The SN 1006 Remnant: Optical Proper Motions, Deep Imaging, Distance, and Brightness at Maximum

Winkler, P. F.; Gupta, Gaurav; Long, Knox S.

doi:10.1086/345985

Cited by 165 publications

(211 citation statements)

References 54 publications

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“…The value of the shock velocity calculated by this means agrees well with the recent measurement in X-rays by Katsuda et al (2009), yielding (0.48 ± 0.04) arcsec yr −1 in the synchrotron emitting regions (NE and SW), which corresponds to 5000 ± 400 km s −1 for a distance of 2.2 kpc. This does not contradict the value of (0.28 ± 0.008) arcsec yr −1 measured by Winkler et al (2003) in the optical filaments, which are situated in the NW region of the remnant. All those calculations neglect the dynamic role of accelerated particles however, which is potentially quite important.…”

Section: Discussionsupporting

confidence: 73%

“…The evolution of its luminosity indicates that it is the result of a type Ia supernova (Schaefer 1996), probably the brightest supernova in recorded history. A distance of 2.2 kpc was derived by Winkler et al (2003) based on comparing the optical proper motion with an estimate of the shock velocity A&A 516, A62 (2010) derived from optical thermal line broadening assuming a high Mach number single-fluid shock.…”

Section: Introductionmentioning

confidence: 99%

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First detection of VHEγ-rays from SN 1006 by HESS

Acero¹,

Aharonian²,

Akhperjanian³

et al. 2010

A&A

161

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Aims. Recent theoretical predictions of the lowest very high energy (VHE) luminosity of SN 1006 are only a factor 5 below the previously published HESS upper limit, thus motivating further in-depth observations of this source. Methods. Deep observations at VHE energies (above 100 GeV) were carried out with the high energy stereoscopic system (HESS) of Cherenkov Telescopes from 2003 to 2008. More than 100 h of data have been collected and subjected to an improved analysis procedure. Results. Observations resulted in the detection of VHE γ-rays from SN 1006. The measured γ-ray spectrum is compatible with a power-law, the flux is of the order of 1% of that detected from the Crab Nebula, and is thus consistent with the previously established HESS upper limit. The source exhibits a bipolar morphology, which is strongly correlated with non-thermal X-rays. Conclusions. Because the thickness of the VHE-shell is compatible with emission from a thin rim, particle acceleration in shock waves is likely to be the origin of the γ-ray signal. The measured flux level can be accounted for by inverse Compton emission, but a mixed scenario that includes leptonic and hadronic components and takes into account the ambient matter density inferred from observations also leads to a satisfactory description of the multi-wavelength spectrum.

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Section: Discussionsupporting

confidence: 73%

Section: Introductionmentioning

confidence: 99%

First detection of VHEγ-rays from SN 1006 by HESS

Acero¹,

Aharonian²,

Akhperjanian³

et al. 2010

A&A

161

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“…Figure 5 (top right) shows that the thermal emission (0.5 to 0.8 keV band) is rather uniform, but with a significant minimum toward the northwest. This is paradoxical, because that direction is, according to Hα observations (Winkler et al 2003), where the density in the ambient medium is largest. If it was due to additional extinction there, the column density would need to be about 1.4 × 10 21 cm −2 to reduce the flux by a factor 2 (as observed) in that band.…”

Section: Profilesmentioning

confidence: 99%

Geometry of the non-thermal emission in SN 1006

Rothenflug¹,

Ballet²,

Dubner

et al. 2004

A&A

126

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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“…The profiles of the Balmer lines, especially a broad component that arises from charge transfer between neutral H atoms that penetrate the shock and hot protons behind the shock front, permit a direct estimate of the shock speed of 2890 AE 100 km s À1 on the northwest limb of SN 1006 (Ghavamian et al 2002). The proper motion of the filaments in the northwest of 0>280 AE 0>008 yr À1 (Winkler, Gupta, & Long 2003) implies a distance of 2:17 AE 0:08 kpc and a physical radius of 9.5 pc.…”

Section: Introductionmentioning

confidence: 99%

ChandraCCD Imagery of the Northeast and Northwest Limbs of SN 1006

Long

Reynolds

Raymond

et al. 2003

ApJ

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153

190

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We present deep images of the SN 1006 remnant (G327.6+14.6) with the ACIS instrument on the Chandra X-Ray Observatory. Two regions have been observed, the synchrotron-dominated northeast limb and the thermally dominated northwest limb, as well as a substantial portion of the interior of the remnant shell. The brightest features in the X-ray images correspond closely to radio features in the northeast and to Balmer-dominated filaments in the northwest. The spectra of the brighter filaments in the northeast are harder, with less prominent line emission than those in the northwest. In addition to highly elongated filaments, both images show enhanced clumps of emission well inside of the shock front that appear to be dominated by emission from oxygen. These probably arise from shock-heated ejecta, based on analysis of their X-ray spectra. We find no firm evidence for a halo of X-ray emission outside the shock to the northeast, as predicted by the Fermi shock-acceleration picture, in which relativistic electrons should be diffusing ahead of the shock. Our limits on upstream emission are less than 1.5% of the postshock levels in regions where the supernova remnant is brightest. This strongly suggests that the bright rims are flattened sheets nearly perpendicular to the plane of the sky and that the magnetic field strength jumps at the shock by a factor significantly larger than 4, as has been proposed if the shock puts significant energy into accelerating nonthermal ions. The spectra obtained of the northwest rim are all dominated by the helium-like ions of O, Ne, Mg, and Si expected from shocks with ionization (n e t) parameters of order 100 cm À3 yr and electron temperatures of 0.5-1 keV, far lower than the postshock ion temperature implied by estimates of the shock speed obtained from the shape of the H line.

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The SN 1006 Remnant: Optical Proper Motions, Deep Imaging, Distance, and Brightness at Maximum

Cited by 165 publications

References 54 publications

First detection of VHEγ-rays from SN 1006 by HESS

First detection of VHEγ-rays from SN 1006 by HESS

Geometry of the non-thermal emission in SN 1006

ChandraCCD Imagery of the Northeast and Northwest Limbs of SN 1006

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