Statistics of Galactic Supernova Remnants

Xu, Jianwen; Zhang, Xizhen; Han, J. L.

doi:10.1088/1009-9271/5/2/007

Cited by 38 publications

(57 citation statements)

References 39 publications

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“…To estimate the age of the SNR from the vpshock model we used the relation t y = 3.8 × 10 2 R pc (kT ) −1/2 keV from Xu et al (2005) and assume the temperature derived from X-ray spectral modelling (0.25 keV) and the radius of the SNR, which results in ∼11.8 kyr, consistent with the age inferred by Gaensler et al (2003) from a preliminary X-ray spectral modelling. Also using a similar Sedov model and following Owen et al (2011) who applied it to the spectrum of the SMC SNR IKT 16, we derive -with a shock temperature of 0.17 keV, and the normalisation of the Sedov model fit of 3.74 × 10 −2 cm −5 -the following physical parameters for SNR J0453-6829: electron density in the X-ray emitting material of 1.56 cm −3 , dynamical age of 15.2 kyr, swept-up mass of 830 M and an explosion energy of 7.6 × 10 50 erg.…”

Section: Discussionmentioning

confidence: 95%

Multi-frequency observations of SNR J0453–6829 in the LMC

Haberl

Filipović

Bozzetto

et al. 2012

A&A

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Context. The Large Magellanic Cloud (LMC) is rich in supernova remnants (SNRs), which can be investigated in detail with radio, optical, and X-ray observations. SNR J0453-6829 is an X-ray and radio-bright remnant in the LMC, within which previous studies revealed the presence of a pulsar wind nebula (PWN), making it one of the most interesting SNRs in the Local Group of galaxies. Aims. We study the emission of SNR J0453-6829 to improve our understanding of its morphology, spectrum, and thus the emission mechanisms in the shell and the PWN of the remnant. Methods. We obtained new radio data with the Australia Telescope Compact Array and analysed archival XMM-Newton observations of SNR J0453-6829. We studied the morphology of SNR J0453-6829 from radio, optical, and X-ray images and investigated the energy spectra in the different parts of the remnant. Results. Our radio results confirm that this LMC SNR hosts a typical PWN. The prominent central core of the PWN exhibits a radio spectral index α Core of −0.04 ± 0.04, while in the rest of the SNR shell the spectral slope is somewhat steeper with α Shell = −0.43 ± 0.01. We detect regions with a mean polarisation of P (12 ± 4)% at 6 cm and (9 ± 2)% at 3 cm. The full remnant is of roughly circular shape with dimensions of (31 ± 1) pc × (29 ± 1) pc. The spectral analysis of the XMM-Newton EPIC and RGS spectra allowed us to derive physical parameters for the SNR. Somewhat depending on the spectral model, we obtain for the remnant a shock temperature of around 0.2 keV and estimate the dynamical age to 12 000-15 000 years. Using a Sedov model we further derive an electron density in the X-ray emitting material of 1.56 cm −3 , typical for LMC remnants, a large swept-up mass of 830 M , and an explosion energy of 7.6 × 10 50 erg. These parameters indicate a well evolved SNR with an X-ray spectrum dominated by emission from the swept-up material.

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Section: Discussionmentioning

confidence: 95%

Multi-frequency observations of SNR J0453–6829 in the LMC

Haberl

Filipović

Bozzetto

et al. 2012

A&A

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“…While SNRs can usually be seen for at most a few 10 5 years in X-rays and radio (for the methods used to estimate SNR ages see e.g. Xu et al 2005), BeXRBs are expected to become X-ray active much later (see below). Using the relation t y = 3.8 × 10 2 R pc (kT ) −1/2 keV from Xu et al (2005) of temperature derived from X-ray spectral modelling (0.23 keV) and the size of the SNR (∼2.5 in diameter, corresponding to ∼40 pc at a distance of 60 kpc), we estimate the age of the SNR to ∼16 ky.…”

