A multifrequency radio continuum study of the Magellanic Clouds – I. Overall structure and star formation rates

For, Bi-Qing; Staveley‐Smith, L.; Hurley‐Walker, N.; Franzen, T. M. O.; Kapińska, A. D.; Filipović, Miroslav; Collier, J. D.; Wu, Chen; Grieve, Kevin; Callingham, J. R.; Bell, M. E.; Bernardi, G.; Bowman, Judd D.; Briggs, F.; Cappallo, R. J.; Deshpande, A. A.; Dwarakanath, K. S.; Gaensler, B. M.; Greenhill, L. J.; Hancock, P. J.; Hazelton, B. J.; Hindson, L.; Johnston‐Hollitt, M.; Kaplan, D. L.; Lenc, E.; Lonsdale, Colin J.; McKinley, B.; McWhirter, S. R.; Mitchell, D. A.; Morales, M. F.; Morgan, E.; Morgan, John S.; Oberoi, D.; Offringa, A. R.; Ord, S. M.; Prabu, T.; Procopio, P.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.; Tingay, S. J.; Wayth, R. B.; Webster, R. L.; Williams, A.; Williams, Christopher; Zheng, Qian

doi:10.1093/mnras/sty1960

Cited by 28 publications

(44 citation statements)

References 61 publications

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“…These data have been taken with the ATCA, Parkes and the Molonglo Synthesis Telescope (MOST). Additionally, we make use of Murchison Widefield Array (MWA) data from For et al (2018) andJoseph et al (2019, in prep. ) obtained from the Australia Square Kilometre Ar-ray Pathfinder (ASKAP) Early Science Project observations of the SMC.…”

Section: Radio Continuum Observationsmentioning

confidence: 99%

Discovery of a pulsar-powered bow shock nebula in the Small Magellanic Cloud supernova remnant DEM S5

Alsaberi

Maitra

Filipović

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We report the discovery of a new Small Magellanic Cloud Pulsar Wind Nebula (PWN) at the edge of the Supernova Remnant (SNR) DEM S5. The pulsar powered object has a cometary morphology similar to the Galactic PWN analogs PSR B1951+32 and 'the mouse'. It is travelling supersonically through the interstellar medium. We estimate the Pulsar kick velocity to be in the range of 700-2000 km s −1 for an age between 28-10 kyr. The radio spectral index for this SNR-PWN-pulsar system is flat (-0.29 ± 0.01) consistent with other similar objects. We infer that the putative pulsar has a radio spectral index of -1.8, which is typical for Galactic pulsars. We searched for dispersion measures (DMs) up to 1000 cm −3 pc but found no convincing candidates with a S/N greater than 8. We produce a polarisation map for this PWN at 5500 MHz and find a mean fractional polarisation of P ∼23 percent. The X-ray power-law spectrum (Γ ∼2) is indicative of non-thermal synchrotron emission as is expected from PWN-pulsar system. Finally, we detect DEM S5 in Infrared (IR) bands. Our IR photometric measurements strongly indicate the presence of shocked gas which is expected for SNRs. However, it is unusual to detect such IR emission in a SNR with a supersonic bow-shock PWN. We also find a low-velocity H i cloud of ∼107 km s −1 which is possibly interacting with DEM S5. SNR DEM S5 is the first confirmed detection of a pulsar-powered bow shock nebula found outside the Galaxy.

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Section: Radio Continuum Observationsmentioning

confidence: 99%

Discovery of a pulsar-powered bow shock nebula in the Small Magellanic Cloud supernova remnant DEM S5

Alsaberi

Maitra

Filipović

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Combining Phase I and Phase II data will potentially reveal low surface brightness emission below previous confusion limits, both within and outside of the Galactic Plane, as well as having the higher angular resolution of Phase II with the large-angular scale sensitivity of Phase I (see Figure 6 for an example of the combined imaging potential). The complete population of SNRs in the nearby Magellanic Clouds will also be detectible (Bozzetto et al 2017;For et al 2018).…”

