J/MNRAS/339/105 Western Magellanic Bridge HI observations (Muller+, 2003)
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 2003MNRAS.339..105M
ADC_Keywords: Magellanic Clouds ; H I data ; Radial velocities
Keywords: ISM: bubbles - ISM: structure - Magellanic Clouds
Abstract:
The 21-cm line emission from a 7x6deg2 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 ∼14° 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 7x6deg2
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=-72°20',
and extended 8° in declination and in RA, large enough to fully
encompass the area observed with the ATCA.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 64 163 Table of Magellanic Bridge shell parameters
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See also:
J/other/PASAu/6.471 : Magellanic Clouds bridge region HI profiles (McGee+ 1986)
J/ApJS/101/41 : SMC and Bridge extended catalog (Bica+ 1995)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- [MSZ2003] Sequential shell number
5- 6 I2 h RAh Right ascension (J2000)
8- 9 I2 min RAm Right ascension (J2000)
11- 14 F4.1 s RAs Right ascension (J2000)
16 A1 --- DE- Declination sign (J2000)
17- 18 I2 deg DEd Declination (J2000)
20- 21 I2 arcmin DEm Declination (J2000)
23- 26 F4.1 arcsec DEs Declination (J2000)
29- 33 F5.1 km/s HV Heliocentric velocity
36- 39 F4.1 km/s ExpV Expansion velocity
42- 45 F4.1 arcsec Rad Shell radius in arcmin
48- 52 F5.1 pc Radpc Shell radius in pc
55- 58 F4.1 Myr Age Dynamical age
61- 64 F4.1 [10-7W] logE Energy radiated
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History:
From electronic version of the journal
(End) James Marcout, Patricia Bauer [CDS] 07-Mar-2003