.; Biland, A.; Böck, R.; Bonnoli, G.; Bordas, P.; Bosch‐Ramon, V.; Bretz, T.; Britvitch, I.; Cámara, Miguel; Carmona, E.; Chilingarian, A.; Commichau, S.; Contreras, J. L.; Cortina, J.; Costado, M. T.; Curtef, V.; Dazzi, F.; Angelis, A. De; Mendez, C. Delgado; Reyes, R. de los; Domingo-Santamaría, E.; Lotto, B. De; María, Mónica; Sabata, F. De; Dorner, D.; Doro, M.; Errando, M.; Fagiolini, M.; Ferenc, D.; Fernández, E.; Firpo, R.; Fonseca, M. V.; Font, L.; Galante, N.; García-López, R. J.; Garczarczyk, M.; Gaug, M.; Göebel, F.; Hayashida, M.; Herrero, A.; Höhne, D.; Hose, J.; Hsu, C. C.; Huber, Stefan; Jogler, T.; Kosyra, R.; Kranich, D.; Laille, A.; Leonardo, E.; Lindfors, E.; Lombardi, S.; Longo, F.; López, M.; Lorenz, E.; Majumdar, P.; Maneva, G.; Mankuzhiyil, N.; Mannheim, K.; Mariotti, M.; Martı́nez, M.; Mazin, D.; Merck, C.; Meucci, M.; Meyer, M.; Miranda, J. M.; Mirzoyan, R.; Mizobuchi, S.; Moralejo, A.; Nieto, D.; Nilsson, K.; Ninković, J.; Oña-Wilhelmi, E.; Otte, A. N.; Oya, I.; Panniello, M.; Paoletti, R.; Paredes, J. M.; Pasanen, M.; Pascoli, D.; Pauß, F.; Pegna, R.; Peršić, M.; Peruzzo, L.; Piccioli, A.; Prandini, E.; Puchades, N.; Raymers, A.; Rhode, W.; Ribó, M.; Rico, J.; Rissi, M.; Robert, Aymeric; Rügamer, S.; Saggion, A.; Saito, Takayuki; 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.; Spanier, F.; Stamerra, A.; Stark, L. S.; Takalo, L. O.; Temnikov, P.; Tescaro, D.; Teshima, M.; Torres, D. F.; Turini, N.; Vankov, H.; Venturini, A.; Vitale, V.; Wagner, R. M.; Wittek, W.; Zandanel, F.; Zanin, R.; Zapatero, J.

doi:10.1086/529520

Cited by 74 publications

(55 citation statements)

References 30 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…However, a critical analysis of these observations raised doubts about their validity (Chardin & Gerbier 1989), and in recent years the more sensitive instruments have not confirmed those claims for energies above 500 GeV (Schilling et al 2001;Albert et al 2008a). Nevertheless, microquasars are believed to produce a very high energy (VHE) emission inside the jets: high density and magnetic fields provided by the accretion disk and by the companion star create favorable conditions for effective production of γ rays (Levinson & Blandford 1996;Romero et al 2003;Bosch-Ramon et al 2006).…”

Section: Introductionmentioning

confidence: 99%

MAGIC CONSTRAINTS ON Γ-Ray EMISSION FROM CYGNUS X-3

Aleksić

Antonelli

Antoranz

et al. 2010

ApJ

Self Cite

View full text Add to dashboard Cite

Cygnus X-3 is a microquasar consisting of an accreting compact object orbiting around a Wolf-Rayet star. It has been detected at radio frequencies and up to high-energy γ rays (above 100 MeV). However, many models also predict a very high energy (VHE) emission (above hundreds of GeV) when the source displays relativistic persistent jets or transient ejections. Therefore, detecting such emission would improve the understanding of the jet physics. The imaging atmospheric Cherenkov telescope MAGIC observed Cygnus X-3 for about 70 hr between 2006 March 843 844 ALEKSIĆ ET AL.Vol. 721and 2009 August in different X-ray/radio spectral states and also during a period of enhanced γ -ray emission. MAGIC found no evidence for a VHE signal from the direction of the microquasar. An upper limit to the integral flux for energies higher than 250 GeV has been set to 2.2 × 10 −12 photons cm −2 s −1 (95% confidence level). This is the best limit so far to the VHE emission from this source. The non-detection of a VHE signal during the period of activity in the high-energy band sheds light on the location of the possible VHE radiation favoring the emission from the innermost region of the jets, where absorption is significant. The current and future generations of Cherenkov telescopes may detect a signal under precise spectral conditions.

show abstract

Section: Introductionmentioning

confidence: 99%

MAGIC CONSTRAINTS ON Γ-Ray EMISSION FROM CYGNUS X-3

Aleksić

Antonelli

Antoranz

et al. 2010

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…One possibility is that the void is formed due to the collective action of powerful stellar winds from an association of massive stars, a hypothesis considered by Butt et al (2003) and Albert et al (2008). They argued that the presence of a large, mechanical power density from the stellar winds of the OB stars, make Cygnus OB2 a prime candidate for the investigation of the stellar wind hypothesis for the acceleration of Galactic cosmic rays.…”

Section: Multiwavelength Properties and Interpretationsmentioning

confidence: 99%

“…Based on observations carried out by Whipple in 2003-05, and assuming a spectral shape the same as that of the Crab nebula, it was later reported to be 8% of the Crab nebula flux (Konopelko et al 2007). The MAGIC collaboration, too, has reported a deep exposure of this region (Albert et al 2008). The MAGIC collaboration has also found the source to be extended, with an integral flux and spectral index comparable to that measured by HEGRA.…”

