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An HIÒšStudy of the NGCÒš6744 System
Stuart D. Ryder 1 - Wilfred Walsh 2 - David Malin 3
1 Joint Astronomy Centre, 660 N. A'Ohoku Place, Hilo, HI 96720, U.S.A.
sryder@jach.hawaii.edu
2 Radioastronomisches Institut der UniversitÓ?t Bonn, Auf dem HÓÌgel 71, Bonn D-53121, Germany.
wwalsh@astro.uni-bonn.de
3 Anglo-Australian Observatory, P.O. Box 296, Epping, NSWÒš1710, Australia.
dfm@aaoepp.aao.gov.au
Abstract:
We present the preliminary results of our 5-configuration, 20-pointing mosaic with the Australia Telescope Compact Array of the neutral hydrogen in the nearby spiral galaxy NGCÒš6744. The bulk of the HI resides in a ``ring'' underlying the outer optical disk, with 2ÒšHI spiral arms extending further out to almost 1.5Òšoptical radii. The velocity field is fairly regular, apart from evidence for streaming motions along the HI arms, and the influence of the companion IB(s)m galaxy NGCÒš6744A. We associate a cloud of HI at a heliocentric velocity of 846ÒškmÒš
with another companion object, ESOÒš104-g44. Our attempts to construct a mass model for NGCÒš6744 suffer from poor resolution in the inner disk, and the uncertainty in the total HI flux of NGCÒš6744. We anticipate that HIPASS observations will be crucial in resolving the latter issue.
with another companion object, ESOÒš104-g44. Our attempts to construct a mass model for NGCÒš6744 suffer from poor resolution in the inner disk, and the uncertainty in the total HI flux of NGCÒš6744. We anticipate that HIPASS observations will be crucial in resolving the latter issue.
Keywords: galaxies: individual (NGC 6744) -- galaxies: interactions -- galaxies: kinematics and dynamics -- galaxies: spiral
- Introduction
- ATCA Observations
- Results
- Rotation Curve and Dark Matter Model
- Future Work
- Acknowledgements
- References
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Amelia Ortiz-Gil
1999-02-16
ASKAP
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