HI observations of the Magellanic Bridge课件.pptVIP

T maps SCF maps 55 pixels 37 pixels 精品文档 HI observations of the Magellanic Bridge Erik Muller UOW/ATNF Supervisors: Bill Zealey (UOW) Lister Staveley-Smith (ATNF) 精品文档 Overview: HI observations of the Magellanic Bridge HI Data collection and reduction Magellanic Bridge HI expanding Shell census Evidence for star-formation within the Magellanic Bridge: results of a search for CO emission in the Magellanic Bridge A quick look at H? (maybe..) Statistical tools applied to Bridge HI dataset 精品文档 The Magellanic System: Detected in HI (spin-flip transition of Neutral Hydrogen) by Kerr, Hindman Robinson, (1954), Parkes Telescope (ATNF). Magellanic clouds are ~60kpc (SMC) to ~50kpc (LMC) Their nearness makes them an excellent laboratory in which to observe physical processes with high spatial resolution Magellanic system comprises five elements: Large Magellanic Cloud (LMC) (Kim 1998) Small Magellanic Cloud (SMC) (Staveley-Smith 1998, Stanimirovic 1999) The Magellanic Stream (Putman, Gibson, Stanimirovic etc. 1998) The Leading Arm (Putman 2000) The Magellanic Bridge (Mathewson Cleary 1984) Bridge spans the ~14kpc from western edge of LMC to eastern edge of SMC Formed through tidal interaction of SMC with LMC (Simulations predict 150-200 Myr old - eg. Gardiner Noguchi 1996) Populated by young O-B (7 Myr), as well as older, stars. (eg. Irwin et al, 1995) 精品文档 Peak Pixel map, Linear trans. func. Tmax=0.3 MJy/beam The Magellanic System in HI:Multibeam, Parkes. To the Magellanic Stream To the Leading Arm LMC SMC The Magellanic Bridge 精品文档 HI Data collection Reduction: 144 pointings with ATCA (375m configuration) ~16 minutes/pointing Scanning with Parkes multibeam (inner seven beams) Scanning rate: 1o/min ATCA Data reduced with MIRIAD conventional procedures for data flagging and calibration Parkes and ATCA data merged post-convolution using IMMERGE (Stanimirovic, PhD, 1999) Parkes data reduced on line with ‘LIVEDATA’ Bandpass calibrations, velocity corrections Res