1. Astronomical Wide-field Imaging System for Europe MPE/USM Survey/GTO Projects Mark Neeser MPE / ESO Mark Neeser MPE / ESO Leiden Workshop Nov. 2005

2. MPE/USM GTO Projects KIDS: - large-scale angular power spectrum (dark energy) - very high redshift QSOs - evolution of galaxies and clusters GTO Projects: DEGAS (PI: Hopp) (19 nights/3 years for 3 o ) Science Goals: SFR, mass, morphology of field galaxies in three well-defined redshift bins between 0.3 < z < 1.3 SFR derived from narrow-band imaging of emission-lines (H , H , [OII]) from observations in two NB filters stellar masses from model fitting of the broad-band photometry in the optical & NIR morphology from HST imaging

3. Technical: 3 square degrees in 3 fields (COSMOS, GOODS-S, MUNICS-Deep) u’ g’ r’ i’ z' (if necessary) + H  + NS850 public HST imaging (except MUNICS-Deep) available NIR broad-band imaging (UKIDSS/VISTA) available spectroscopy depths (AB, 5 , 1.6” aperture): u'=25.7 g'=26.8 r'=26.8 i'=26.1 z'=24.9 NB imaging to (at least) SFR = 0.1 solar mass per year MPE/USM GTO Projects AW Challenges: - processing narrow-band filters: cosmetics and = f(r) - accurate photometric redshifts (aperture-matched magnitudes)

4. MPE/USM GTO Projects ezQSO (PI: Neeser) (4.5 nights/3 years for 12 o ) Science Goals: A search for extreme redshift QSOs (5.9 < z < 6.8) by surveying 12 o + 3 o in r‘, i‘, and z‘ filters to flux levels 10 times fainter than Sloan. Candidate selection based on: 1/ z‘ detections with r´ and i´ -band drop-outs 2/ J-band snapshot follow-up with (r‘/i‘ - z‘) vs (z‘ - J) colour selection 3/ spectroscopic confirmation. Within proposed KIDS area in order to provide high quality r´ and i´-band data

5. MPE/USM GTO Projects Based on 4 o Rz’ survey with SOFI J-band follow-up L/T type dwarf QSO candidate QSO candidate R Iz’ J

6. MPE/USM GTO Projects Limits (5  ; 2 “ aperture; AB): r‘ = 25.2 (KIDS) i‘ = 24.2 (KIDS) z‘ = 24.5 (KIDS + GTO) ==> a further 10 ksec / KIDS field Technical: single, contiguous field near south Galactic pole based on stellar paucity (  = 00 h 29 m 42 s ;  = -30 o 36‘ 00“) 12 o + 3 o (from DEGAS) AW Challenges: - finding ~200 good high z QSO candidates among 5.5 x 10 6 sources

7. MPE/USM GTO Projects VST-16 (PI: Meisenheimer) (65 nights for 18 o ) Science Goals: a large area, moderately deep, multi-colour survey with very accurate photometric redshifts for > 10 6 galaxies. - evolution of QSOs and AGN between 1 < z < 6 - galaxy evolution and SF history as a function of environment - large scale structures Technical: 18 square degrees in 7 fields: - processing narrow-band filters: cosmetics and = f(r) - accurate photometric redshifts (aperture-matched photometry)

8. Technical: 3 square degrees in 3 fields (COSMOS, GOODS-S, MUNICS-Deep) u’ g’ r’ i’ z' (much of which from KIDS) Strömgren v NB1 + NB2 + NB3(quad) + NB4(quad) available NIR (UKIDSS/VISTA) MPE/USM GTO Projects AW Challenges: - processing narrow-band filters: cosmetics and = f(r) - accurate photometric redshifts (aperture-matched photometry) - SAssociate lists of 10 6 sources up to 20 levels deep

9. MPE/USM GTO Projects OmegaTranS (PI: Saglia) (~25 nights / year; mostly bright) Science Goals: a survey for transiting extra-solar hot jupiters in short period (1 to 9 day) orbits. - explore the period, mass, and radius-distributions of close in planets and to understand the formation and evolution of these objects Technical: target ~120 000 F, G, and K-dwarfs (14.5-17.5mag) in 10 fields close to galactic plane (near l = 300 o ) 10 fields with 20 second exposure times ==> a cycle time of 12 minutes (incl. overhead) for eg., a 3 hour transit ==> 15 data points (5  detections will be at 1.8, 3.0, 4.8 milli-mag level for a R=15, 16, and 17 star, respectively) expected detection rate ~15-20 planets per year (only 8 currently known)

10. MPE/USM GTO Projects compared to OGLE (5 transits), OmegaTranS has 3 x larger field-of-view and 4 x more mirror area AW Challenges: - 20 sec. exposure times ==> ~7 TB of raw science data per year - detection of variable sources (from these filter-out the curves with the characteristics of transits) - photometric accuracies of ~2 milli-magnitudes

11. We propose to use German Omegacam GTO time for a large and deep variability survey, using the KIDS photometry as first epoch and observing a second (and sometimes a third) epoch in the g-band to similar depth. Main goal is the search for RR Lyrae star candidates in the extreme outer halo of the Milky Way. The survey also promises to contain a huge number of other interesting transients (e.g. SNe, GRB), variable objects (other types of variable stars, AGN), and up to now unknown objects. Bomans/Bochum We propose to study the space distribution of the white dwarf population with OmegaCam in a 125 sq. deg. field of sky. Scale height and mid-plane densities as well as proper-motions shall be derived for the first time. In particular the thick disk and halo populations are at the focus of our interest. It requires the distances of the stars to be determined. This can be achieved by estimating the white dwarf ’s gravity and using the mass-radius relation. We device a new technique to measure the Hδ line strength by combining narrow band (Str ̈ mgren v) with broad band photometry. The latter will become available from the OmegaCam KIDS survey. Hence we have to add the v band images only for selected survey fields. As a by-product we shall be able to measure the distribution of extreme Horizontal Branch stars through out the Galactic halo, another unprecedented measurement. Heber/Bamberg MPE/USM GTO Projects

12. Moehler/ESO Ziegler/Goettingen The excess of UV radiation observed in many elliptical galaxies and bulges of spiral galaxies poses an intriguing puzzle to our understanding of low mass stellar evolution, which predicts a negligible amount of hot stars able to produce UV radiation for such old metal-rich systems. Recent observations and theories suggest that extreme horizontal branch (EHB) stars and their progeny should be the cause of the UV excess. EHB star candidates have been detected towards the Galactic bulge, which is the closest representation of an old, metal-rich spheroid system and allows a detailed verification of the EHB scenario for the UV excess by studying individual stars. In one bulge field we have observed spectra of EHB star candidates, most of which are indeed evolved hot stars. We now want to extend our study to other areas of the bulge by means of wide field multi-band photometry. We will use the Halpha filter segments on OmegaCAM to image the [Oii] 3727 line redshifted to z = 0.77. This will yield star formation rates down to ≈ 1 Msun to rapidly decline. In addition to [Oii] at z ≈ 0.8, field galaxies will be visible at z ≈ 0.35 via their Halpha and/or [Oiii] 5005 emission. Instead of extrapolating UV flux measurements as previous studies, we’ll examine emission line fluxes. MPE/USM GTO Projects