Astro nomical W ide-field I maging S ystem for E urope

Astronomical Wide-field Imaging System for EuropeAstronomical Wide-field Imaging System for Europe

MPE/USM Survey/GTO ProjectsMPE/USM Survey/GTO Projects

Mark Neeser MPE / ESO Mark Neeser MPE / ESO

Leiden Workshop Nov. 2005

MPE/USM GTO ProjectsMPE/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

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


AW Challenges: - processing narrow-band filters: cosmetics and = f(r)- accurate photometric redshifts (aperture-matched magnitudes)


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


Based on4 o Rz’survey withSOFI J-bandfollow-up

L/T typedwarf

QSOcandidate

QSOcandidate

R I z’ J


• 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 ( = 00h 29m 42s ; = -30o 36‘ 00“) • 12 o + 3 o (from DEGAS)

AW Challenges: - finding ~200 good high z QSO candidates among 5.5 x 106 sources


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 > 106 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:

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)


AW Challenges: - processing narrow-band filters: cosmetics and = f(r)- accurate photometric redshifts (aperture-matched photometry)- SAssociate lists of 106 sources up to 20 levels deep


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 = 300o)

• 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)


• 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

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 withOmegaCam 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


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 ofhot 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.


Documents

Astro nomical W ide-field I maging S ystem for E urope