A 4.8 and 8.6 GHz Survey of the Large Magellanic Cloud. I. The Images

Dickel, John R.; McIntyre, V.; Gruendl, R. A.; Milne, D. K.

doi:10.1086/426916

Cited by 61 publications

(58 citation statements)

References 17 publications

(21 reference statements)

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“…The WR region appears to be similar to the 30 Doradus (Tarantula Nebula), which also dominates the Hα (Gaustad et al 2001), far-IR (Meixner et al 2006), and radio (Dickel et al 2005) emission of the LMC, as shown in Fig. 7, but it contributes very little to total stellar mass.…”

Section: Dust and Star Formation In The Wr Region: High Densitymentioning

confidence: 89%

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Spatially-resolved dust properties of the GRB 980425 host galaxy

Michałowski

Hunt

Palazzi

et al. 2014

A&A

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Gamma-ray bursts (GRBs) have been proposed as a tool for studying star formation in the Universe, so it is crucial to investigate whether their host galaxies and immediate environments are in any way special compared with other star-forming galaxies. Here we present spatially resolved maps of dust emission of the host galaxy of the closest known GRB 980425 at z = 0.0085 using our new high-resolution observations from Herschel, Atacama Pathfinder Experiment (APEX), Atacama Large Millimeter Array (ALMA) and Australia Telescope Compact Array (ATCA). We modelled the spectral energy distributions of the host and of the star-forming region displaying the Wolf-Rayet signatures in the spectrum (WR region), located 800 pc from the GRB position. The host is characterised by low dust content and a high fraction of UV-visible star formation, similar to other dwarf galaxies. These galaxies are abundant in the local universe, so it is not surprising to find a GRB in one of them, assuming the correspondence between the GRB rate and star formation. The WR region contributes substantially to the host emission at the far-infrared, millimetre, and radio wavelengths and we propose that this is a consequence of its high gas density. If dense environments are also found close to the positions of other GRBs, then the ISM density should also be considered, along with metallicity, an important factor influencing whether a given stellar population can produce a GRB.

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Section: Dust and Star Formation In The Wr Region: High Densitymentioning

confidence: 89%

“…7. Mosaic of the images of the Large Magellanic Cloud (Gaustad et al 2001;Meixner et al 2006;Dickel et al 2005). North is up and east is to the left.…”

Section: Dust and Star Formation In The Wr Region: High Densitymentioning

confidence: 99%

Spatially-resolved dust properties of the GRB 980425 host galaxy

Michałowski

Hunt

Palazzi

et al. 2014

A&A

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“…To this end, extensive mappings of the MCs have recently been conducted at a number of wavelengths. Surveys have been made in H I emission at 21-cm (HIPASS: Barnes et al 2001;Brüns et al 2005;Staveley-Smith et al 1997Stanimirović et al 1999;and Muller et al 2003), in molecular spectral CO lines (NANTEN: Fukui et al 1999;Mizuno et al 2001), as well as in the radio continuum (Haynes et al 1991;Dickel et al 2005), in the thermal infrared (IRAS: Beichman et al 1988;MSX: Mill et al 1994;SAGE: Meixner et al 2006; S 3 MC: Bolatto et al 2007), in the nearinfrared (DENIS: Epchtein et al 1997;2MASS: Skrutskie et al 2006), in broadband optical colors (MCPS: Zaritsky et al 2002Zaritsky et al , 2004 as well as in optical emission lines (MCELS: Smith et al 1998), and at ultraviolet (Smith, Cornett & Hill 1987) and X-ray wavelengths (ROSAT: Snowden & Petre 1994; Chandra and ACIS: Townsley et al 2006). While these surveys have deepened our understanding of the Clouds themselves -e.g., their star formation history, their stellar content, and their overall structure (van der Marel 2001) -the H I investigations are central to understanding the most obvious product of the MW-MC interaction -the Magellanic Stream.…”

Section: Introductionmentioning

confidence: 99%

The Origin of the Magellanic Stream and its Leading Arm

Nidever

Majewski

Burton

2008

Astrophysics and Space Science Proceedings

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We explore the Magellanic Stream (MS) using a Gaussian decomposition of the H I velocity profiles in the Leiden-Argentine-Bonn (LAB) all-sky H I survey. This decomposition exposes the MS to be composed of two filaments distinct both spatially (as first pointed out by Putman et al.) and in velocity. Using the velocity coherence of the filaments, one can be traced back to its origin in what we identify as the SouthEast H I Overdensity (SEHO) of the Large Magellanic Cloud (LMC), which includes 30 Doradus. Parts of the Leading Arm (LA) can also be traced back to the SEHO in velocity and position. Therefore, at least one-half of the trailing Stream and most of the LA originates in the LMC, contrary to previous assertions that both the MS and the LA originate in the Small Magellanic Cloud (SMC) and/or in the Magellanic Bridge. The two MS filaments show strong periodic, undulating spatial and velocity patterns that we speculate are an imprint of the LMC rotation curve. If true, then the drift rate of the Stream gas away from the Magellanic Clouds is ∼49 km s −1 and the age of the MS is ∼1.74 Gyr. The Staveley-Smith et al. high-resolution H I data of the LMC show gas outflows from supergiant shells in the SEHO that seem to be creating the LA and LMC filament of the MS. Blowout of LMC gas is an effect not previously accounted for but one that probably plays an important role in creating the MS and LA.

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“…Radio-continuum surveys were predominately based on observations from the Aus- as well as the 6 cm and 3 cm mosaics published by Dickel et al (2005); Wong et al (2012). In addition, a 36 cm Molonglo Synthesis Telescope (MOST) mosaic image (as described in Mills et al 1984) was used.…”

Section: Magellanic Clouds Surveysmentioning

confidence: 99%

Supernova Remnants in the Magellanic Clouds

Bozzetto

Filipović

Haberl

et al. 2015

Publications of The Korean Astronomical Society

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We present an ongoing study of the complete sample of supernova remnants (SNRs) and candidates in the Magellanic Clouds. 108 objects in both Clouds are considered to be either SNR or reliable candidates. This represents the most complete sample of all known SNRs in any galaxy. It therefore allows us to study SNR population properties such as the age-diameter (Age-D) relation. Here, we show that this Age-D relation is strongly dependant on the local environment in which SNRs are residing.

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A 4.8 and 8.6 GHz Survey of the Large Magellanic Cloud. I. The Images

Cited by 61 publications

References 17 publications

Spatially-resolved dust properties of the GRB 980425 host galaxy

Spatially-resolved dust properties of the GRB 980425 host galaxy

The Origin of the Magellanic Stream and its Leading Arm

Supernova Remnants in the Magellanic Clouds

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