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Science
Programmes with WFCAM
1.
Introduction
2.
Widefield Infrared Galaxy Surveys
2.1
Local Galaxies
2.2 Galaxies at High Redshift
2.3 Clusters
3.
The UKIRT Wide Field and the use of near-IR selected samples of quasars
for cosmology
3.1
Introduction
3.2
Near Infrared KX selection of Quasars and Number Counts
3.3 Damped Lyman Alpha Galaxies and
the History of Star Formation
3.4 Dusty Lenses and the Value of
the Cosmological Constant
3.5 Red Quasars
4.
The UKIRT Wide Field In Galactic Astronomy
4.1
Introduction
4.2
Brown Dwarfs and Very Low Mass Stars
4.3 The Cool White Dwarfs
4.4 Stellar Populations and Galactic
Structure
4.5 Star Formation and the Initial
Luminosity Function
4.6 Dust Properties in Star-Forming
Regions
4.7 Source Confusion
4.8 The J-H, H-K colour plane
Possibilities
for Large Public Surveys with WFCAM
This
section is based on a paper submitted to the Sept 1998 meeting of the
Ground Based Facilities Committee by the IfA of the University of Edinburgh.
1.
Introduction
2.
Survey Forms - Private, Consortia and Public
3.
Key Science Drivers for Survey Design
3.1
Generic Atlas Drivers
3.2
Galaxies at z<0.1
3.3 Galaxies at z =1-2
3.4 Quasars
3.5 Star Formation Regions
3.6 Galactic Structure
3.7 Preliminary Survey Design
3.8 High Latitude Sky Atlas
3.9 Galactic Plane Atlas
3.10 Mid Latitude Survey
3.11 Deep Survey
3.12 Very Deep Survey
3.13 Survey Schedule
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