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Observing with VST/ OmegaCAM

Observing with VST/ OmegaCAM. Want to submit an ‘open time’ observing proposal for VST/ OmegaCAM ?. 2. NO, you can’t !. BUT. Time allocated to Public Surveys GTO, Chilean (Open Time available in the future). Observing with VST/ OmegaCAM.

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Observing with VST/ OmegaCAM

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  1. Observing with VST/OmegaCAM Want to submit an ‘open time’ observing proposal for VST/OmegaCAM? 2 NO, you can’t ! BUT Time allocated to Public Surveys GTO, Chilean (Open Time available in the future)

  2. Observing with VST/OmegaCAM • Policies:Following recommendations by STC and OPC, roughly 75% of the ESO time on VST (and VISTA) will be devoted to Public Surveys. • Public Survey Panel (PSP): experts from the community, review PS proposals submitted to ESO and give recommendation to OPC for final acceptance, periodically review progress and achievements of PS • ESO Survey Team (EST): evaluate and coordinate the operational implementation of public survey observations (OBs, strategy, time allocation), monitor the progress of the public surveys, oversee the delivery of data products from the Survey Teams to the ESO archive, etc.

  3. VST/OmegaCAM time allocation • GTO/OmegaCAM: 15% eligible 20% but decreased • for first years • Chilean: 10% • Public Surveys: ~70% • GTO/INAF: hrs Allocated hours

  4. VST Public Surveys

  5. VST Public Surveys (Feb 2013) 528 hrs 657 hrs 207 hrs

  6. KIDS Public Survey • Science cases of KIDS • Matter distribution in the universe through weak • gravitational lensing 'Strong lensing' --> Measure dark matter in galaxy clusters --> Observations with HST

  7. KIDS Public Survey - Gravitational lensing (KIDS) 'Weak lensing' --> Measure dark matter all over the universe --> Need large field and very sharp images --> OmegaCAM@VST! Other science: dark energy, structure of galaxy halos, evolution of galaxies and clusters, stellar streams and the Galactic halo. • synergy with VIKING (VISTA PS) • covering the same area in 5 near-IR • bands

  8. KIDS south coverage (as of Feb’13)

  9. VPHAS+ Public Survey Galactic plane survey (u,g,r,i,Hα) NB_659 filter Segmented filter purchased by members of the VPHAS+ consortium • Science cases of VPHAS+ • Identification and study of emission line objects • Wolf-Rayet and other massive evolved emission line stars in the • inner Milky Way • compact planetary nebulae and rapidly evolving post-AGB stars • Be stars of all types - including young Herbig stars • clustered and field T Tau stars

  10. VPHAS+ Public Survey Galactic plane survey (u,g,r,i, Hα) • a range of interacting binary stars: symbiotics, 'supersoft' compact • binaries, WD/NS/BH accreting binaries • white dwarfs, horizontal branch stars and large numbers of early • A-type stars via their strong Hα absorption

  11. ATLAS Public Survey • Science cases of ATLAS • Determine the dark energy equation of state by • detecting 'baryon wiggles' in the power-spectrum • of ~450000 z~0.7 Luminous Red Galaxies (LRGs) • photo-z from VST ATLAS + VHS imaging • Galaxy groups and clusters

  12. ATLAS coverage as ofDec 2012 g’-band r’-band COMPLETED REMAINING

  13. Science cases of OmegaCAM, GTO/Chilean: - Monitoring of Supernovae - Monitoring of stars in star clusters and dwarf galaxies- Wide-field surveys of galaxies and galaxy clusters

  14. OmegaCAM Data • REMEMBER: data from PUBLIC surveys becomes publicly • available immediately (accessible via ESO archive) • - Data volumes: 550 MB per file (uncompressed) • Approximately 80 GB per night (VISTA: ~200GB/night) • VST data reduction centers: AstroWise, CASU, VST tube • No data reduction at ESO, only for quality control KIDS ATLAS VPHAS+

  15. OmegaCAM Data/Data Access ESO Phase3: Public Survey Teams must deliver reduced data products to ESO (March 2013 first submission) Access to reduced images and catalogs: www.eso.org/sci/observing/phase3

  16. Operations + quality control at the telescope • no night astronomer, fully operated by TIOs (like at VISTA) • clear indication of how to classify an execution •  sophisticated QC0 script which determines OB grade • - quick pipeline reduction of 8/32 chips. QC0 evaluates • three IQ parameters: • mean FWHM, ellipticity, FWHM (IQ) variation across FOV

  17. Data quality/QC0 at the telescope DISTRIBUTION of IQ variation over FOV (based on ~10,000 images) z’ 90% percentile i’ g’ OB successfully executed if dIQ < 25% r’ u’

  18. Data quality/QC0 at the telescope Performance: (based on ~10000 images) Mean measuredFWHM per filter 0.90 arcsec (r’,i’,z’) 0.95 arcsec (g’) 1.10 arcsec (u’) Mean ellipticity5 % Mean dIQ 4.3%

  19. Observing with VST/OmegaCAM Empty queues for full moon and thin conditions ~40 hrs per semester FM  that’s your niche for the near future! FM hrs/night FM

  20. QUESTIONS? ASK NOW OR WRITE TO usd-help@eso.org THANKS

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