A new look at the large-scale H I structure of the Large Magellanic Cloud

By L. Staveley-Smith, Sungeun Kim, M. Calabretta, R. Haynes, M. Kesteven. 2002

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We present a Parkes multibeam H i survey of the Large Magellanic Cloud (LMC). This survey, which is sensitive to spatial structure in the range 200 pc ∼ 10 kpc, complements the Australia Telescope Compact survey, which is sensitive to structure in the range 15 pc ∼ 500 pc. With an rms column density sensitivity of 8 ×10 16 cm −2 for narrow lines and 4×10 17 cm −2 for typical linewidths of 40 km s −1 , emission is found to be extensive well beyond the main body of the LMC. Arm-like features extend from the LMC to join the Magellanic Bridge and the Leading Arm, a forward counterpart to the Magellanic Stream. These features, whilst not as dramatic as those in the SMC, appear to have a common origin in the Galactic tidal field, in agreement with recent 2MASS and DENIS results for the stellar population. The diffuse gas which surrounds the LMC, particularly at pa’s 90 ◦ to 330 ◦ , appears to be loosely associated with tidal features, but loosening by the ram pressure of tenuous Galactic halo gas against the outer parts of the LMC cannot be discounted. High-velocity clouds, which lie between the Galaxy and the LMC in velocity and which appear in the UV spectra of some LMC stars, are found to be associated with the LMC if their heliocentric velocity exceeds about +100 km s −1 . They are possibly the product of energetic outflows from the LMC disk. The H i mass of the LMC is found to be (4.8 ± 0.2) × 10 8 M⊙ (for an assumed distance of 50 kpc), substantially more than previous recent measurements.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/3aab1fde9673cf8f84f956d0edbc7cbe2380db54

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Citations in the corpus

• 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;…”
• Planck 2015 results - XXVIII. The Planck Catalogue of Galactic cold clumps (2015, unknown): “◦ 09 centred on the Galactic coordinates (279.03, − 33.60), as defined by Staveley-Smith et al. (2003), are flagged ( XFLAG_LMC ) as part of the LMC, and 3 others falling inside a radius of 2.”
• The Parkes HI survey of the Magellanic System (2004, methodology): “We derive a total H mass of M(H ) = (4.6± 0.1)× 108 M for the LMC, if we use the same borders between the emission from the LMC and the neighboring H gas as Staveley-Smith et al. (2003).”
• The role of dwarf galaxy interactions in shaping the Magellanic System and implications for Magellanic Irregulars (2012, background): “The H I kinematics yield V rot = 80 km s−1 (Staveley-Smith et al. 2003a), data from red supergiants give V rot = 107 km s−1 (Olsen & Massey 2007) and carbon stars yield V rot = 61 km s−1 (van der Marel et al. 2002).”
• SPITZER SAGE SURVEY OF THE LARGE MAGELLANIC CLOUD. III. STAR FORMATION AND ∼1000 NEW CANDIDATE YOUNG STELLAR OBJECTS (2008, background): “Figure 8 shows the YSOs overlayed on a two-color image of H i gas (Staveley-Smith et al. 2003) in green and CO gas (Fukui et al. 1999) in red.”
• The Origin of the Magellanic Stream and Its Leading Arm (2007, background): “…a region of dense H I and intense star-formation in the southeast of the LMC. Analysis of the high spatial resolution H I Parkes data of the LMC (Staveley-Smith et al. 2003) indicates that supergiant shells in the SEHO are probably responsible for blowing out much of the gas from the LMC,…”
• THE STAR FORMATION HISTORY OF THE LARGE MAGELLANIC CLOUD (2009, background): “The complicated interaction history, both with the SMC and our Galaxy, provide many opportunities for complicated dynamical effects and distorted morphological features (cf. Staveley-Smith et al. 2003).”