Detection of X-ray emission from the remnant of the supernova 1006 A.D.

Winkler, P. F.; Laird, F. N.

doi:10.1086/182066

Cited by 18 publications

(8 citation statements)

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“…The remnant of SN 1006, G327.6+14.6, was first identified through its radio emission by Gardner & Milne (1965). X-ray emission was detected by Winkler & Laird (1976), and very soon afterward van den Bergh (1976) reported faint optical filaments associated with SN 1006. More recent radio maps (Reynolds & Gilmore 1986;Moffett et al 1993) show a somewhat barrel-shaped shell, 30 ′ in diameter and brightest along the NE and SW limbs.…”

Section: Introductionmentioning

confidence: 99%

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

Winkler¹,

Gupta²,

Long³

2003

ApJ

165

195

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We report the first measurement of proper motions in the SN 1006 remnant (G327.6+14.6) based entirely on digital images. CCD images from three epochs spanning a period of 11 years are used: 1987 from Las Campanas, and 1991 and 1998 from CTIO. The filaments in SN 1006 are non-radiative, appearing only in the Balmer lines of hydrogen. Delicate filaments-probably thin sheets seen in projectiondelineate the shock front along the northwest rim of the remnant. We use the center of curvature of the filaments to define a convenient geometry, and integrate along short segments to obtain one-dimensional profiles. These remain unchanged, within seeing and statistical errors, from one epoch to another. Measuring the shift in a direction perpendicular to the filaments, we obtain proper motions of 280±8 mas yr −1 along the entire length where the filaments are well defined, with little systematic variation along the filaments. In addition to the measurements of the well-defined filaments in the NW of SN 1006, we also report very deep Hα imaging observations of the entire remnant that clearly show very faint emission surrounding almost the entire shell, as well as some diffuse emission regions in the (projected) interior.Combining the proper motion measurement with a recent measurement of the shock velocity based on spectra of the same filaments by Ghavamian et al. leads to a distance of 2.17 ± 0.08 kpc to SN 1006. Several lines of argument suggest that SN 1006 was a Type Ia event, so the improved distance measurement can be combined with the peak luminosity for SNe Ia, as recently determined for events in galaxies with Cepheid-based distances, to calculate the apparent brightness of the spectacular event that drew wide attention in the eleventh century. The result, V max = −7.5 ± 0.4, lies squarely in the middle of the wide range of estimates based on the historical observations.

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Section: Introductionmentioning

confidence: 99%

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

Winkler¹,

Gupta²,

Long³

2003

ApJ

165

195

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“…SN 1006 has been the prototype laboratory for the study of electron acceleration to high energies in shocks. X-rays from this object were first reported by Winkler & Laird (1976). The earlier featureless spectrum ( Becker et al 1980) was modeled as the loss-steepened extrapolation of the radio synchrotron spectrum by Reynolds & Chevalier (1981).…”

Section: Introductionmentioning

confidence: 99%

X‐Ray Observations of SN 1006 withINTEGRAL

Kalemci

Reynolds

Boggs

et al. 2006

ApJ

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The remnant of the supernova of 1006 AD, the remnant first showing evidence for the presence of X-ray synchrotron emission from shock-accelerated electrons, was observed for $1000 ks with INTEGRAL in order to study electron acceleration to very high energies. The aim of the observation was to characterize the synchrotron emission and attempt to detect nonthermal bremsstrahlung using the combination of IBIS and JEM-X spatial and spectral coverage. The source was detected with JEM-X between the 2.4 and 8.4 keV bands and was not detected with either ISGRI or SPI above 20 keV. The ISGRI upper limit is about a factor of 4 above current model predictions, but confirms the presence of steepening in the power law extrapolated from lower energies (<4 keV).

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“…For example, SN 1006 and 3C 58 are thought to have been Type Ia (Winkler et al 2003) and Type II (Panagia & Weiler 1980) supernovae, respectively. SN 1006 has an X-ray luminosity (1-10 keV) of $5 ; 10 34 ergs s À1 (Winkler & Laird 1976;Winkler et al 2003), and 3C 58 has an X-ray luminosity (0.1-4 keV) of only $10 34 ergs s À1 (Helfand et al 1995). Therefore, neither of these young SNRs would have been detected by the Chandra surveys.…”

Section: Are the [O Iii] Nebulae Snrs?mentioning

confidence: 96%

Why are X-Ray Sources in the M31 Bulge So Close to Planetary Nebulae?

et al. 2004

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We compare a deep (37 ks) Chandra ACIS-S image of the M31 bulge with deep [O iii] Local Group Survey data of the same region. Through precision image alignment using globular cluster X-ray sources, we are able to improve constraints on possible optical/X-ray associations suggested by previous surveys. Our image registration allows us to rule out several emission-line objects, previously suggested to be the optical counterparts of X-ray sources, as true counterparts. At the same time, we find six X-ray sources peculiarly close to strong [O iii] emission-line sources, classified as planetary nebulae (PNs) by previous optical surveys. Our study shows that, while the X-rays are not coming from the same gas as the optical line emission, the chances of these six X-ray sources lying so close to cataloged PNs is only $1%, suggesting that there is some connection between these [O iii] emitters (possibly PNs) and the X-ray sources. We discuss the possibility that these nebulae are misidentified supernova remnants, and we rule out the possibility that the X-ray sources are ejected X-ray binaries. There is a possibility that some cases involve a PN and a low-mass X-ray binary that occupy the same undetected star cluster. Beyond this unconfirmed possibility and the statistically unlikely one that the associations are spatial coincidences, we are unable to explain these [O iii]/X-ray associations.

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Detection of X-ray emission from the remnant of the supernova 1006 A.D.

Cited by 18 publications

References 0 publications

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

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

X‐Ray Observations of SN 1006 withINTEGRAL

Why are X-Ray Sources in the M31 Bulge So Close to Planetary Nebulae?

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