XMM-Newton observation of the Tycho supernova remnant

Decourchelle, A.; Sauvageot, J.-L.; Audard, M.; Aschenbach, B.; Sembay, S.; Rothenflug, R.; Ballet, J.; Stadlbauer, T.; West, R. G.

doi:10.1051/0004-6361:20000115

Cited by 123 publications

(144 citation statements)

References 29 publications

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“…The isolated X-ray emitting ejecta fragments were discovered in the middle-aged Vela SNR (Aschenbach et al 1995) and also in type Ia Tycho SNR (e.g. Decourchelle et al 2001). A model of X-ray line emission from fast moving ejecta fragments predicts that the fragments interacting with molecular clouds are the brightest and they could be detected from a few kpc distances (Bykov 2002).…”

Section: Have Established Thementioning

confidence: 99%

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XMM-Newton study of hard X-ray sources in IC 443

Bocchino

Bykov

2003

A&A

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Abstract. We present XMM-Newton observations of hard X-ray emission from the field of IC 443, a supernova remnant interacting with a molecular cloud. The hard emission from the field is dominated by 12 isolated sources having 2-10 keV flux > ∼ 10 −14 erg cm −2 s −1 . Only a fraction of the sources are expected to be extragalactic or stars on statistical grounds, while the others may be associated with the remnant. We have analyzed near-infrared K band and also DSS optical data for all of the detected sources, finding that six X-ray sources are located in a relatively small 15 × 15 region where there is strong 2.2 µm infrared emission, indicating interaction with a molecular cloud. The source 1SAX J0618.0+2227, the brightest in this region (excluding the plerion), is resolved with XMM-Newton into two sources, one of which is extended and has a hard power law spectrum photon index < ∼ 1.5) and shows some indications of spectral line signatures (e.g. Si), while the other is point-like and has a featureless spectrum of steeper photon index ∼2.2. Possible interpretations of some of the discrete sources in terms of interaction between the SNR and the molecular cloud are discussed.

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Section: Have Established Thementioning

confidence: 99%

“…Some X-ray knots, e.g. the silicon-rich shrapnel, were observed in the Vela SNR by Aschenbach et al (1995) and Miyata et al (2001) and also in the Tycho SNR with XMM-Newton by Decourchelle et al (2001). Supersonic motion of the knots in the ambient medium will result in a bow shock/knot-shock structure creation.…”

Section: Fast-moving Isolated Ejecta Fragmentsmentioning

confidence: 99%

XMM-Newton study of hard X-ray sources in IC 443

Bocchino

Bykov

2003

A&A

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“…While Tycho's SNR is the prototype of a type Ia SN, Kepler's SNR is probably a type Ia as well, but with substantial circumstellar material (Reynolds et al 2007). In both remnants, a radial onion elemental structure is roughly preserved with iron toward the inner region and silicon in the outer ones (Decourchelle et al 2001;Cassam-Chenaï et al 2004a). Conversely, in the core-collapse supernova Cas A, there is an important spatial inversion of a significant portion of the SN core (Hughes et al 2000a).…”

Section: Nucleosynthesis Productsmentioning

confidence: 98%

Supernova remnants, planetary nebulae and superbubbles: Prospects for new XMM‐Newton observations

Decourchelle¹

2008

Astron Nachr

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“…First, owing to its high Galactic latitude (b = 14.6 • ), the foreground extinction to SN1006 is relatively low (N H = 6.8 × 10 20 cm −2 ; Dubner et al * E-mail:pandataotao@gmail.com 2002) among the Galactic SNRs. Therefore, soft X-ray emission lines from some relatively light elements, for example, oxygen, are particularly strong compared to other young SNRs of the same type (e.g., the Tycho's SNR; Decourchelle et al 2001;G1.9+0.3;Borkowski et al 2013). Second, the density of the surrounding medium of SN1006 is low (n 0 ∼ 0.3 cm −3 ; Dubner et al 2002).…”

Section: Introductionmentioning

confidence: 99%

XMM–Newtonlarge programme on SN1006 – II. Thermal emission

Li¹,

Decourchelle²,

Miceli³

et al. 2016

Mon. Not. R. Astron. Soc.

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Based on the XMM-Newton large program on SN1006 and our newly developed tools for spatially resolved spectroscopy analysis as described in Li et al. (2015) (Paper I), we study the thermal emission from ISM and ejecta of SN1006 by analyzing the spectra extracted from 583 tessellated regions dominated by thermal emission. With some key improvements in spectral analysis as compared to Paper I, we obtain much better spectral fitting results with significantly less residuals. The spatial distributions of the thermal and ionization states of the ISM and ejecta show significantly different features, which are in general consistent with a scenario that the ISM (ejecta) is heated and ionized by the forward (reverse) shock propagating outward (inward). Different heavy elements show different spatial distributions so different origins, with Ne mostly from the ISM, Si and S mostly from the ejecta, and O and Mg from both the ISM and ejecta. Fe L-shell line emissions are only detected in a small shell-like region SE to the center of SN1006, indicating that most of the Fe-rich ejecta has not yet or just recently been reached by the reverse shock. The overall abundance patterns of the ejecta for most of the heavy elements, except for Fe and sometimes for S, are consistent with typical Type Ia SN products. The NW half of the SNR interior between the NW shell and the soft X-ray brighter SE half probably represents a region with turbulently mixed ISM and ejecta, so has enhanced emission from O, Mg, Si, and S, lower ejecta temperature, and a large diversity of ionization age. In addition to the asymmetric ISM distribution, an asymmetric explosion of the progenitor star is also needed to explain the asymmetric ejecta distribution.

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XMM-Newton observation of the Tycho supernova remnant

Cited by 123 publications

References 29 publications

XMM-Newton study of hard X-ray sources in IC 443

XMM-Newton study of hard X-ray sources in IC 443

Supernova remnants, planetary nebulae and superbubbles: Prospects for new XMM‐Newton observations

XMM–Newtonlarge programme on SN1006 – II. Thermal emission

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