These are some suggested topics for discussion during our workshop:
Markers:
- What is best to use as markers for the power spectrum - Halpha galaxies?
- Is there a way to use productively the higher number densities of galaxies we are likely to find, at least from space?
- How homogeneous does the selection of markers need to be?
- Are there issues with Halpha line identification - e.g. confusion with
NII, OIII?
- What spectral resolution is needed for line identification and redshift
measurement? d[ln(1+z)]=0.002 is 13A for Halpha.
Observations:
- What signal to noise measurement of the markers are needed? Issues of
Malmquist bias.
- What is the true resolution of grisms needed, given multipixel objects?
- How practical are these grisms given, e.g., the SNAP focal plane?
- Should the survey field be continuous or are long strips with gaps
between them ok?
- How best to take advantage of SNAP's 9 filters and photo-z accuracy?
Analysis:
- How serious are redshift space distortions and what to do about them?
- How does a d[ln(1+z)] translate into a resolution R and v.v.,
realistically?
- What are the subtleties in the method of oscillation fitting?
- Calibration issues?
Theory:
- Redshift shells, redshift ranges, 2D vs. 3D
- Where will baryon oscillation surveys/detections be in 5 years?
(OmegaCam, FMOS, AAOmega, VIMOS, (V)ISTA, HET, etc.)
- How best to take advantage of ground/space complementarity?