Section: Supernova Remnants and Pulsar Wind Nebulaementioning

confidence: 99%

“…Rather, the synchrotron spectrum at low frequencies (below 1 GHz) is rather flat, with a spectral index (α where S ν ∝ ν α ) of approximately −0.6, coupled with a break and an exponential decline at GHz frequencies. Previous studies show that the MWA Phase I synthesised beam is too large to allow for resolved radio spectral index maps of specific star-forming regions even in the nearest galaxies, such as the Magellanic Clouds (For et al 2018) and NGC 253 (Kapińska et al 2017).…”

Section: Nearby Galaxies and Magellanic Cloudsmentioning

confidence: 99%

“…In the neighbouring Magellanic Clouds, the MWA Phase II capabilities will enable the quantification of the cosmic ray energy spectrum and the measurement of spatial variations that arise from shock re-acceleration, spectral aging, and absorption effects-the primary goal of The Deep Survey of the Magellanic System (MAGE-X, For et al 2018). The importance of hydrodynamical environmental processes such as ram pressure is understood in the cluster environment (e.g.…”

Section: Nearby Galaxies and Magellanic Cloudsmentioning

confidence: 99%

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Science with the Murchison Widefield Array: Phase I results and Phase II opportunities

Beardsley

Johnston‐Hollitt

Trott

et al. 2019

Publ. Astron. Soc. Aust.

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The Murchison Widefield Array (MWA) is an open access telescope dedicated to studying the low frequency (80-300 MHz) southern sky. Since beginning operations in mid 2013, the MWA has opened a new observational window in the southern hemisphere enabling many science areas. The driving science objectives of the original design were to observe 21 cm radiation from the Epoch of Reionisation (EoR), explore the radio time domain, perform Galactic and extragalactic surveys, and monitor solar, heliospheric, and ionospheric phenomena. All together 60+ programs recorded 20,000 hours producing 146 papers to date. In 2016 the telescope underwent a major upgrade resulting in alternating compact and extended configurations. Other upgrades, including digital back-ends and a rapid-response triggering system, have been developed since the original array was commissioned. In this paper we review the major results from the prior operation of the MWA, and then discuss the new science paths enabled by the improved capabilities. We group these science opportunities by the four original science themes, but also include ideas for directions outside these categories.

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“…The GaLactic and Extragalactic All-sky MWA (GLEAM; Wayth et al 2015) survey observed the whole sky south of declination (Dec) +30 • from 2013 to 2015 between 72 and 231 MHz. A major data release covering 24 402 deg 2 of extragalactic sky was published by Hurley-Walker et al (2017), while individual studies have published smaller regions such as the Magellanic Clouds (For et al 2018).…”

Section: Introductionmentioning

confidence: 99%

GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey II: Galactic plane 345° <l< 67°, 180° <l< 240°

Hurley‐Walker

Hancock

Franzen

et al. 2019

Publ. Astron. Soc. Aust.

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This work makes available a further 2,860 deg 2 of the GLEAM survey, covering half of the accessible Galactic Plane, across twenty frequency bands sampling 72-231 MHz, with resolution 4'-2'. Unlike previous GLEAM data releases, we used multi-scale c l e a n to better deconvolve large-scale Galactic structure. For the Galactic longitude ranges 345 • < l < 67 • , 180 • < l < 240 • , we provide a compact source catalogue of 22,037 components selected from a 60-MHz bandwidth image centred at 200-MHz, with RMS noise ≈ 10-20 mJy beam −1 and position accuracy better than 2". The catalogue has a completeness of 50 % at ≈ 120 mJy, and a reliability of 99.86 %. It covers Galactic latitudes 1 • ≤ |b| ≤ 10 • toward the Galactic Centre and |b| ≤ 10 • for other regions, and is available from Vizier; images covering |b| ≤ 10 • for all longitudes are made available on the GLEAM VO server and SkyView.

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A multifrequency radio continuum study of the Magellanic Clouds – I. Overall structure and star formation rates

Cited by 28 publications

References 61 publications

Discovery of a pulsar-powered bow shock nebula in the Small Magellanic Cloud supernova remnant DEM S5

Discovery of a pulsar-powered bow shock nebula in the Small Magellanic Cloud supernova remnant DEM S5

Science with the Murchison Widefield Array: Phase I results and Phase II opportunities

GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey II: Galactic plane 345° <l< 67°, 180° <l< 240°

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