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SUMMARY:Imaging of dust and molecular gas in high-redshift galaxies - Pade
 lis Papadopoulos (Cardiff)
DTSTART:20170113T113000Z
DTEND:20170113T123000Z
UID:TALK67663@talks.cam.ac.uk
CONTACT:Martin Haehnelt
DESCRIPTION: In  the age of ALMA images of dust continuum and carbon monox
 ide (CO) line emission are our new and powerful  tools  for deducing struc
 tural characteristics of early galaxies such as disc scalelengths\, H2 gas
  velocity fields and enclosed H2 and dynamical masses. Such images are als
 o used to deduce the Toomre Q parameter of gas-rich disks at high redshift
 s\, an important parameter for  deciding how star-formation is driven in t
 hese extreme objects.\nThe rising Cosmic Microwave Background (CMB) places
  a fundamental constraint on the structural information  that can be deduc
 ed from such images\, progressively erasing all spatial and spectral contr
 asts between their brightness distributions and the CMB. This limitation i
 s unique to\nmillimetre/submillimetre wavelengths and unlike its known eff
 ect on the global dust continuum and molecular line emission of galaxies\,
  it cannot be addressed simply. We have found two possible ways around it 
 that will be discussed in some detail.\n
LOCATION:Kavli LMR\, IoA
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