Section: Introductionmentioning

confidence: 99%

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

Aliu

Aune

Behera³

et al. 2014

ApJ

Self Cite

View full text Add to dashboard Cite

TeV J2032+4130 was the first unidentified source discovered at very high energies (VHEs; E > 100 GeV), with no obvious counterpart in any other wavelength. It is also the first extended source to be observed in VHE gamma rays. Following its discovery, intensive observational campaigns have been carried out in all wavelengths in order to understand the nature of the object, which have met with limited success. We report here on a deep observation of TeV J2032+4130 based on 48.2 hr of data taken from 2009 to 2012 by the Very Energetic Radiation Imaging Telescope Array System experiment. The source is detected at 8.7 standard deviations (σ ) and is found to be extended and asymmetric with a width of 9. 5 ± 1. 2 along the major axis and 4. 0 ± 0. 5 along the minor axis. The spectrum is well described by a differential power law with an index of 2.10 ± 0.14 stat ± 0.21 sys and a normalization of (9.5 ± 1.6 stat ± 2.2 sys ) × 10 −13 TeV −1 cm −2 s −1 at 1 TeV. We interpret these results in the context of multiwavelength scenarios which particularly favor the pulsar wind nebula interpretation.

show abstract

“…All instruments find a power-law spectrum consistent with Γ = 2.1, although there appears to be some disagreement between VERITAS and MAGIC as to the flux normalization [56,57]. No measurement thus far has found evidence for either an energy-dependent morphology of the source or a spectral cutoff up to 20 TeV, although current measurements are not highly constraining in either case [56,57].Based on deep VERITAS observations of TeV J2032+4130, Aliu et al[57] strongly suggest that TeV J2032+4130 is a relic PWN powered by the co-located gamma-ray pulsar PSR J2032+4127 [50]. Uncertainties in the estimate of the pulsar's distance raise questions about TeV J2032+4130's relationship to other structures in Cygnus-X.…”

mentioning

confidence: 91%

“…Subsequent observations by the IACT observatories MAGIC and VERITAS have confirmed the extension of the source and provided more precise measurements of its spectrum. All instruments find a power-law spectrum consistent with Γ = 2.1, although there appears to be some disagreement between VERITAS and MAGIC as to the flux normalization [56,57]. No measurement thus far has found evidence for either an energy-dependent morphology of the source or a spectral cutoff up to 20 TeV, although current measurements are not highly constraining in either case [56,57].…”

mentioning

confidence: 99%

Pulsar Wind Nebulae and Cosmic Rays: A Bedtime Story

Weinstein¹

2014

Nuclear Physics B - Proceedings Supplements

View full text Add to dashboard Cite

The role pulsar wind nebulae play in producing our locally observed cosmic ray spectrum remains murky, yet intriguing. Pulsar wind nebulae are born and evolve in conjunction with SNRs, which are favored sites of Galactic cosmic ray acceleration. As a result they frequently complicate interpretation of the gamma-ray emission seen from SNRs. However, pulsar wind nebulae may also contribute directly to the local cosmic ray spectrum, particularly the leptonic component. This paper reviews the current thinking on pulsar wind nebulae and their connection to cosmic ray production from an observational perspective. It also considers how both future technologies and new ways of analyzing existing data can help us to better address the relevant theoretical questions. A number of key points will be illustrated with recent results from the VHE (E > 100 GeV) gamma-ray observatory VERITAS. Keywords: IntroductionThe discovery of cosmic rays in the early twentieth century [1, 2] inaugurated a decades-long, serialized mystery story that has yet to be completed. At the heart of the mystery lies a set of of simple questions. What particles appear in the cosmic ray spectrum that we see from Earth? Where do these particles originate? How are they accelerated? In recent decades direct cosmic ray observations have brought us a wealth of information on the cosmic ray spectrum and its composition, clues to the types of environments in which cosmic rays are born. The interaction of these particles with interstellar magnetic fields, however, prevents them from being traced back to their point of origin.In order to pursue the other half of this mystery-the nature of cosmic ray accelerators-we must use the secondary photon radiation produced in these cosmic ray nurseries. These high-energy (300 MeV -100 GeV) and very high-energy (VHE; E > 100 GeV) gamma rays are not deflected by interstellar magnetic fields and can be used to map cosmic ray populations in and near their parent accelerators. The different processes by which relativistic cosmic ray electrons, protons, and heavier nuclei produce high-energy gamma rays leave characteristic imprints on the gamma-ray energy spectrum of particular astrophysical accelerators. These features may be used to constrain the composition and energy spectrum of accelerated particle populations.The local cosmic ray spectrum is known to be a mix of protons and heavier nuclei, with a smaller admixture of leptons. A mix of astrophysical accelerators within and outside our Galaxy is believed to contribute, including shocks arising in supernova remnants (SNRs), shocks formed by interacting high-velocity winds from massive stars [3], pulsars, and active galactic nuclei (AGN). We focus here on a single subplot of a much larger story-the role played by pulsar wind nebulae (PWNe) in our quest to understand the Galactic cosmic ray spectrum. Dramatis PersonaeNo single gamma-ray observatory provides a complete picture of the gamma-ray sky at all energies and spatial scales. The Fermi Gamma-ray Space Telescope (...

show abstract

MAGIC Observations of the Unidentified γ-Ray Source TeV J2032+4130

Cited by 74 publications

References 30 publications

MAGIC CONSTRAINTS ON Γ-Ray EMISSION FROM CYGNUS X-3

MAGIC CONSTRAINTS ON Γ-Ray EMISSION FROM CYGNUS X-3

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

Pulsar Wind Nebulae and Cosmic Rays: A Bedtime Story

Contact Info

Product

Resources

About