The radio structure of supernova remnant 0540-693

Manchester, R. N.; Staveley‐Smith, L.; Kesteven, M. J.

doi:10.1086/172877

Cited by 62 publications

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“…0077. This is only a factor of ∼1.5 larger than the yearly proper motion value reported by Manchester et al (1993b), see Table 1. This allows a direct estimate of the proper motion of the pulsar using accurate superposition of the F555W and F547M images taken at epochs separated by 4 years (see Sect.…”

Section: Proper Motion and Astrometrymentioning

confidence: 53%

“…Even the structures of the PWNe appear to be similar. Both have a torus and jets (Gotthelf & Wang 2000), although the proper motion for PSR B0540-69.3, suggested by Manchester et al (1993b) based on a displacement between the pulsar optical position • 7 −31.…”

Section: Introductionmentioning

confidence: 99%

“…There are, however, differences on a larger scale. While the PWN of PSR B0540-69.3 is surrounded by an X-ray and radio emitting outer shell of radius ∼30 , or ∼7.3 pc (Manchester et al 1993b;Gotthelf & Wang 2000), an outer shell around the Crab is still not confirmed (although high-velocity gas has been revealed in the UV, Sollerman et al 2000). Another difference is that SNR 0540-69.3 is oxygen-rich (e.g., Kirshner et al 1989;Serafimovich et al 2004), whereas the Crab Nebula has nearly normal solar abundances of metals (Blair et al 1992, and references therein).…”

Section: Introductionmentioning

confidence: 99%

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The young pulsar PSR B0540-69.3 and its synchrotron nebula in the optical and X-rays

Serafimovich¹,

Shibanov²,

Lundqvist³

et al. 2004

A&A

184

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Abstract. The young PSR B0540-69.3 in the LMC is the only pulsar (except the Crab pulsar) for which a near-UV spectrum has been obtained. However, the absolute flux and spectral index of the HST/FOS spectrum are significantly higher than suggested by previous broad-band time-resolved groundbased UBVRI photometry. To investigate this difference, observations with ESO/VLT/FORS1 and analysis of HST/WFPC2 archival data were done. We show that the HST and VLT spectral data for the pulsar have > ∼ 50% nebular contamination and that this is the reason for the above-mentioned difference. The broadband HST spectrum for the range 3300-8000 Å is clearly nonthermal and has a negative spectral index, F ν ∝ ν −α with α ν = 1.0719 . This is different from the almost flat spectrum of the Crab pulsar, and also steeper than for the previously published broadband photometry of PSR B0540-69.3. We have also studied the spatial variations of the brightness and spectral index of the Pulsar Wind Nebula (PWN) around the pulsar, and find no significant spectral index variation over the PWN. The HST data show a clear asymmetry of the surface brightness distribution along the major axis of the torus-like structure of the PWN with respect to the pulsar position, also seen in Chandra/HRC X-ray images. This is different from the Crab PWN and likely linked to the asymmetry of the surrounding SN ejecta. The HST/WFPC2 archival data have an epoch separation of 4 years, and this allows us to estimate the proper motion of the pulsar. We find a motion of 4.9 ± 2.3 mas yr −1 (corresponding to a transverse velocity of 1190 ± 560 km s −1 ) along the southern jet of the PWN. If this is confirmed at a higher significance level by future observations, this makes PSR B0540-69.3 the third pulsar with a proper motion aligned with the jet axis of its PWN, which poses constraints on pulsar kick models. To establish the multiwavelength spectrum of the pulsar and its PWN, we have included recent Chandra X-ray data, and discuss the soft pulsar X-ray spectrum based on spectral fits including absorption by interstellar gas in the Milky Way, LMC as well as the supernova ejecta. We have compared the multiwavelength spectra of PSR B0540-69.3 and the Crab pulsar, and find that both PSR B0540-69.3 and the Crab pulsar have a weaker flux in the optical than suggested by a low-energy power-law extension of the X-ray spectrum. This optical depression is more severe for PSR B0540-69.3 than for the Crab pulsar. The same trend is seen for the PWNe of the two pulsars, and continues for low energies also out in the radio band. We discuss possible interpretations of this behavior.

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Section: Proper Motion and Astrometrymentioning

confidence: 53%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The young pulsar PSR B0540-69.3 and its synchrotron nebula in the optical and X-rays

Serafimovich¹,

Shibanov²,

Lundqvist³

et al. 2004

A&A

184

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“…2) the flux density decreases as expected whereas at lower frequencies non-thermal radiation of the shell dominates. Overall, the radio-continuum properties of SNR J0453-6829 are very similar to SNR B0540-693, the most prominent SNR with a PWN in the LMC (Manchester et al 1993). Mathewson et al (1983) found distinctive optical connections to X-ray and radio features of this SNR.…”

Section: Discussionmentioning

confidence: 76%

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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“…A double-knee break between the optical and X-rays is not excluded either (Serafimovich et al 2005). At the same time, the IR part of the G21.5-09 spectrum is probably almost 3 The data are taken for the Crab from Green et al (2004), Temim et al (2006), Grasdalen (1979), Veron-Cetty & Woltjer (1993), and Kirsch et al (2005); for G21.5-0.9 from Zajczyk et al (2012); for B0540-69.3 from Manchester et al (1993), Williams et al (2008), Mignani et al (2012), and Serafimovich et al (2005); for 3C 58 from Shibanov et al (2008), Shearer & Neustroev (2008), and Slane et al (2008). 4 We indicate in the plot the SNR (870 yr, Bietenholz & Bartel 2008) and spindown (4800 yr, Camilo et al 2006) ages for this PWN.…”

Section: Multiwavelength Spectrum Of the Torus-like Pwnmentioning

confidence: 99%

The PSR J1124-5916 wind nebula in the near-infrared

Zharikov

Zyuzin²,

Shibanov

et al. 2013

A&A

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Context. The young radio pulsar J1124-5916 is associated with the Cas A like supernova remnant G292.0+1.8. It powers a compact torus-like pulsar wind nebula with a jet first detected in X-rays and then identified in the optical and mid-infrared. Aims. We carried out deep near-infrared observations of the pulsar field to identify the pulsar and its nebula in this range. Methods. The direct-imaging mode of the NACO adaptive optics instrument at the ESO VLT in the H and K s bands was used.Results. We detected a faint, H = 21.30(10) and K s = 20.45(10), extended elliptical object in both bands, whose center position is consistent with the X-ray position of the pulsar. The morphology of the object and the orientation of its major axis agree well with those observed for the pulsar torus-like nebula in the mid-infrared, optical, and X-rays. This suggests that it is the near-infrared counterpart of the nebula. The measured fluxes compiled with the data in other ranges show a complicated unabsorbed power-law spectrum of the torus-like nebula with several steep breaks between the near-infrared and mid-infrared, the optical and X-rays, and possibly in the mid-infrared. This implies a multiple relativistic particle population responsible for the synchrotron emission of the nebula in different spectral ranges. We have not resolved the pulsar counterpart from its nebula and place only upper limits on its brightness, H ≥ 23.9 and K s ≥ 22.7. Based on that, its contribution to the total near-infrared flux of the pulsar+nebula system is ≤10%, which is comparable with the expected contribution in the optical.

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The radio structure of supernova remnant 0540-693

Cited by 62 publications

References 0 publications

The young pulsar PSR B0540-69.3 and its synchrotron nebula in the optical and X-rays

The young pulsar PSR B0540-69.3 and its synchrotron nebula in the optical and X-rays

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

The PSR J1124-5916 wind nebula in the near-infrared

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