Symmetry of the radio emission from two high-latitude supernova remnants, G296.5 + 10.0 and G327.6 + 14.6 (SN 1006)

Roger, R. S.; Milne, D. K.; Kesteven, M. J.; Wellington, K. J.; Haynes, R. F.

doi:10.1086/166703

Cited by 87 publications

(85 citation statements)

References 0 publications

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“…This could not be done directly from the images because of the strong contribution of the thermal emission outside the bright limbs. Figure 8 overlays the same ratio obtained from the MOST + Parkes radio map (Roger et al 1988). Qualitatively, a very similar azimuthal modulation is obtained with both radio maps, even though significant differences exist (most conspicuously between both bright limbs).…”

Section: Synchrotron Cut-off Frequencymentioning

confidence: 62%

“…This can be achieved from the merging of interferometric with single dish data, which allows to recover information at all spatial frequencies. The Molonglo/Parkes 843 MHz radio map (Roger et al 1988) suited our purpose, but its spatial resolution (HPBW 64 ×43 ) was somewhat too low.…”

Section: Radiomentioning

confidence: 99%

“…The most natural reason for that morphology is that the pre-supernova orientation of the magnetic field created a preferred axis. The radio observations were interpreted as being due to the magnetic field being initially oriented from southeast to northwest, so that the bright limbs correspond to Roger et al 1988). The dashed line shows the limit between the "interior" and the "limbs" used in Sect.…”

Section: Profilesmentioning

confidence: 99%

“…2.1). The diamonds were obtained using the radio map of Roger et al (1988). In the radial profile (right) the simple crosses were obtained without any background subtraction.…”

Section: Synchrotron Cut-off Frequencymentioning

confidence: 99%

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Geometry of the non-thermal emission in SN 1006

Rothenflug¹,

Ballet²,

Dubner

et al. 2004

A&A

123

158

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Abstract. SN 1006 is the prototype of shell supernova remnants, in which non-thermal synchrotron emission dominates the X-ray spectrum. The non-thermal emission is due to the cosmic-ray electrons accelerated behind the blast wave. The X-ray synchrotron emission is due to the highest energy electrons, and is thus a tracer of the maximum energy electrons may reach behind a shock. We have put together all XMM-Newton observations to build a full map of SN 1006. The very low brightness above 2 keV in the interior indicates that the bright non-thermal limbs are polar caps rather than an equator. This implies that the ambient magnetic field runs southwest to northeast, along the Galactic plane. We used a combined VLA/Parkes radio map to anchor the spectrum at low energy, and model the spectra with synchrotron emission from a cut-off power-law electron distribution, plus a thermal component. We present radial and azimuthal profiles of the cut-off frequency. The cut-off frequency decreases steeply with radius towards the center and with position angle away from the maximum emission. The maximum energy reached by accelerated particles, as well as their number, must be higher at the bright limbs than elsewhere. This implies interesting constraints for acceleration at perpendicular shocks. Overall the XMM-Newton data is consistent with the model in which the magnetic field is amplified where acceleration is efficient.

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Section: Synchrotron Cut-off Frequencymentioning

confidence: 62%

Section: Radiomentioning

confidence: 99%

Section: Profilesmentioning

confidence: 99%

“…2.1). The diamonds were obtained using the radio map of Roger et al (1988). In the radial profile (right) the simple crosses were obtained without any background subtraction.…”

Section: Synchrotron Cut-off Frequencymentioning

confidence: 99%

See 2 more Smart Citations

Geometry of the non-thermal emission in SN 1006

Rothenflug¹,

Ballet²,

Dubner

et al. 2004

A&A

123

158

View full text Add to dashboard Cite

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“…The X-ray source 1E 1207.4−5209 was discovered with the Einstein satellite (Helfand & Becker 1984) close to the center of G296.5+10.0, a ∼7 kyr old supernova remnant (SNR) located at a distance of ∼2 kpc (Roger et al 1988;Giacani et al 2000). It was the second thermally-emitting, radio-quiet, isolated neutron star (INS) candidate found inside a SNR, after 1E 161348−5055 in RCW 103 (Tuohy & Garmire 1980).…”

Section: Introductionmentioning

confidence: 99%

HST and VLT observations of the neutron star 1E 1207.4–5209

Luca

Mignani

Sartori

et al. 2010

A&A

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The peculiar central compact object 1E 1207.4−5209 in the G296.5+10.0 supernova remnant has been proposed to be an "antimagnetar" -a young neutron star born with a weak dipole field. Accretion, possibly of supernova fallback material, has also been invoked to explain a large surface temperature anisotropy as well as the generation of peculiar cyclotron absorption features superimposed on its thermal spectrum. Interestingly enough, a faint optical/infrared source was proposed as a possible counterpart to 1E 1207.4−5209, but later questioned, based on coarse positional coincidence. On the basis of the large offset of 1E 1207.4−5209 with respect to the center of its host supernova remnant, the source should move at ∼70 mas yr −1 . Thus, we tested the association by measuring the proper motion of the proposed optical counterpart. Using Hubble Space Telescope (HST) observations spanning 3.75 years, we computed a 3σ upper limit of 7 mas yr −1 . Absolute astrometry on the same HST data set also places the optical source significantly off the 99% confidence Chandra position. This allows us to safely rule out the association. Using the HST data set, coupled to ground-based observations collected at the ESO/Very Large Telescope (VLT), we set the deepest limits ever obtained on the optical/infrared emission from 1E 1207.4−5209. By combining these limits with the constraints derived from X-ray timing, we rule out accretion as the source of the thermal anisotropy of the neutron star.

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