TY - JOUR
T1 - A neutral hydrogen survey of the large magellanic cloud
T2 - Aperture synthesis and multibeam data combined
AU - Kim, Sungeun
AU - Staveley-Smith, Lister
AU - Dopita, Michael A.
AU - Sault, Robert J.
AU - Freeman, Kenneth C.
AU - Lee, Youngung
AU - Chu, You Hua
PY - 2003/10
Y1 - 2003/10
N2 - 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-22 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.
AB - 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-22 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.
KW - Galaxies: ISM
KW - ISM: atoms
KW - Magellanic Clouds
KW - Radio lines: galaxies
UR - http://www.scopus.com/inward/record.url?scp=0345448287&partnerID=8YFLogxK
U2 - 10.1086/376980
DO - 10.1086/376980
M3 - Review article
AN - SCOPUS:0345448287
SN - 0067-0049
VL - 148
SP - 473
EP - 486
JO - Astrophysical Journal, Supplement Series
JF - Astrophysical Journal, Supplement Series
IS - 2
ER -