G106.3+2.7: A Supernova Remnant in a Late Stage of Evolution

Pineault, S.; Joncas, G.

doi:10.1086/316863

Cited by 50 publications

(63 citation statements)

References 18 publications

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“…Kothes et al (2006a) performed a multi-frequency analysis towards the PWN and found a spectral break at about 4.3 GHz. The overall spectral index of the whole SNR is α ∼ −0.6, while the compact "head" region has a flatter spectrum than the "tail" region (Pineault & Joncas 2000).…”

Section: G890+47 (Hb21)mentioning

confidence: 96%

“…3.9. G106.3+2.7 G106.3+2.7 is a comet-shaped SNR discovered by Joncas & Higgs (1990) from the DRAO northern Galactic plane survey at 408 MHz, and further studied by Pineault & Joncas (2000). The SNR consists of a compact "head" region containing an off-center PWN G106.6+2.9 in the north, the so-called "Boomerang" and a diffuse "tail" region (see Fig.…”

Section: G890+47 (Hb21)mentioning

confidence: 99%

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A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Han

Reich

et al. 2011

A&A

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Context.Observations of large supernova remnants (SNRs) at high frequencies are rare, but provide valuable information about their physical properties. Aims. The total intensity and polarization properties of 16 large SNRs in the Galactic plane are investigated based on observations of the Urumqi λ6 cm polarization survey of the Galactic plane with an angular resolution of 9. 5. Methods. We extracted total intensity and linear polarization maps of large SNRs from the Urumqi λ6 cm survey, obtained their integrated flux densities, and derived the radio spectra by using these flux densities together with previously published flux densities at various frequencies. In particular, Effelsberg λ11 cm and λ21 cm survey data were used to calculate integrated flux densities. The λ6 cm polarization data also delineate the magnetic field structures of the SNRs. Results. We present the first total intensity maps at λ6 cm for SNRs G106.3+2.7, G114.3+0.3, G116.5+1.1, G166.0+4.3 (VRO 42.05.01), G205.5+0.5 (Monoceros Nebula), and G206.9+2.3 (PKS 0646+06) and the first polarization measurements at λ6 cm for SNRs G82.2+5.3 (W63), G106.3+2.7, G114.3+0.3, G116.5+1.1, G166.0+4.3 (VRO 42.05.01), G205.5+0.5 (Monoceros Nebula), and G206.9+2.3 (PKS 0646+06). Most of the newly derived integrated radio spectra are consistent with previous results. The new flux densities obtained from the Urumqi λ6 cm, Effelsberg λ11 cm and λ21 cm surveys are crucial to determine the spectra of SNR G65.1+0.6, G69.0+2.7 (CTB 80), G93.7−0.2, and G114.3+0.3. We find that G192.8−1.1 (PKS 0607+17) consists of background sources, H ii regions, and extended diffuse emission of thermal nature, and conclude that G192.8−1.1 is not a SNR.

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Section: G890+47 (Hb21)mentioning

confidence: 96%

Section: G890+47 (Hb21)mentioning

confidence: 99%

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Han

Reich

et al. 2011

A&A

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“…Willis (1973), (3) Dickel & DeNoyer (1975), (4) Landecker & Caswell (1983), (5) Taylor et al (1992), (6) Mantovani et al (1985), (7) Reich et al (1988, Wolfgang Reich, priv. communication), (8) , (9) Pineault & Chastenay (1990), (10) Weiler & Shaver (1978), (11) Wendker et al (1991), (12) Landecker et al (1993), (13) Higgs et al (1977), (14) Higgs et al (1991), (15) Reich et al (2003), (16) Matthews et al (1977), (17) Matthews & Shaver (1980), (18) Hirabayashi & Takahashi (1972), (19) Haslam et al (1980), (20) Lalitha et al (1984), (21) Velusamy & Kundu (1974), (22) Mantovani et al (1982), (23) Landecker et al (1985), (24) Mantovani et al (1991), (25) Goss et al (1984), (26) Kothes et al (2005), (27) Pineault & Joncas (2000), (28) Kothes (2003), (29) …”

Section: Notes On Individual Objectsmentioning

confidence: 99%

A catalogue of Galactic supernova remnants from the Canadian Galactic plane survey

Kothes

Федотов

Foster³

et al. 2006

A&A

153

174

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We present a new catalogue containing all known Galactic supernova remnants observed in phase I and II of the Canadian Galactic Plane Survey (65. Stokes I images at 1420 MHz of 34 SNRs and at 408 MHz of 36 SNRs are displayed. From these 1 and 3 -resolution data (respectively) we determine accurate centre positions and angular dimensions. The flux densities at 1420 and 408 MHz are integrated and combined with values from the literature to define more accurate radio spectra. The CGPS polarization data at 1420 MHz were examined and significant linear polarization from 18 SNRs is found, with a modest signal from 6 others.

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“…The cometary shaped, radio continuum source G106.3+2.7 was described as a supernova remnant (SNR) by Joncas & Higgs (1990) and Pineault & Joncas (2000). A small, shell-like structure, the ''Boomerang,'' with a length of about 3 0 , is located at the northeastern tip of the SNR's head structure.…”

Section: Introductionmentioning

confidence: 99%

The Boomerang PWN G106.6+2.9 and the Magnetic Field Structure in Pulsar Wind Nebulae

Kothes

Reich

Uyanıker

2006

ApJ

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We present new observations at high radio frequencies made with the Effelsberg 100 m radio telescope of the ''Boomerang'' pulsar wind nebula ( PWN ) G106.65+2.96, which is part of the supernova remnant (SNR) G106.3+2.7. Including low-frequency data from the Canadian Galactic Plane Survey allows us to develop a complete picture of the PWN and its evolution in a very complex environment. The radio continuum spectrum reveals a break between 4 and 5 GHz that is the result of synchrotron cooling. We find evidence that the reverse shock of the initial supernova shock wave has driven away the original PWN, which explains why the current nebula around the pulsar has such a low radio luminosity. An analysis of the energy budget of the pulsar, the magnetic field in the nebula, and the lifetime of relativistic electrons gives a magnetic field of 2.6 mG in the PWN with an age of 3900 yr. This is not the age of the SNR but the time that has passed since the reverse shock crushed the original PWN. A comparison of our polarization measurements with those of other PWNe leads to a simple model of the magnetic field structure within such an object. Using this model, we derive an angle of about 30 between the Galactic north and the spin axis of the pulsar, projected onto the plane of the sky. The spin axis is pointing away from us, toward the northwest. This agrees nicely with the results of Ng and Romani, who in a 2004 paper calculated an angle of 20 from their fits of a model torus to a Chandra measurement of the Boomerang. The nebula contains a toroidal magnetic field structure, yet the rotation measure distribution indicates a radial magnetic field as its cause.

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G106.3+2.7: A Supernova Remnant in a Late Stage of Evolution

Cited by 50 publications

References 18 publications

A Sino-Germanλ6 cm polarization survey of the Galactic plane

A Sino-Germanλ6 cm polarization survey of the Galactic plane

A catalogue of Galactic supernova remnants from the Canadian Galactic plane survey

The Boomerang PWN G106.6+2.9 and the Magnetic Field Structure in Pulsar Wind Nebulae

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