A radio continuum study of the Magellanic Clouds

Filipović, Miroslav; Jones, P. A.; White, Graeme L.; Haynes, R. F.; Klein, U.; Wielebinski, R.

doi:10.1051/aas:1997317

Cited by 39 publications

(52 citation statements)

References 11 publications

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“…The Parkes survey at 4.8 and 8.5 GHz (Filipovic et al 1997) allow to put an upper limit to the free-free contribution. The radio free-free flux from H II regions scales with ν −0.1 .…”

Section: Resultsmentioning

confidence: 99%

Millimeter dust emission from an SMC cold molecular cloud

Rubio¹,

Boulanger

Rantakyrö

et al. 2004

A&A

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Abstract. We presented SIMBA 1.2 mm continuum observations of SMCB1-1 an SMC molecular cloud known to be distant from massive ionizing stars. The gas mass derived from the SIMBA flux is a factor of ∼10 higher than the virial mass previously reported from CO observations. We propose an interpretation where the virial mass underestimates the total mass because the CO emission comes from dense clumps which do not trace the full cloud area and velocity distribution. This work sets an important question for the understanding of star formation in low metallicity gas. Do CO observations grossly underestimate the amount of dense self gravitating clouds where stars can form?

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“…The Parkes survey at 4.8 and 8.5 GHz (Filipovic et al 1997) allow to put an upper limit to the free-free contribution. The radio free-free flux from H II regions scales with ν −0.1 .…”

Section: Resultsmentioning

confidence: 99%

Millimeter dust emission from an SMC cold molecular cloud

Rubio¹,

Boulanger

Rantakyrö

et al. 2004

A&A

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“…described the creation of a new high resolution image at 20 cm for the SMC. This was done by combining three archived images from ATCA projects (C159, C1288 and C1197) plus the Parkes image from Filipovic et al (1997). The images included array configurations of 375-m, 6A, H214 and H75.…”

Section: Archival Data and New Radio-continuum Observationsmentioning

confidence: 99%

Radio planetary nebulae in the Small Magellanic Cloud

Leverenz¹,

Filipović²,

Bojičić³

et al. 2016

Astrophys Space Sci

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We present ten new radio continuum (RC) detections at catalogued planetary nebula (PN) positions in the Small Magellanic Cloud (SMC): SMP S6, LIN 41, LIN 142, SMP S13, SMP S14, SMP S16, J 18, SMP S18, SMP S19 and SMP S22. Additionally, six SMC radio PNe previously detected, LIN 45, SMP S11, SMP S17, LIN 321, LIN 339 and SMP S24 are also investigated (re-observed) here making up a population of 16 radio detections of catalogued PNe in the SMC. These 16 radio detections represent ∼15 % of the total catalogued PN population in the SMC. We show that six of these objects have characteristics that suggest that they are PN mimics: LIN 41, LIN 45, SMP S11, LIN 142, LIN 321 and LIN 339. We also present our

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“…We have extracted all archival radio-continuum observations of IKT 16 using the Australia Telescope Compact Array (ATCA) comprising observations at 4 radio wavelengths: 20, 13, 6 and 3 cm for ATCA (Dickel et al 2001;Filipović et al 2002;Payne et al 2004;Filipović et al 1997). In addition we make use of the Molonglo Observatory Synthesis Telescope (MOST) SMC survey at 36 cm (843 MHz) (Turtle et al 1998).…”

Section: Radio Observationsmentioning

confidence: 99%

IKT 16: a composite supernova remnant in the Small Magellanic Cloud

Owen

Filipović

Ballet

et al. 2011

A&A

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Aims. IKT 16 is an X-ray and radio-faint supernova remnant (SNR) in the Small Magellanic Cloud (SMC). A previous X-ray study of this SNR found a hard X-ray source near its centre. Using all available archival and proprietary XMM-Newton data, alongside new multi-frequency radio-continuum surveys and optical observations at Hα and forbidden [SII] and [OIII] lines, we aim to constrain the properties of the SNR and discover the nature of the hard source within. Methods. We combine XMM-Newton datasets to produce the highest quality X-ray image of IKT 16 to date. We use this, in combination with radio and optical images, to conduct a multi-wavelength morphological analysis of the remnant. We extract separate spectra from the SNR and the bright source near its centre, and conduct spectral fitting of both regions. Results. We find IKT 16 to have a radius of 37 ± 3 pc, with the bright source located 8 ± 2 pc from the centre. This is the largest known SNR in the SMC. The large size of the remnant suggests it is likely in the Sedov-adiabatic phase of evolution. Using a Sedov model to fit the SNR spectrum, we find an electron temperature kT of 1.03 ± 0.12 keV and an age of ≈14700 yr. The absorption found requires the remnant to be located deep within the SMC. The bright source is fit with a power law with index Γ = 1.58 ± 0.07, and is associated with diffuse radio emission extending towards the centre of the SNR. We argue that this source is likely to be the neutron star remnant of the supernova explosion, and infer its transverse kick velocity to be 580 ± 100 km s −1 . The X-ray and radio properties of this source strongly favour a pulsar wind nebula (PWN) origin.

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A radio continuum study of the Magellanic Clouds

Cited by 39 publications

References 11 publications

Millimeter dust emission from an SMC cold molecular cloud

Millimeter dust emission from an SMC cold molecular cloud

Radio planetary nebulae in the Small Magellanic Cloud

IKT 16: a composite supernova remnant in the Small Magellanic Cloud

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