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Optical observations of the young supernova remnant SNR 0540-69.3 and its pulsar
Stockholm University, Faculty of Science, Department of Astronomy.
Stockholm University, Faculty of Science, Department of Astronomy.
Stockholm University, Faculty of Science, Department of Astronomy.
2005 (English)In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 35, no 6, 1106-1111 p.Article in journal (Refereed) Published
Abstract [en]

We have used the ESO NTT/EMMI and VLT/FORS1 instruments to examine the LMC supernova remnant 0540-69.3 as well as its pulsar (PSR B0540-69) and pulsar-powered nebula in the optical range. Spectroscopic observations of the remnant covering the range of 3600 7350 Å centered on the pulsar produced results consistent with those of [Kirshner, R.P., Morse, J.A., Winkler, P.F., et al. The penultimate supernova in the Large Magellanic Cloud - SNR 0540-69.3. Astrophys.J. 342, 260 271, 1989.] but also revealed many new emission lines. The most important are [Ne III] λλ3869, 3967 and Balmer lines of hydrogen. In both the central part of the remnant, as well as in nearby H II regions, the [O III] temperature is higher than ˜2 × 104 K, but lower than previously estimated. For PSR B0540-69, previous optical data are mutually inconsistent: HST/FOS spectra indicate a significantly higher absolute flux and steeper spectral index than suggested by early time-resolved groundbased UBVRI photometry. We show that the HST and VLT spectroscopic data for the pulsar have ≳50% nebular contamination, and that this is the reason for the previous difference. Using HST/WFPC2 archival images obtained in various bands from the red part of the optical to the NUV range we have performed an accurate photometric study of the pulsar, and find that the spectral energy distribution of the pulsar emission has a negative slope with α=1.07-0.19+0.20. This is steeper than derived from previous UBVRI photometry, and also different from the almost flat spectrum of the Crab pulsar. We also estimate that the proper motion of the pulsar is 4.9 ± 2.3 mas year‑1, corresponding to a transverse velocity of 1190 ± 560 km s‑1, projected along the southern jet of the pulsar nebula.

Place, publisher, year, edition, pages
2005. Vol. 35, no 6, 1106-1111 p.
Keyword [en]
Supernova remnants, Pulsars, Spectroscopy, Photometry, Astrometry, Supernova remnants: individual: SNR 0540-69.3, Pulsars: individual: PSR B0540-69.3
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Astronomy
Identifiers
URN: urn:nbn:se:su:diva-30952DOI: 10.1016/j.asr.2005.01.071OAI: oai:DiVA.org:su-30952DiVA: diva2:274787
Available from: 2009-11-01 Created: 2009-11-01 Last updated: 2017-12-12Bibliographically approved
In thesis
1. Supernova remnants and their pulsar wind nebulae
Open this publication in new window or tab >>Supernova remnants and their pulsar wind nebulae
2012 (English)Doctoral thesis, comprehensive summary (Other academic)
Abstract [en]

Massive stars die in powerful stellar explosions, so-called supernovae. In most cases, a neutron star or a black hole is expected to form in the center. The ejected material in these explosions expands out into the surroundings for tens of thousands of years, forming a supernova remnant. If a rapidly rotating neutron star, i.e. pulsar, has been created in the center, a pulsar wind nebula (PWN) will form around it. This thesis focuses mainly on the composite supernova remnant SNR B0540-69.3, as well as the pulsar\psr. This object has a dynamical PWN for which detailed observations have been done using various ground-based and space-borne telescopes. The thesis also includes a detailed study of the Crab-like supernova remnant 3C 58, which allowed us to detect optical emission from the pulsar+PWN system. This made it become the third PWN, after the Crab nebula and the 0540 PWN, to be seen in the optical.

Place, publisher, year, edition, pages
Stockholm: Department of Astronomy, Stockholm University, 2012. 44 p.
Keyword
pulsars, supernovae, ISM
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Astronomy
Identifiers
urn:nbn:se:su:diva-79103 (URN)978-91-7447-466-4 (ISBN)
Public defence
2012-09-24, FA32, AlbaNova universitetscentrum, Roslagstullsbacken 21, Stockholm, 10:00 (English)
Opponent
Supervisors
Available from: 2012-09-03 Created: 2012-08-27 Last updated: 2012-09-03Bibliographically approved

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