Section: Discussionmentioning

confidence: 99%

“…Xu et al 2005), BeXRBs are expected to become X-ray active much later (see below). Using the relation t y = 3.8 × 10 2 R pc (kT ) −1/2 keV from Xu et al (2005) of temperature derived from X-ray spectral modelling (0.23 keV) and the size of the SNR (∼2.5 in diameter, corresponding to ∼40 pc at a distance of 60 kpc), we estimate the age of the SNR to ∼16 ky. If one compares the ages estimated for SNRs in the SMC by van der Heyden et al (2004) with their sizes as listed in Badenes et al (2010), one finds ages of at most 25 ky for remnants with diameters around 40-50 pc.…”

Section: Discussionmentioning

confidence: 99%

SXP 1062, a young Be X-ray binary pulsar with long spin period

Haberl

Sturm

Filipović

et al. 2011

A&A

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Context. The Small Magellanic Cloud (SMC) is ideally suited to investigating the recent star formation history from X-ray source population studies. It harbours a large number of Be/X-ray binaries (Be stars with an accreting neutron star as companion), and the supernova remnants can be easily resolved with imaging X-ray instruments. Aims. We search for new supernova remnants in the SMC and in particular for composite remnants with a central X-ray source. Methods. We study the morphology of newly found candidate supernova remnants using radio, optical and X-ray images and investigate their X-ray spectra.Results. Here we report on the discovery of the new supernova remnant around the recently discovered Be/X-ray binary pulsar CXO J012745.97−733256.5 = SXP 1062 in radio and X-ray images. The Be/X-ray binary system is found near the centre of the supernova remnant, which is located at the outer edge of the eastern wing of the SMC. The remnant is oxygen-rich, indicating that it developed from a type Ib event. From XMM-Newton observations we find that the neutron star with a spin period of 1062 s (the second longest known in the SMC) shows a very high average spin-down rate of 0.26 s per day over the observing period of 18 days. Conclusions. From the currently accepted models, our estimated age of around 10 000−25 000 years for the supernova remnant is not long enough to spin down the neutron star from a few 10 ms to its current value. Assuming an upper limit of 25 000 years for the age of the neutron star and the extreme case that the neutron star was spun down by the accretion torque that we have measured during the XMM-Newton observations since its birth, a lower limit of 0.5 s for the birth spin period is inferred. For more realistic, smaller long-term average accretion torques our results suggest that the neutron star was born with a correspondingly longer spin period. This implies that neutron stars in Be/X-ray binaries with long spin periods can be much younger than currently anticipated.

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“…where d = 0.58 and e = 0.083kpc (Xu et al 2005). Assuming the SNR and PSR distributions plotted in Fig.2, the Galaxy should contain 217 SNRs and 13176 PSRs.…”

Section: Galactic Spatial Distributions Of Psrs and Snrs And Their Vhmentioning

confidence: 98%

Constraints on the TeV source population and its contribution to the galactic diffuse TeV emission

Casanova

Dingus

2008

Astroparticle Physics

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The detection by the HESS atmospheric Cerenkov telescope of fourteen new sources from the Galactic plane makes it possible to estimate the contribution of unresolved sources like those detected by HESS to the diffuse Galactic emission measured by the Milagro Collaboration. The number-intensity relation and the luminosity function for the HESS source population are investigated. By evaluating the contribution of such a source population to the diffuse emission we conclude that a significant fraction of the TeV energy emission measured by the Milagro experiment could be due to unresolved sources like HESS sources. Predictions concerning the number of sources which Veritas, Milagro, and HAWC should detect are also given.

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Statistics of Galactic Supernova Remnants

Cited by 38 publications

References 39 publications

Multi-frequency observations of SNR J0453–6829 in the LMC

Multi-frequency observations of SNR J0453–6829 in the LMC

SXP 1062, a young Be X-ray binary pulsar with long spin period

Constraints on the TeV source population and its contribution to the galactic diffuse TeV emission

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