hi self absorption n.
Download
Skip this Video
Loading SlideShow in 5 Seconds..
HI Self - Absorption PowerPoint Presentation
Download Presentation
HI Self - Absorption

Loading in 2 Seconds...

play fullscreen
1 / 17

HI Self - Absorption - PowerPoint PPT Presentation


  • 52 Views
  • Uploaded on

HI Self - Absorption. Peculiar Puzzle and Potential Probe Predating the Arecibo Telescope Paul F. Goldsmith. The 21-cm Line of Atomic Hydrogen. Discovered in 1951 by Ewen and Purcell (2002 Gordon Lecture at Arecibo)

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about 'HI Self - Absorption' - gay-keller


An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
hi self absorption

HI Self - Absorption

Peculiar Puzzle and Potential Probe Predating

the Arecibo Telescope

Paul F. Goldsmith

the 21 cm line of atomic hydrogen
The 21-cm Line of Atomic Hydrogen
  • Discovered in 1951 by Ewen and Purcell (2002 Gordon Lecture at Arecibo)
  • Seen in EMISSION, which was not surprising since theories indicated that atomic gas in Milky Way would be warm (T ~ 100 K)
hinsa spectra in arecibo survey of taurus li goldsmith 2003
HINSA Spectra in Arecibo Survey of Taurus (Li & Goldsmith 2003)

Width of the HINSA features is so narrow that they must come from COLD (< 20K) gas!

Line minimum is so deep that in some cases the gas must again be below 20 K!

significance of atomic hydrogen within well shielded molecular clouds
Significance of Atomic Hydrogen Within Well-Shielded Molecular Clouds
  • HI destroyedby conversion to H2 on grain surfaces
  • HI formed by cosmic ray destruction of H2
  • STEADY-STATE ABUNDANCE of HI is ~ 1 cm-3 corresponding to 10-4 fractional abundance w.r.t. total proton density (due to preponderance of H2 )
how to proceed from here
How to Proceed From Here?
  • We have defined a large-scale survey of the Taurus region for HINSA to be carried out using ALFA – the L-band 7 element focal plane array
  • Map several hundred square degrees with good sensitivity
  • Compare with 12CO and 13CO maps from FCRAO (300 hours of telescope time already awarded)
  • ~ 100 hours of AO observing time required to get high sensitivity maps of COLD and WARM HI
the alfa tau project
The ALFA – TAUProject
  • When we compare the kinematics of cold and warm atomic gas -- are they the same?
  • What is the relationship of the atomic and the molecular gas?
  • What is the characteristic timescale for dark cloud cores as traced by residual HI?
  • Can we develop a scenario for the evolution from atomic to molecular material and then from molecular clouds to cores to young stars?