Three-Dimensional Fabry-Perot Imaging Spectroscopy of the Crab Nebula, Cassiopeia A, and Nova GK Persei

Lawrence, Stephen S.; MacAlpine, G. M.; Uomoto, Alan; Woodgate, B. E.; Brown, L. W.; Oliversen, R. J.; Lowenthal, James D.; Liu, C.

doi:10.1086/117477

Cited by 96 publications

(140 citation statements)

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“…The LWS spectra reproduced in Fig. 1 shows velocity broadened profiles in [O III] A 88 urn in the northern (blueshifted) and south-eastern (redshifted) parts of the shell, similar to the velocity profiles associated with the shocked fast optical filaments measured by Lawrence et al (1995). Towards the centre of the remnant, however, where there is only faint optical emission, the [O III] A 88 /mi emission is comparably bright to that seen in the shell, with radial velocities within the ± 5000 km s -1 range expected for freely expanding cold ejecta interior to the reverse shock.…”

supporting

confidence: 74%

Observations of Supernova Remnants With ISO

Tuffs

1998

Highlights astron.

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Pointed observations with ISO have been made, or are planned, towards 58 supernova remnants (SNRs) in the galaxy and Magellanic clouds. The main emphasis is on detailed studies of gas, dust and synchrotron emission from selected regions within 24 well studied galactic remants. First results are available for Cas A (Lagage et al. 1996(Lagage et al. , 1997Tuffs et al. 1997;Unger et al. 1997), the Cygnus Loop (deCourchelle et al 1997;Fischera et al. 1997), RCW103 (Oliva et al. 1997Wright et al. 1997), and W44 and 3C391 (Reach andRho 1996). These are providing insights into issues such as the yield and composition of condensates in supernova ejecta, the processing of grains by adiabatic and radiative shocks, and the measurement of cold gas, inaccessible to optical observations, both from cool regions in radiative shocks and from unshocked ejecta. In this progress report these points are illustrated with reference to Cas A, the prototype of an ejecta-dominated remnant of a massive core-collapse supernova, and the Cygnus Loop and RCW103 as prime examples of radiative shocks delineating the interaction of fast blast waves with diffuse atomic and dense molecular clouds, respectively. The MIR spectrum of Cas A is very rich and continuum emission is spectrally confused with fine structure, molecular and solid state emission features over much of the wavelength range of ISOPHOT-S. A faint underlying continuum can nevertheless be discerned longwards of A ~ 7 \im , with a broad bump from 8-11 fim which may plausibly be identified with silicate. The morphological similarity between ISOCAM CVF images at A 9.8 fj,m and in the [SIV] and [Ne II] lines delineating ejecta thus provides convincing evidence for the presence of condensates in the supernova ejecta (Lagage et al. 1996), the first such detection in a galactic SNR. Also seen in the ISOPHOT-S spectra are precursor molecules of the condensates, notably SiO around 8.05/xm, raising the prospect that deeper observations could measure isotope ratios in the ejecta. In common with the other SNRs observed so far, none of the unidentified emission features commonly attributed to PAHs are apparent in the spectra towards Cas A.The brightness of the diffuse MIR counterpart to the radio and X-ray shell declines dramatically with decreasing wavelength, consistent with a paucity of emission from grains with temperatures >200K (with sizes <50nm). The brightness of the shell measured by ISOPHOT in a spectral region apparently free of spectral features around 6/imis comparable with the extrapolation of 1148

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supporting

confidence: 74%

Observations of Supernova Remnants With ISO

Tuffs

1998

Highlights astron.

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“…Fig. 3 in Lawrence et al (1995) shows that the QSF distribution does not coincide with the distribution of the other emitting components of the Cas A SNR, and that the distribution of the QSF does not have a spherical shape. The same can be seen by comparing Fig.…”

Section: Discussionmentioning

confidence: 92%

The hydrodynamics of the supernova remnant Cassiopeia A

Veelen

Langer

Vink

et al. 2009

A&A

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Aims. There are large differences in the proposed progenitor models for the Cas A SNR. One of these differences is the presence or absence of a Wolf-Rayet (WR) phase of the progenitor star. The mass loss history of the progenitor star strongly affects the shape of the Supernova remnant (SNR). In this paper we investigate whether the progenitor star of Cas A had a WR phase or not and how long it may have lasted.Methods. We performed two-dimensional multi-species hydrodynamical simulations of the CSM around the progenitor star for several WR life times, each followed by the interaction of the supernova ejecta with the CSM. We then looked at the influence of the length of the WR phase and compared the results of the simulations with the observations of Cas A. Results. The difference in the structure of the CSM, for models with different WR life times, has a strong impact on the resulting SNR. With an increasing WR life time the reverse shock velocity of the SNR decreases and the range of observed velocities in the shocked material increases. Furthermore, if a WR phase occurs, the remainders of the WR shell will be visible in the resulting SNR. Conclusions. Comparing our results with the observations suggests that the progenitor star of Cas A did not have a WR phase. We also find that the quasi-stationary flocculi (QSF) in Cas A are not consistent with the clumps from a WR shell that have been shocked and accelerated by the interaction with the SN ejecta. We can also conclude that for a SN explosion taking place in a CSM that is shaped by the wind during a short (≤ 15000 yr) WR phase, the clumps from the WR shell will be visible inside the SNR.

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“…10 ; van den Bergh & Kamper 1985). However, velocity maps in the [S II] doublet show that this line of emission is dynamically quite coherent, with velocities systematically decreasing ]900 to ]600 km s~1 from north to south (Lawrence et al 1995). The cluster of yellowish knots located farther west along the southern fringe of this line of Ðlaments (see Fig.…”

Section: Arge-scale Reverse Shock Featuresmentioning

confidence: 85%

“…1 east, and southeast by red [S III] bright emission, appears kinematically to be a single, coherent ringlike structure. When sampled via its [S II] jj6716, 6731 emission, this ring spans a radial velocity range from [2700 km s~1 in the southwest to [900 km s~1 in the north, with a characteristic mean around [1800 km s~1 (Lawrence et al 1995). The ringÏs most blueshifted material ([2700^300 km s~1) is the orangish-colored features near the peak-like Ðlament at the bottom of the ring and extends westward to just south of the bright double stars.…”

Section: Main Shell Structurementioning

confidence: 99%

“…High-velocity, radiative ejecta Ðlaments and FMKsÈwhich exhibit strong O, S, and Ar lines but no H, He, or N emissionÈdominate the SNRÏs optical structure and are mainly organized in large ringlike structures (diameters D0.5È1.0 pc) situated on the surface of the expanding shell (Reed et al 1991 ;Lawrence et al 1995). Fainter optical ejecta have been found outside of the shell, mainly located in a northeastern Ñare or "" jet ÏÏ of S-rich ejecta, with some 70] other fainter knots elsewhere around the remnantÏs outer periphery (see Fesen 2001, and references therein).…”

Section: Introductionmentioning

confidence: 99%

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