The Radio Continuum of the Large Magellanic Cloud. I. The Sources at 6 cm Wavelength

McGee, R. X.; Brooks, JW; Batchelor, R.

doi:10.1071/ph720581

Cited by 42 publications

(19 citation statements)

References 5 publications

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“…We compared our data with several single dish surveys of the LMC, the Molonglo observations at 408 MHz (Clarke et al 1976) and the Parkes observations at 5 GHz (McGee et al 1972a) and 4.75 GHz (Filipovic et al 1995). We identify sources of the ATCA catalogue with objects listed in the Molonglo Radio Source Catalogue 4, if the difference in position is smaller than the HPBW of the Molonglo telescope (2.…”

Section: Comparison With Radio Observationsmentioning

confidence: 99%

A catalogue of compact radio sources in and behind the Large Magellanic Cloud

Marx

Dickey

Mebold

1997

Astron. Astrophys. Suppl. Ser.

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Abstract. We present the results of a continuum snapshot survey of a 3• × 4• region of the Large Magellanic Cloud including the area of the giant molecular cloud and the 30 Doradus nebula. The observations have been carried out with the Australia Telescope Compact Array (ATCA) 1 at 1.4 and 2.4 GHz. Most fields are complete to about 6 mJy peak flux density at 1.4 GHz and to about 3 mJy at 2.4 GHz. The positions, peak and integral flux densities of 113 compact (< 54 ) sources detected at 1.4 GHz and of 70 sources (< 34 ) detected at 2.4 GHz are presented. Positions are accurate to about 3 and peak flux densities are accurate to about 10% or better, depending on the source position relative to the pointing centers. 32 of the sources detected at 1.4 GHz are coincident with Hα objects in the catalogue of Davies et al.; these are possibly intrinsic to the LMC. However, we suppose that most are background objects, since the number vs. flux agrees with predictions of extragalactic source counts from other surveys.

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Section: Comparison With Radio Observationsmentioning

confidence: 99%

A catalogue of compact radio sources in and behind the Large Magellanic Cloud

Marx

Dickey

Mebold

1997

Astron. Astrophys. Suppl. Ser.

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“…We combined our flux density values with those of previous radio observations at various frequencies ( McGee et al 1972;Clarke et al 1976;Mathewson et al 1985;Filipovic et al 1995;Bock et al 1999) and used a linear regression fit (log frequency vs. log flux density) to obtain a spectral index for the SNR of À0.21 (Table 1, Fig. 6).…”

Section: Radio Emissionmentioning

confidence: 99%

Supernova Remnants in the Magellanic Clouds. IV. X‐Ray Emission from the Largest Supernova Remnant in the Large Magellanic Cloud

Williams¹,

Chu²,

Dickel³

et al. 2004

ApJ

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We present the first X-ray detection of SNR 0450À70.9, the largest known supernova remnant (SNR) in the Large Magellanic Cloud. To study the physical conditions of this SNR, we have obtained XMM-Newton X-ray observations, optical images and high-dispersion spectra, and radio continuum maps. Optical images of SNR 0450À70.9 show a large, irregular elliptical shell with bright filaments along the eastern and western rims and within the shell interior. The interior filaments have higher [S ii]/H ratios and form an apparent inner shell morphology. The X-ray emission region is smaller than the full extent of the optical shell, with the brightest X-ray emission found within the small interior shell and on the western rim of the large shell. The expansion velocity of the small shell is $220 km s À1 , while that of the large shell is $120 km s À1 . The radio image shows central brightening and a fairly flat radio spectral index over the SNR. However, no point X-ray or radio source corresponding to a pulsar is detected, and the X-ray emission is predominantly thermal. Therefore, these phenomena can be most reasonably explained in terms of the advanced age of the large SNR. Using hydrodynamic models combined with a nonequilibrium ionization model for thermal X-ray emission, we derived a lower limit on the SNR age of~45,000 yr, well into the later stages of SNR evolution. Despite this, the temperature and density derived from spectral fits to the X-ray emission indicate that the remnant is still overpressured and thus that the development is largely driven by hot gas in the SNR interior. Subject headingg s: ISM: individual (SNR 0450À70.9) -Magellanic Clouds -supernova remnants -X-rays: ISM

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“…In the past 30 years, numerous radio observations of many discrete sources in the MCs have been undertaken. In 1972, McGee et al (1972a made detailed observations of the LMC at 5.00 GHz with the Parkes radio telescope (See Table 1 for a summary of the radio-source surveys of the LMC) and established the first catalogue of discrete radio sources in the LMC, known as the MC catalogue. Later, McGee et al (1976) presented a list of sources towards the Small Magellanic Cloud (SMC) at 5.00 GHz (See Table 2 for a summary of the radio-source surveys of the SMC).…”

Section: High-frequency Radio Continuum Surveys Of Discrete Sources Imentioning

confidence: 99%

A radio continuum study of the Magellanic Clouds

Filipović

Haynes

White

et al. 1998

Astron. Astrophys. Suppl. Ser.

113

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Abstract. We present a study of discrete radio sources in the Magellanic Clouds (MCs) using the latest large-scale radio surveys made with the Parkes radio telescope between 1.4 and 8.55 GHz. These surveys achieved higher sensitivity then previous surveys done with the Parkes telescope and so the number of discrete radio sources detected towards the MCs has increased by factor of five. Also, we have obtained improved positions, flux densities and radio spectral indices for all of these sources.A total of 483 sources towards the Large Magellanic Cloud (LMC) and 224 towards the Small Magellanic Cloud (SMC) have been detected at at least one radio frequency. Most of the MC's sources have been classified in one of three groups: SNRs, H ii regions or background sources according to classification criteria established here. In total, 209 discrete radio sources in the LMC and the 37 sources in the SMC are classified here to be either H ii regions or SNRs. We investigate their luminosity functions as well as the statistics of background sources behind the MCs. Also, we examine the distribution of SNRs and H ii regions in the MCs.

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The Radio Continuum of the Large Magellanic Cloud. I. The Sources at 6 cm Wavelength

Abstract: The Large Magellanic Cloud has been surveyed in the radio continuum at a wavelength of 6 cm with the 4' arc beam of the Parkes radio telescope. A catalogue of 95 sources and diagrams of their brightness contours are presented here.

Cited by 42 publications

References 5 publications

A catalogue of compact radio sources in and behind the Large Magellanic Cloud

A catalogue of compact radio sources in and behind the Large Magellanic Cloud

Supernova Remnants in the Magellanic Clouds. IV. X‐Ray Emission from the Largest Supernova Remnant in the Large Magellanic Cloud

A radio continuum study of the Magellanic Clouds

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