Summary of Oxford meeting on the 27th Jan

This is just a summary of what was discussed at the Oxford meeting on 27th Jan. Sorry about the delay but Chris Simpson and myself have been trying to figure out how the magnitudes relate (in real terms) to the UKIDSS surveys.

To summarise:

1. Initially 20sq.deg to (all Vega) K~22, H~22.8, J~23.5, Y~24.2, Z~25 (or 21.5,22.3,23,23.8,24.5 - see below) , all 5sigma (2" aperture) with the aim of eventually covering 50sq.deg. obviously we get the 50 sq.deg quicker at the shallower depths (quoted in original email).

Although at the meeting it was decided to go to K~22 this isn't yet a firm limit as the quoted depth of the UDS of K~23 isn't measured in the same aperture as the magnitudes I quote. Chris and myself think we've sorted this out and it has an effective depth of K~22.3 in the 2" apertures I'm using which corresponds to K~21.5 in total galaxy magnitudes (i.e., my magnitudes lose ~half the light from an 8-kpc effective radius galaxy).

Depending on how you define L* at high redshift, and which population synthesis code you ise to passively evolve an L* galaxy this corresponds to z~<4 and lower. Therefore, I'd like to leave the details about the required depth after we know what is happening with any Ultra-Deep (1 tile) proposal.

2. Fields to be covered

XMM-LSS (6 sq.deg)

CDF-S (6 sq.deg)

Elais-S1 (9 sq.deg)

New Equatorial Field (VIDEO-2000!) 14hrs (~21 sq.deg)

Still to be confirmed

South Pole accessible field (RA DEc yet to be decided - depends on where other survey fields will concentrate)

SSA22 again dependent on SP field

3. Science

Main driver:

Galaxy evolution as a function of environment

Other drivers:

Hiz galaxy clusters - get a lot of cluster information from VIDEO data alone, particularly at 1.3 < z< 1.7. Higher-z (proto-)cluster candidates can be followed up with VLTs

High-redshift QSO luminosity function

Transiting/variable phenomena in the Galaxy

Synergies with Type-Ia supernovae searches and many other things that I haven't listed but other people can think on.

4. Links with future instrumentation

ESO

NON-ESO

ESA

Any comments are welcome.

cheers Matt

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