Corporation, propriété et capitalisme

Pineault, Éric

doi:10.1522/030275957

Cited by 4 publications

(9 citation statements)

References 1 publication

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“…Previous to Veritas observations, Zhang et al (2009) over-predicted the value of the flux at high energies. To model the radio upper limits these authors assumed that all the emission obtained from the images of Pineault et al (1997) was coming from the PWN, which caused also an over-estimation of the radio flux. In the model presented in Fig.…”

Section: Hess J1846-029 (Kes 75)mentioning

confidence: 99%

Time-dependent modeling of TeV-detected, young pulsar wind nebulae

Torres

Cillis

Martín

et al. 2014

Journal of High Energy Astrophysics

157

238

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The increasing sensitivity of instruments at X-ray and TeV energies have revealed a large number of nebulae associated to bright pulsars. Despite this large data set, the observed pulsar wind nebulae (PWNe) do not show a uniform behavior and the main parameters driving features like luminosity, magnetization, and others are still not fully understood. To evaluate the possible existence of common evolutive trends and to link the characteristics of the nebula emission with those of the powering pulsar, we selected a sub-set of 10 TeV detections which are likely ascribed to young PWNe and model the spectral energy distribution with a time-dependent description of the nebulae's electron population. In 9 of these cases, a detailed PWNe model, using up-to-date multiwavelength information, is presented. The best-fit parameters of these nebula are discussed, together with the pulsar characteristics. We conclude that TeV PWNe are particle-dominated objects with large multiplicities, in general far from magnetic equipartition, and that relatively large photon field enhancements are required to explain the high level of Comptonized photons observed. We do not find significant correlations between the efficiencies of emission at different frequencies and the magnetization. The injection parameters do not appear to be particularly correlated with the pulsar properties either. We find that a normalized comparison of the SEDs (e.g., with the corresponding spin-down flux) at the same age significantly reduces the spectral distributions dispersion.

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Section: Hess J1846-029 (Kes 75)mentioning

confidence: 99%

Time-dependent modeling of TeV-detected, young pulsar wind nebulae

Torres

Cillis

Martín

et al. 2014

Journal of High Energy Astrophysics

157

238

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“…Mavromatakis (2003) derive column densities that imply ISM densities of 0.5 cm −3 at the distance of 2 kpc and conclude, based on the properties of the optical emission, that an extended radio blob seen to the north of the SNR is probably unrelated to it, but perhaps associated to a bipolar HII region. This had also been concluded by Pineault et al (1996) after comparing the infrared properties of the SNR and the northern component, which are very different, as is the morphology of the HI gas in both regions. According to Mavromatakis (2003), the low ionization optical images further indicate an inhomogenous and patchy intestellar medium.…”

Section: Introductionmentioning

confidence: 62%

“…Lorimer et al (1998) cite the study by Lozinskaya et al (1993) and use a distance of 1.3 kpc. Pineault et al (1996) find an interesting HI region that shows a correlation with the remnant's morphology at a kinematic distance of 10 kpc, but this distance is probably less likely for G73.9+0.9. A distance closer to more recent estimates of 1.8 kpc is adopted here.…”

Section: Introductionmentioning

confidence: 82%

Modeling the Multiwavelength Emission From G73.9+0.9: Gamma Rays From an Snr–mc Interaction

Araya

2015

ApJ

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G73.9+0.9 has been classified as a probable shell-type supernova remnant (SNR), although it has also been suggested that this object could be a pulsar wind nebula (PWN). Here, a broadband model of the non-thermal emission of G73.9+0.9 from radio to gamma-rays is presented. The model includes a new gamma-ray observation obtained with analysis of 7 years of data from the Fermi LAT telescope. Above 200 MeV the source is detected with a significance of 13σ and the spectrum of the radiation is best described by a power law with an index of ∼2.5. The leptonic mechanisms are hard to reconcile with the measured radio and gamma-ray SED. A PWN origin for the high-energy emission is also not very likely, due to the lack of detection of pulsars and of X-ray emission in the region, as well as from the shape of the gamma-ray spectrum. Given the possibility that the object is interacting with molecular clouds, a hadronic origin of the high-energy emission is more likely, and the spectral properties of the cosmic rays responsible for this radiation are derived.Subject headings: acceleration of particles-radiation mechanisms: non-thermal-ISM: individual objects: G73.9+0.9-ISM: supernova remnants.

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“…This breakout phenomenon may be caused by more rapid expansion of the blast wave shock into a lower density region toward the NW. HI observations supported this interpretation (Pineault et al 1993(Pineault et al , 1997. The latter papers place the SNR at 1.4±0.3 kpc, the kinematic distance corresponding to the systemic velocity of a partial HI shell (−16 km/s) that the authors find to the NW.…”

Section: Cta 1: General Featuresmentioning

confidence: 73%

“…CTA 1 was subject of intense observational campaigns in the past years. There have been both ROSAT and ASCA X-ray observations (Seward et al 1995, Slane et al 1997, as well as optical, infrared and radio studies (see Pineault et al 1997 andBrazier et al 1998 for a review).…”

Section: Cta 1: General Featuresmentioning

confidence: 99%

Status of the Connection between Unidentified EGRET Sources and Supernova Remnants: The Case of CTA 1

Torres

Dame

Romero

Multiwavelength Approach to Unidentified Gamma-Ray Sources

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In this paper we briefly comment on the observational status of the possible physical association between unidentified EGRET sources and supernova remnants (SNRs) in our Galaxy. We draw upon recent results presented in the review by Torres et al. (Physics Reports, 2003), concerning molecular gas in the vicinity of all 19 SNRs found to be positionally coincident with EGRET sources at low Galactic latitudes. In addition, we present new results regarding the supernova remnant CTA 1. Our findings disfavor the possibility of a physical connection with the nearby (in projection) EGRET source. There remains possible, however, that the compact object produced in the supernova explosion be related with the observed γ-ray flux.

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Corporation, propriété et capitalisme

Cited by 4 publications

References 1 publication

Time-dependent modeling of TeV-detected, young pulsar wind nebulae

Time-dependent modeling of TeV-detected, young pulsar wind nebulae

Modeling the Multiwavelength Emission From G73.9+0.9: Gamma Rays From an Snr–mc Interaction

Status of the Connection between Unidentified EGRET Sources and Supernova Remnants: The Case of CTA 1

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