A Neutral Hydrogen Survey of the Large Magellanic Cloud: Aperture Synthesis and Multibeam Data Combined

By Sungeun Kim, L. Staveley-Smith, M. Dopita, R. Sault, Kenneth C. Freeman, Youngung Lee, Y. Chu. 2003

233 citations recorded by the source corpus.

Recent H I surveys of the Large Magellanic Cloud (LMC) with the Australia Telescope Compact Array and the Parkes multibeam receiver have focused, respectively, on the small-scale (<20′) structure of the interstellar medium (ISM) and the large-scale (>1°) structure of the galaxy. Using a Fourier-plane technique, we have merged both data sets, providing an accurate set of images of the LMC sensitive to structure on scales of 15 pc upward. The spatial dynamic range (2.8 orders of magnitude), velocity resolution (1.649 km s-1), brightness temperature sensitivity (2.4 K), and column density sensitivity (7.2 × 1018 cm-2 per 1.649 km s-1 channel) allow for studies of phenomena ranging from the galaxy-wide interaction of the LMC with its close neighbors to the small-scale injection of energy from supernovae and stellar associations into the ISM of the LMC. This paper presents the merged data and size spectrum of H I clouds, which is similar to the typical size spectrum of the holes and shells in the H I distribution. The H I clouds in the LMC have been identified by defining a cloud to be an object composed of all pixels in right ascension, declination, and velocity that are simply connected and that lie above the threshold brightness temperature.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/152b8a53a7b7a779c4f3bec9547a0b916b4ea139

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Citations in the corpus

A WIDE-FIELD HIGH-RESOLUTION H i MOSAIC OF MESSIER 31. I. OPAQUE ATOMIC GAS AND STAR FORMATION RATE DENSITY (2009, background): “…Survey of Galactic H I has achieved 36 arcmin and 1.3 km s−1 resolution over 360 degrees and reaches 0.08 K RMS Kalberla et al. (2005) and the Large Magellanic Cloud survey of Kim et al. (2003) achieves 1 arcmin and 1.7 km s−1 resolution over 12×10 degrees and reaches 2.5 K RMS.”
Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy’s Evolution (SAGE). I. Overview and Initial Results (2006, unknown): “The ISM gas that fuels star formation (Fukui et al. 1999; Mizuno et al. 2001; Y. Fukui et al. 2006, in preparation; Staveley-Smith et al. 2003; Kim et al. 2003), the stellar components that trace the history of star formation (Zaritsky et al. 2004; Van Dyk et al. 1999; Nikolaev & Weinberg 2000;…”
HI4PI: a full-sky H i survey based on EBHIS and GASS (2016, background): “1 displays a part of the Leading Arm region (row 2; Brüns et al. 2005; Venzmer et al. 2012; For et al. 2013) of the Magellanic Clouds (row 3; Kim et al. 2003; Brüns et al. 2005) and the M31/M33 region (row 4; Braun et al. 2003; Thilker et al. 2004; Wolfe et al. 2016; Kerp et al. 2016a).”
THE FRACTAL DENSITY STRUCTURE IN SUPERSONIC ISOTHERMAL TURBULENCE: SOLENOIDAL VERSUS COMPRESSIVE ENERGY INJECTION (2007, unknown): “…Dp ∼ 1.2 . . . 1.6 (e.g., Beech 1987; Bazell & Desert 1988; Dickman et al. 1990; Falgarone et al. 1991; Vogelaar et al. 1991; Hetem & Lepine 1993; Vogelaar & Wakker 1994; Westpfahl et al. 1999; Kim et al. 2003; Lee 2004; Sánchez et al. 2007) with most of the studies finding Dp ∼ 1.3 . . .1.4.”
The Parkes HI survey of the Magellanic System (2004, methodology): “H studies at high angular resolution were performed by Kim et al. (1998, 2003) Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20040321 for the LMC and by Stanimirovic et al. (1999, 2004) for the SMC, using the Australia Telescope…”
THE CO-TO-H2 CONVERSION FACTOR FROM INFRARED DUST EMISSION ACROSS THE LOCAL GROUP (2011, methodology): “We use the first CO map of the LMC obtained by NANTEN (Fukui et al. 1999), the Australia Telescope Compact Array (ATCA) + Parkes H I map of Kim et al. (1998, 2003), and IR maps from the Spitzer SAGE legacy program (Meixner et al. 2006; Bernard et al. 2008).”
The Origin of the Magellanic Stream and Its Leading Arm (2007, background): “The high spatial resolution H I data from Kim et al. (2003) show this region to have many thin outflows from the SEHO (see their Fig.”
Star formation and feedback in smoothed particle hydrodynamic simulations – I. Isolated galaxies (2006, methodology): “Images of the Large Magellanic Cloud in HI show similar features (see Figure 4 of Jones et al. (1999) or Figure 3 of Kim et al. (2003) for a similar image of the Circinus Galaxy).”
Non-standard grain properties, dark gas reservoir, and extended submillimeter excess, probed by Herschel in the Large Magellanic Cloud (2011, methodology): “We use the [H i]21 cm map observed by Kim et al. (2003).”
Interstellar Turbulence I: Observations and Processes (2004, background): “Padoan et al. (2001c) measured the line-of-sight thickness of the LMC using the transition length where the slope of the spectral correlation function versus separation goes from steep on small scales to shallow on large scales.”