The peculiar X-ray morphology of the supernova remnant G292.0+1.8 - Evidence for an asymmetric supernova explosion

Tuohy, I. R.; Burton, W. M.; Clark, David H.

doi:10.1086/183871

Cited by 37 publications

(29 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This trend is consistent with the geometric projection expected from an expanding shell. A new feature, unseen in the earlier photographic images of G292.0+1.8 (Goss et al 1979;Tuohy et al 1982) but clearly detected both in the [O iii] image ( Fig. 1) and our RFP scans ( Fig.…”

mentioning

confidence: 58%

“…Although the core-collapse supernovae that produced these OSNRs should have all left behind rotating neutron stars (pulsars), G292.0+1.8 is the only Galactic remnant from this class found to harbor both an active pulsar (Camilo et al 2002;Hughes et al 2003) and associated pulsar wind nebula (PWN; Hughes et al 2001). Earlier Einstein HRI observations indicated that a central bar of enhanced X-ray emission was present in G292.0 + 1.8, superimposed on an ellipsoidal disk of emission ( Tuohy et al 1982). Recent Chandra imagery of G292.0+1.8 ( Park et al 2002( Park et al , 2004Gonzalez & Safi-Harb 2003) have revealed that the X-ray bar is of normal composition, suggesting that G292.0 + 1.8 is interacting with circumstellar wind material.…”

Section: à3mentioning

confidence: 99%

“…It is kinematically resolved into multiple components by our RFP observations in Figure 2: a bar-shaped structure of material at zero radial velocity, projected onto a high-velocity component of clumpy material. Due to its intrinsic faintness, the belt emission escaped detection in the earlier photographic plate images of G292.0+1.8 (Goss et al 1979;Tuohy et al 1982). As we show below, the bar seen in our RFP scans appears to be the optical counterpart to the bar seen in the Chandra images by Park et al (2002Park et al ( , 2004 and Gonzalez & Safi-Harb (2003).…”

mentioning

confidence: 91%

See 2 more Smart Citations

Exploring the Kinematics of the Oxygen‐rich Supernova Remnant G292.0+1.8: Ejecta Shells, Fast‐moving Knots, and Shocked Circumstellar Material

Ghavamian¹,

Hughes²,

Williams³

2005

ApJ

View full text Add to dashboard Cite

We present the results of an in-depth optical study of the core-collapse supernova remnant G292.0+1.8 using the Rutgers Fabry-Perot (RFP) imaging spectrometer. Our observations provide a detailed picture of the supernova remnant in the emission lines of [O iii] k5007, H , and [N ii] k6548. The [O iii] Fabry-Perot scans reveal a bright crescent-shaped spur of previously known high-velocity (V radial $ 1500 km s À1 ) O-rich ejecta located on the eastern side of the remnant. The spur consists of a semicoherent structure of mostly redshifted material, along with several clumps that have apparently broken out of the more orderly shell-like expansion. The high-velocity (k600 km s À1 ) component of the spur also displays a scalloped morphology characteristic of Rayleigh-Taylor instabilities. We also find a large number of fast-moving knots (FMKs) of O-rich ejecta undetected in prior photographic plate images and similar to features seen in Cas A. The FMKs are distributed sparsely in the interior of G292.0+1.8 and are seen mostly in blueshifted emission out to V radial % À1700 km s À1 . The position-velocity distribution of the FMKs can be kinematically described as a shell 3A4 in radius expanding at a velocity of 1700 km s À1. Another feature apparent in the [O iii] scans is an equatorial belt consisting of both a barlike structure at zero radial velocity and a clumpy, highvelocity ejecta component seen in projection along the line of sight. Portions of the zero-velocity bar are spatially well correlated with a similar structure seen in the Chandra X-ray image of G292.0+1.8. The bar is also detected in our H RFP images at zero radial velocity, providing further evidence that this structure is of circumstellar origin. We find that the optical and X-ray properties of the bar are consistent with incomplete (partially radiative) shocks in material of moderate densities. There are also a number of faint, elongated structures seen in H at zero radial velocity across the interior of G292.0+1.8 that lack [O iii] and X-ray counterparts. These filaments may be low-density H i clouds photoionized by hard radiation from the interior of the remnant. Overall, these results suggest that G292.0+1.8 is currently interacting with a low-density environment. We find no evidence for high-velocity H or [N ii] emission over the dynamical range sampled by the RFP. Assuming a distance of 6 kpc for G292.0+1.8, we estimate a kinematic age of (3000-3400)d 6 yr for this remnant.

show abstract

mentioning

confidence: 58%

Section: à3mentioning

confidence: 99%

mentioning

confidence: 91%

See 1 more Smart Citation

Exploring the Kinematics of the Oxygen‐rich Supernova Remnant G292.0+1.8: Ejecta Shells, Fast‐moving Knots, and Shocked Circumstellar Material

Ghavamian¹,

Hughes²,

Williams³

2005

ApJ

View full text Add to dashboard Cite

show abstract

“…(Hwang et al 2001 consider a highly asymmetric explosion and subsequent evolution to account for their Chandra Doppler map of Cas A.) X-ray observations of G292.0+1.8 by Tuohy, Clark, & Burton (1982) revealed a barlike feature that they attributed to a ring of oxygen-rich material ejected into the equatorial plane. Examination of a velocity map generated from optical observations of 1E 0102.2À7219 led Tuohy & Dopita (1983) to suggest that its velocity structure could be modeled in terms of a severely distorted ring of ejecta.…”

Section: Discussionmentioning

confidence: 99%

ChandraHigh‐Resolution X‐Ray Spectrum of Supernova Remnant 1E 0102.2−7219

Flanagan

Canizares

Dewey

et al. 2004

ApJ

View full text Add to dashboard Cite

Chandra High Energy Transmission Grating Spectrometer observations of the supernova remnant (SNR) 1E 0102.2À7219 in the Small Magellanic Cloud reveal a spectrum dominated by X-ray emission lines from hydrogen-like and helium-like ions of oxygen, neon, magnesium, and silicon, with little iron. The dispersed spectrum shows a series of monochromatic images of the source in the light of individual spectral lines. Detailed examination of these dispersed images reveals Doppler shifts within the SNR, indicating bulk matter velocities on the order of 1000 km s À1 . These bulk velocities suggest an expanding ringlike structure with additional substructure, inclined to the line of sight. A two-dimensional spatial/velocity map of the SNR shows a striking spatial separation of redshifted and blueshifted regions and indicates a need for further investigation before an adequate three-dimensional model can be found. The radii of the ringlike images of the dispersed spectrum vary with ionization stage, supporting an interpretation of progressive ionization due to passage of the reverse shock through the ejecta. Plasma diagnostics with individual emission lines of oxygen are consistent with an ionizing plasma in the low-density limit and provide temperature and ionization constraints on the plasma. Assuming a pure metal plasma, the mass of oxygen is estimated at $6 M , consistent with a massive progenitor.

show abstract

“…Although the center-filled radio morphology suggested an interior plerionic component, strong X-ray emission lines seemed to rule out such speculations. High resolution imaging with the Einstein HRI revealed its peculiar morphology (Tuohy et al 1982) and X-ray emission was found to come from two distinct components, the central barlike feature and the ellipsoidal disk of approximately uniform surface brightness. Both the elemental abundances determined from X-ray spectra (Hughes et al 1994) and the peculiar morphology suggested a Type II SN explosion.…”

Section: G2920+18 (Mshll-s4)mentioning

confidence: 99%