Supernova remnants in the Large Magellanic Cloud - A photographic study in /O III/ and /S II/

Lasker, B. M.

doi:10.1086/130147

Cited by 11 publications

(6 citation statements)

References 6 publications

(16 reference statements)

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“…Perhaps the most famous known concentration of superbubbles lies in the LMC, as shown by observations dating back from the late seventies, although at the time they were simply called SNRs (e.g., Lasker 1977). Early Einstein observations revealed the presence of many previously unknown X-ray emitting superbubbles, of diameter ∼ 100 pc or more, and X-ray luminosities L X ∼ 1 − 10 × 10 35 erg s −1 (e.g., Chu & Mac Low 1990), so in the same range as the predicted X-ray luminosity of the CMa shell alone.…”

Section: A Cma Superbubble ?mentioning

confidence: 99%

Runaways and shells around the CMa OB1 association

Fernandes

Montmerle

Santos-Silva

et al. 2019

A&A

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Context. The origin of the arc-shaped Sh 2-296 nebula is still unclear. Mainly due to its morphology, the nebula has been suggested to be a 0.5 Myr-old supernova remnant (SNR) that could be inducing star formation in the CMa OB1 association. Therefore, this region can be an excellent laboratory for the investigation of the influence of massive stars on their surroundings. Aims. We aim to show, for the first time, that the nebula is part of a large, shell-like structure, which we have designated the "CMa shell", enclosing a bubble created by successive supernova (SN) explosions. We identified three runaway stars, associated with bowshock structures, in the direction of the CMa shell and we investigate the possibility that they have originated in the center of the shell. Methods. By analyzing images of the CMa OB1 association at several wavelengths, we clearly see that the Sh 2-296 nebula is in fact part of a large structure, which can be approximated by a large (with a diameter of ∼ 60 pc) elliptical shell. Using the recent Gaia-DR2 astrometric data, we trace back the path of the three runaway stars, in order to find their original position in the past, with relation to the CMa shell. We also revise the heating and ionization of the Sh 2-296 nebula, by comparing the photon budget provided by the O stars in the region with results from radio observations. Results. We find that the runaway stars have likely been ejected from a Trapezium-like progenitor cluster on three successive SN explosions having taken place ∼ 6, ∼ 2 and ∼ 1 Myr ago. We also show that the few late-type O stars in the region cannot explain the ionization of the Sh 2-296 nebula and other mechanisms need to be at work. Conclusions. We argue that, though we now have evidence for several SNe events in the CMa OB1 association, the SNe probably played a minor role in triggering star formation in these clouds. In contrast, the CMa OB1 association, as it is now, likely testifies to the last stages of a star-forming region.

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Section: A Cma Superbubble ?mentioning

confidence: 99%

Runaways and shells around the CMa OB1 association

Fernandes

Montmerle

Santos-Silva

et al. 2019

A&A

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“…The SNR N186 D appears at the northern edge of DEM L50. The fact that N186 D is detected in [Oiii] while DEM L50 is not suggests they may be two physically distinct objects (Lasker 1977); similar Hi kinematics in both objects, however, may indicate that the SNR is associated with the larger bubble (Oey et al 2002), and thus the exact relationship between the SNR and the superbubble remains unclear. SNR N186 D's X-ray spectra can be fit by a nonequilibrium model or a two-temperature equilibrium model.…”

Section: Snrsmentioning

confidence: 99%

Observational Constraints on Superbubble X-Ray Energy Budgets

Jaskot

Strickland

Oey

et al. 2011

ApJ

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The hot, X-ray-emitting gas in superbubbles imparts energy and enriched material to the interstellar medium (ISM) and generates the hot ionized medium, the ISM's high-temperature component. The evolution of superbubble energy budgets is not well understood, however, and the processes responsible for enhanced X-ray emission in superbubbles remain a matter of debate. We present Chandra ACIS-S observations of two X-ray-bright superbubbles in the Large Magellanic Cloud (LMC), DEM L50 (N186) and DEM L152 (N44), with an emphasis on disentangling the true superbubble X-ray emission from non-related diffuse emission and determining the spatial origin and spectral variation of the X-ray emission. An examination of the superbubble energy budgets shows that on the order of 50% of the X-ray emission comes from regions associated with supernova remnant (SNR) impacts. We find some evidence of mass-loading due to swept-up clouds and metallicity enrichment, but neither mechanism provides a significant contribution to the X-ray luminosities. We also find that one of the superbubbles, DEM L50, is likely not in collisional ionization equilibrium. We compare our observations to the predictions of the standard Weaver et al. model and to 1-D hydrodynamic simulations including cavity supernova impacts on the shell walls. Our observations show that mass-loading due to thermal evaporation from the shell walls and SNR impacts are the dominant source of enhanced X-ray luminosities in superbubbles. These two processes should affect most superbubbles, and their contribution to the X-ray luminosity must be considered when determining the energy available for transport to the ISM.

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“…1v).ÈThis remnant shows optical extensions to the north and south, including Ðlaments that appear to be streaming out from the SNR. [O III] and [S II] images taken by Lasker (1977) show northern and southern extensions of N86 that might represent breakouts. The elongated X-ray morphology follows these optical features fairly closely, suggesting that the irregular X-ray structure is due to breakouts of the hot gas into cavities in the surrounding ISM (Paper II).…”

Section: Appendix a Individual Snr Properties And Referencesmentioning

confidence: 99%

Supernova Remnants in the Magellanic Clouds. III. An X‐Ray Atlas of Large Magellanic Cloud Supernova Remnants

Williams

Chu

Dickel

et al. 1999

ASTROPHYS J SUPPL S

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We have used archival ROSAT data to present X-ray images of 31 supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). We have classiÐed these remnants according to their X-ray morphologies, into the categories of shell-type, di †use face, centrally brightened, point-sourceÈdominated, and irregular. We suggest possible causes of the X-ray emission for each category and for individual features of some of the SNRs.

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Supernova remnants in the Large Magellanic Cloud - A photographic study in /O III/ and /S II/

Cited by 11 publications

References 6 publications

Runaways and shells around the CMa OB1 association

Runaways and shells around the CMa OB1 association

Observational Constraints on Superbubble X-Ray Energy Budgets

Supernova Remnants in the Magellanic Clouds. III. An X‐Ray Atlas of Large Magellanic Cloud Supernova Remnants

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