A radio model of the 30 Doradus region

Mills, B. Y.; Turtle, A. J.; Watkinson, Anne

doi:10.1093/mnras/185.2.263

Cited by 39 publications

(20 citation statements)

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“…However, well away from the 30 Doradus nebula itself, low levels of emission are easily detected and the sensitivity is comparable to that shown in Figure I. The whole region has been discussed by Mills et al (1978) and it was shown that the radio emission is predominantly thermal, arising from the numerous H II regions. The present results confirm the main features of the earlier 1415 MHz map obtained with the Fleurs Synthesis Telescope but the greater sensitivity reveals many new correspondences with fainter Ha emission features.…”

Section: The 30 Doradus Regionmentioning

confidence: 63%

A Radio Continuum Survey of the Magellanic Clouds

Mills

Turtle

1984

Symp. - Int. Astron. Union

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Continuum radio emission from the Large Magellanic Cloud was first detected just 30 years ago (Mills & Little, 1953). Subsequently, surveys of the Clouds were made after each new advance in southern hemisphere instrumentation and the principal surveys are listed and briefly described in Table I. They cover a range of frequencies from 19.7 MHz to 8.4 GHz. The early surveys at low frequencies were chiefly concerned with the overall synchrotron emission from the Clouds but, as resolution improved, emphasis has shifted to the individual sources, both emission nebulae and supernova remnants, which can be recognized as Cloud members. Of recent years the unique position of the Clouds for studying radio sources in external galaxies has been undermined by the development of powerful synthesis telescopes in the northern hemisphere; these have provided equivalent sensitivity and better spatial resolution on M31, and several other northern galaxies can also be studied effectively. However, with the commissioning of the Molonglo Observatory Synthesis Telescope (MOST) in 1981 the Clouds have been restored to their rightful place befitting the closest galaxies.

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Section: The 30 Doradus Regionmentioning

confidence: 63%

A Radio Continuum Survey of the Magellanic Clouds

Mills

Turtle

1984

Symp. - Int. Astron. Union

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“…The complex was first recognized to contain an SNR through its Crab-like radio spectrum (Le Marne 1968;Mills et al 1978), which was later confirmed by others (e.g. Dickel et al 1994).…”

Section: Lmc: N157bmentioning

confidence: 69%

The physical structure of Magellanic Cloud HII regions

Vermeij¹,

Damour²,

Hulst³

et al. 2002

A&A

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Abstract. We present infrared and optical spectroscopic data for 11 H  regions and one Supernova Remnant in the Large and Small Magellanic Cloud. The infrared data have been obtained with the Short Wavelength Spectrometer and Long Wavelength Spectrometer on board the Infrared Space Observatory as part of a Guaranteed Time Program on H  regions in Local Group Galaxies. Aim of this project is to give a new and improved analysis of the physical structure of the sample H  regions by combining as much spectral data as possible. A detailed account is given here of the reduction process, and the quality and reliability of the presented fluxes are discussed.

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“…The spectral characteristics are most similar to those of N157B. Based on its radio and X-ray spectra, N157B has been identified as a Crab-type SNR (Mills, Turtle, & Watkinson 1978;Clark et al 1982;Mathewson et al 1983), and it is known to contain a pulsar (Marshall et al 1998). Based on the spectral similarities between MF16 and N157B, we suspect that a significant portion of the X-ray luminosity of MF16 is contaminated by a non-thermal-plasma source.…”

Section: Luminosity Considerationmentioning

confidence: 89%

What Produced the Ultraluminous Supernova Remnant in NGC 6946?

Dunne

Gruendl

Chu

2000

The Astronomical Journal

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The ultraluminous supernova remnant (SNR) in NGC 6946 is the brightest known SNR in X-rays, ~1000 times brighter than Cas A. To probe the nature of this remnant and its progenitor, we have obtained high-dispersion optical echelle spectra. The echelle spectra detect H-alpha, [N II], and [O III] lines, and resolve these lines into a narrow (FWHM ~20--40 km/s) component from un-shocked material and a broad (FWHM ~250 km/s) component from shocked material. Both narrow and broad components have unusually high [N II]/H-alpha ratios, ~1. Using the echelle observation, archival HST images, and archival ROSAT X-ray observations, we conclude that the SNR was produced by a normal supernova, whose progenitor was a massive star, either a WN star or a luminous blue variable. The high luminosity of the remnant is caused by the supernova ejecta expanding into a dense, nitrogen-rich circumstellar nebula created by the progenitor.Comment: 20 pages, 5 figures. To be published in The Astronomical Journal, March 200

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A radio model of the 30 Doradus region

Cited by 39 publications

References 0 publications

A Radio Continuum Survey of the Magellanic Clouds

A Radio Continuum Survey of the Magellanic Clouds

The physical structure of Magellanic Cloud HII regions

What Produced the Ultraluminous Supernova Remnant in NGC 6946?

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