Optical identification and spectrum of the supernova remnant G292.0 + 1.8

Goss, W. M.; Shaver, P. A.; Zealey, W. J.; Murdin, Paul; Clark, David H.

doi:10.1093/mnras/188.2.357

Cited by 58 publications

(50 citation statements)

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“…this foreground gas is confined to only the near part of the spiral arm, we conclude that the most likely lower limit for the SNR is a systemic velocity of 0 km s À1 , corresponding to a distance of at least 6:2 AE 0:9 kpc. 6 This is broadly consistent with the distance to the SNR of 5.4 kpc implied by reddening of its optical filaments (Goss et al 1979) and with the distance of 6:4 AE 1:3 kpc implied by the dispersion measure of the associated pulsar J1124À5916 (Cordes & Lazio 2002). In future discussion, we adopt a distance to the system of 6d 6 kpc.…”

Section: H I Absorptionsupporting

confidence: 77%

“…In the optical, high-velocity oxygen rich filaments were identified, characteristic of emission from a young SNR with a massive progenitor (Goss et al 1979;van den Bergh 1979;Braun et al 1983) and arguing for an age $1700 yr. In X-rays, the SNR showed an ellipsoidal disk of emission (Tuohy, Clark, & Burton 1982), with an emissionline spectrum resulting from the shock-heated ejecta of a massive progenitor (Clark, Tuohy, & Becker 1980;Hughes & Singh 1994).…”

Section: Introductionmentioning

confidence: 99%

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A Multifrequency Radio Study of Supernova Remnant G292.0+1.8 and Its Pulsar Wind Nebula

Gaensler

Wallace²

2003

ApJ

121

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We present a detailed radio study of the young supernova remnant (SNR) G292.0+1.8 and its associated pulsar PSR J1124À5916, using the Australia Telescope Compact Array at observing wavelengths of 20, 13, and 6 cm. We find that the radio morphology of the source consists of three main components: a polarized flat-spectrum central core coincident with the pulsar J1124À5916, a surrounding circular steep-spectrum plateau with sharp outer edges, and superposed on the plateau, a series of radial filaments with spectra significantly flatter than their surroundings. H i absorption argues for a lower limit on the distance to the system of 6 kpc. The core clearly corresponds to radio emission from a pulsar wind nebula powered by PSR J1124À5916, while we conclude that the plateau represents the surrounding SNR shell. The plateau's sharp outer rim delineates the SNR's forward shock, while the thickness of the plateau region demonstrates that the forward and reverse shocks are well separated. Assuming a distance of 6 kpc and an age for the source of 2500 yr, we infer an expansion velocity for the SNR of $1200 km s À1 , an ambient density $0.9 cm À3 , an ejected mass $5.9 M , and a supernova explosion energy $1:1 Â 10 51 ergs. We interpret the flat-spectrum radial filaments superposed on the steeper spectrum plateau as Rayleigh-Taylor unstable regions between the forward and reverse shocks of the SNR. The flat radio spectrum seen for these features results from efficient second-order Fermi acceleration in strongly amplified magnetic fields.

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Section: H I Absorptionsupporting

confidence: 77%

Section: Introductionmentioning

confidence: 99%

A Multifrequency Radio Study of Supernova Remnant G292.0+1.8 and Its Pulsar Wind Nebula

Gaensler

Wallace²

2003

ApJ

121

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“…The red supergiant wind from the progenitor star can extend to the observed radii, so this is the likely ambient medium. Strong mass loss is consistent with the absence of Balmer lines in the spectrum of G292.0+1.8 (Goss et al 1979), implying that most of the H envelope had been lost before the supernova.…”

supporting

confidence: 59%

Pulsar Wind Nebulae and Their Supernovae

Chevalier¹

2004

Symp. - Int. Astron. Union

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Abstract. Young supernova remnants that contain pulsar wind nebulae provide diagnostics for both the inner part of the supernova and the interaction with the surrounding medium, providing an opportunity to relate these objects to supernova types. Among observed young nebulae, there is evidence for a range of supernova types, including Type lIP (Crab Nebula and SN 1054) and Type lIb/lIn/IlL (G292.0+1.8).

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“…To date there have been six OSNRs identified: Cassiopeia A ( Minkowski 1957;Chevalier & Kirshner 1978Reed et al 1995;Fesen et al 2001), Puppis A ( Winkler & Kirshner 1985), and G292.0+1.8 (Goss et al 1979;van den Bergh 1979;Braun et al 1983;Sutherland & Dopita 1995) in the Galaxy, 0540À69.3 (Kirshner et al 1989) and N132D ( Lasker 1978( Lasker , 1980Morse et al 1995Morse et al , 1996Blair et al 2000) in the LMC, E0102À72.2 in the SMC ( Dopita et al1981;Tuohy & Dopita 1983;Blair et al 2000), and a spatially unresolved remnant in NGC 4449 ( Kirshner & Blair 1980;Blair et al 1983). 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).…”

Section: à3mentioning

confidence: 99%

“…The first optical imagery of G292.0+1.8 was performed by Goss et al (1979), who discovered a bright, crescent-shaped spur of nebulosity coincident with the extended radio source position. Their spectra showed emission lines of oxygen and neon, but little or no line emission from hydrogen, helium, or nitrogen.…”

Section: à3mentioning

confidence: 99%

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

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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.

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Optical identification and spectrum of the supernova remnant G292.0 + 1.8

Cited by 58 publications

References 0 publications

A Multifrequency Radio Study of Supernova Remnant G292.0+1.8 and Its Pulsar Wind Nebula

A Multifrequency Radio Study of Supernova Remnant G292.0+1.8 and Its Pulsar Wind Nebula

Pulsar Wind Nebulae and Their Supernovae

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

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