X-Ray Proper Motions and Shock Speeds Along the Northwest Rim of Sn 1006

Katsuda, Satoru; Long, Knox S.; Petre, Robert; Reynolds, Stephen P.; Williams, Brian J.; Winkler, P. F.

doi:10.1088/0004-637x/763/2/85

Cited by 31 publications

(25 citation statements)

References 30 publications

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“…The inferred shock velocity for SN 1006 is roughy consistent with the proper motion of the shock ahead of the knot (Winkler et al 2003; Katsuda et al 2013a). Therefore, a simple interpretation is that the knot was heated by a forward shock.…”

Section: +72supporting

confidence: 57%

High-Resolution X-Ray Spectroscopy of Galactic Supernova Remnants

Katsuda

Tsunemi

2014

APP

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High-resolution X-ray spectroscopy of Galactic supernova remnants (SNRs), based on grating spectrometers onboard XMM-Newton and Chandra, has been revealing a variety of new astrophysical phenomena. Broadened oxygen lines for a northwestern compact knot in SN 1006 clearly show a high oxygen temperature of ∼300 keV. The high temperature together with a lower electron temperature (kTe ∼ 1 keV) can be reasonably interpreted as temperature non-equilibration between electrons and oxygen behind a collisionless shock. An ejecta knot in the Puppis A SNR shows blueshifted line emission by ∼1500 km s −1 . The line widths are fairly narrow in contrast to the SN 1006's knot; an upper limit of 0.9 eV is obtained for O VIII Lyα, which translates to an oxygen temperature of kTO < 30 keV. The low temperature suggests that the knot was heated by a reverse shock whose velocity is ∼4 times slower than that of a forward shock. Anomalous intensity ratios in O VII Heα lines, i.e., a stronger forbidden line than a resonance line, is found in a cloud-shock interaction region in Puppis A. The line ratio can be best explained by the charge-exchange emission that should arise at interfaces between the cold/warm clouds and the hot plasma. There are several other targets for which we plan to analyze high-quality grating data prior to the operation of the soft X-ray spectrometer onboard Astro-H.

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Section: +72supporting

confidence: 57%

High-Resolution X-Ray Spectroscopy of Galactic Supernova Remnants

Katsuda

Tsunemi

2014

APP

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“…The statistical uncertainties come from the fits themselves: we report the best fit as the shift in which the value of χ 2 is minimized, and take as the 90% confidence limits the value of the shift in each direction where χ 2 has risen by 2.706. For the systematic uncertainties, the typical reported values, such as those in Katsuda et al (2013), of the registration uncertainties in aligning the images are irrelevant for our purposes. Instead, we found that varying the choice of fit region for each shock front, marked by the shaded grey areas, resulted in slightly different values for the shock velocity.…”

Section: Measurements and Discussionmentioning

confidence: 99%

The Expansion of the Young Supernova Remnant 0509-68.7 (N103B)

Williams

Blair

Borkowski

et al. 2018

ApJL

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We present a second epoch of Chandra observations of the Type Ia LMC SNR 0509-68.7 (N103B) obtained in 2017. When combined with the earlier observations from 1999, we have a 17.4-year baseline with which we can search for evidence of the remnant's expansion. Although the lack of strong point source detections makes absolute image alignment at the necessary accuracy impossible, we can measure the change in the diameter and the area of the remnant, and find that it has expanded by an average velocity of 4170 (2860, 5450) km s −1 . This supports the picture of this being a young remnant; this expansion velocity corresponds to an undecelerated age of 850 yr, making the real age somewhat younger, consistent with results from light echo studies. Previous infrared observations have revealed high densities in the western half of the remnant, likely from circumstellar material, so it is likely that the real expansion velocity is lower on that side of the remnant and higher on the eastern side. A similar scenario is seen in Kepler's SNR. N103B joins the rare class of Magellanic Cloud SNRs with measured proper motions.

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“…The historical type Ia supernova remnant (SNR) SN 1006 is an ideal target to study the Fermi acceleration process in astrophysical shocks. It is a dynamically young remnant with shock velocity v s ∼ 5000 km/s (Katsuda et al 2009(Katsuda et al , 2013Winkler et al 2014), that evolves in a tenuous medium (n 0 ∼ 0.035 cm −3 in the southeastern limb, see Miceli et al 2012). It is spatially extended (radius R ∼ 15 ′ ) and shows a rather simple bilateral non-thermal morphology.…”

Section: Introductionmentioning

confidence: 99%

Shock-Cloud Interaction and Particle Acceleration in the Southwestern Limb of Sn 1006

Miceli

Acero

Dubner

et al. 2014

ApJ

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The supernova remnant SN 1006 is a powerful source of high-energy particles and evolves in a relatively tenuous and uniform environment, though interacting with an atomic cloud in its northwestern limb. The X-ray image of SN 1006 reveals an indentation in the southwestern part of the shock front and the HI maps show an isolated cloud (southwestern cloud) having the same velocity as the northwestern cloud and whose morphology fits perfectly in the indentation. We performed spatially resolved spectral analysis of a set of small regions in the southwestern nonthermal limb and studied the deep X-ray spectra obtained within the XMM-Newton SN 1006 Large Program. We also analyzed archive HI data, obtained combining single dish and interferometric observations. We found that the best-fit value of the N H derived from the X-ray spectra significantly increases in regions corresponding to the southwestern cloud, while the cutoff energy of the synchrotron emission decreases. The amount of the N H variations corresponds perfectly with the HI column density of the southwestern cloud, as measured from the radio data. The decrease in the cutoff energy at the indentation clearly reveals that the back side of the cloud is actually interacting with the remnant. The southwestern limb therefore presents a unique combination of efficient particle acceleration and high ambient density, thus being the most promising region for γ−ray hadronic emission in SN 1006. We estimate that such emission will be detectable with the Fermi telescope within a few years.

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X-Ray Proper Motions and Shock Speeds Along the Northwest Rim of Sn 1006

Cited by 31 publications

References 30 publications

High-Resolution X-Ray Spectroscopy of Galactic Supernova Remnants

High-Resolution X-Ray Spectroscopy of Galactic Supernova Remnants

The Expansion of the Young Supernova Remnant 0509-68.7 (N103B)

Shock-Cloud Interaction and Particle Acceleration in the Southwestern Limb of Sn 1006

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