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J/MNRAS/339/105 Western Magellanic Bridge HI observations (Muller+, 2003)
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Beginning of ReadMe :J/MNRAS/339/105 Western Magellanic Bridge HI observations (Muller+, 2003)
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High-resolution HI observations of the Western Magellanic Bridge.
Muller E., Staveley-Smith L., Zealey W., Stanimirovic S.
<Mon. Not. R. Astron. Soc. 339, 105 (2003)>
=2003MNRAS.339..105M
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ADC_Keywords: Magellanic Clouds ; H I data ; Radial velocities
Keywords: ISM: bubbles - ISM: structure - Magellanic Clouds
Abstract:
The 21-cm line emission from a 7x6deg^2^ region east of and adjoining
the Small Magellanic Cloud (SMC) has been observed with the Australia
Telescope Compact Array and the Parkes telescopes. This region
represents the westernmost part of the Magellanic Bridge, a gas-rich
tail extending 14deg to the Large Magellanic Cloud. A rich and complex
neutral hydrogen (HI) structure containing shells, bubbles and
filaments is revealed. On the larger scale, the HI of the Bridge is
organized into two velocity components. This bimodality, which appears
to originate in the SMC, converges to a single velocity component
within the observed region. A census of shell-like structures suggests
a shell population with characteristics similar to that of the SMC.
Description:
Here we present high spatial and velocity resolution observations of
the Magellanic Bridge, conducted with both the Australia Telescope
Compact Array (ATCA) and with the Parkes telescope.
ATCA observation of the 21-cm H I line were made over a 7x6deg^2^
field using the 375-m configuration of the ATCA. These observations
were made over three sessions: 1997 April 13, 15-16, 18; 1997 October
9-15; and 2000 January 29-February 2. The ATCA observations were made
using a 4-MHz bandwidth, with 1024 channels at a central frequency of
1.420GHz.
Parkes observations were made using the Multibeam receiver on the 64-m
Parkes telescope, during 1999 November 2-8. Only the seven inner
receivers of the Multibeam array were used, with each beam having a
FWHM width of 14.1arcmin. 48 overlapping scans were made in
declination, using the on-the-fly mapping mode at 1deg/min in
declination. The scans were centred on RA=02h00m, DE=-72deg20',
and extended 8deg in declination and in RA, large enough to fully
encompass the area observed with the ATCA.