Limits on radio emission from pulsar wind nebulae

Gaensler, B. M.; Stappers, B. W.; Frail, D. A.; Moffett, D. A.; Johnston, Scott M.; Chatterjee, Sabyasachi

doi:10.1046/j.1365-8711.2000.t01-1-03626.x

Cited by 42 publications

(65 citation statements)

References 35 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…From the new image no evidence is found, down to the noise level of our data, for the radio counterpart to either the X-ray PWN or the surrounding radio shell associated with its host SNR. There are many pulsars for which the search of radio PWNe yielded negative results (e.g., Gaensler et al 2000;Giacani et al 2009Giacani et al , 2014. In these cases, the failure to detect the nebular emission has been explained as a consequence of two main physical conditions based on either a high magnetic field that inhibits the production of synchrotron radiation at longer wavelengths or severe adiabatic losses that occur in young and energetic pulsars lying in a very low ambient density (∼0.003 cm −3 ).…”

Section: Resultsmentioning

confidence: 99%

Unveiling the origin of HESS J1809−193

Castelletti

Giacani

Petriella

2016

A&A

View full text Add to dashboard Cite

Aims. The main goal of this paper is to provide new insights on the origin of the observable flux of γ rays from HESS J1809−193 using new high-quality observations in the radio domain. Methods. We used the Expanded Very Large Array (now known as the Karl G. Jansky Very large Array, JVLA) to produce a deep full-synthesis imaging at 1.4 GHz of the vicinity of PSR J1809−1917. These data were used in conjunction with 12 CO observations from the James Clerk Maxwell Telescope in the transition line J = 3−2 and atomic hydrogen data from the Southern Galactic Plane Survey to investigate the properties of the interstellar medium in the direction of the source HESS J1809−193. Results. The new radio continuum image, obtained with a synthesized beam of 8 × 4 and a sensitivity of 0.17 mJy beam −1 , reveals with unprecedented detail all the intensity structures in the field. No radio counterpart to the observed X-ray emission supposed to be a pulsar wind nebula powered by PSR J1809−1917 is seen in the new JVLA image. We discovered a system of molecular clouds on the edge of the supernova remnant (SNR) G11.0−0.0 shock front, which is positionally coincident with the brightest part of the TeV source HESS J1809−193. We determine, on the basis of kinematic and morphological evidences, a physical link of the SNR with the clouds for which we estimated a total (molecular plus atomic) mass of ∼3 × 10 3 M and a total proton density in the range 2-3 × 10 3 cm −3 . Conclusions. We propose as the most likely origin of the very high-energy γ-ray radiation from HESS J1809−193 a hadronic mechanism through collisions of ions accelerated at the SNR G11.0−0.0 shock with the molecular matter in the vicinity of the remnant.

show abstract

Section: Resultsmentioning

confidence: 99%

Unveiling the origin of HESS J1809−193

Castelletti

Giacani

Petriella

2016

A&A

View full text Add to dashboard Cite

show abstract

“…R99 suggested that the K3 site, a ∼ 20 mJy enhancement above the general flux in G313.6+0.3, was the radio counterpart to AX J1420.1-6049. Assuming a typical radio PWN spectral index α = −0.3, Gaensler et al (2000) note the fraction ǫ of the spin-down energy which goes into radio emission is related to the 20 cm flux density by S 20cm ≈ 3.3 × 10 6 ǫĖ 37 /(d/8kpc) 2 mJy. This suggests an efficiency ǫ ∼ 6 × 10 −6 at a distance of 8 kpc which is rather low compared to most other detected radio PWN (Frail & Scharringhausen 1997;Gaensler et al 2000), and would be even lower if the true distance is closer.…”

Section: Discussionmentioning

confidence: 99%

Multiwavelength Studies of PSR J1420−6048, a Young Pulsar in the Kookaburra

Roberts

Romani

Johnston

2001

The Astrophysical Journal

View full text Add to dashboard Cite

We present X-ray, radio, and infrared observations of the 68 ms pulsar PSR J1420−6048 and its surrounding nebula, a possible counterpart of the γ−ray source GeV J1417−6100/3EG J1420−6038. Pulsed X-ray emission at the radio period is marginally detected by ASCA from a source embedded in the hard spectrum X-ray nebula AX J1420.1−6049. At radio wavelengths, the pulsar is found to be strongly linearly and circularly polarized, and the polarization sweep is measured. A comparison of high resolution ATCA radio imaging of the Kookaburra's upper wing (G313.6+0.3), which contains the pulsar and the X-ray nebula, with infrared images suggests the radio emission is partly non-thermal.

show abstract

“…Very recently, two different objects were proposed by different groups, as being 1RXS J170849-400910 IR counterpart, and there still is an open debate on which one is the AXP counterpart (Israel et al 2003b;Safi-Harb and West 2005;Durant and van Kerkwijk 2006). A diffuse (∼8 ) radio emission at 1.4 GHz was recently reported, possibly associated with the supernova remnant G346.5-0.1 (Gaensler et al 2000).…”

Section: Introductionmentioning

confidence: 99%

X-ray intensity-hardness correlation and deep IR observations of the anomalous X-ray pulsar 1RXS J170849-400910

Rea

Israel

Oosterbroek³

et al. 2007

Astrophys Space Sci

View full text Add to dashboard Cite

We report here on X-ray and IR observations of the Anomalous X-ray Pulsar (AXP) 1RXS J170849-400910. First, we report on new XMM-Newton, Swift-XRT and Chandra observations of this AXP, which confirm the intensity-hardness correlation observed in the long term Xray monitoring of this source. These new X-ray observations show that the AXP flux is rising again, and the spectrum hardening. If the increase of the source intensity is indeed connected with the glitches and a possible bursting activity, we expect this source to enter in a bursting active

show abstract

Limits on radio emission from pulsar wind nebulae

Cited by 42 publications

References 35 publications

Unveiling the origin of HESS J1809−193

Unveiling the origin of HESS J1809−193

Multiwavelength Studies of PSR J1420−6048, a Young Pulsar in the Kookaburra

X-ray intensity-hardness correlation and deep IR observations of the anomalous X-ray pulsar 1RXS J170849-400910

Contact Info

Product

Resources

About