observing with vst/ omegacam
DESCRIPTION
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. - PowerPoint PPT PresentationTRANSCRIPT
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Observing with VST/OmegaCAM
Want to submit an ‘open time’ observing
proposal for VST/OmegaCAM?2
NO, you can’t !
Time allocated to Public Surveys GTO, Chilean
(Open Time available in the future)
BUT
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- 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.
Observing with VST/OmegaCAM
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VST/OmegaCAM time allocation
• GTO/INAF: • GTO/OmegaCAM: 15% eligible 20% but
decreasedfor first years
• Chilean: 10%• Public Surveys: ~70% hrs
Allocated hours
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VST Public Surveys
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VST Public Surveys
528 hrs
657 hrs
207 hrs
(Feb 2013)
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KIDS Public Survey
Science cases of KIDS- Matter distribution in the universe through weak gravitational lensing
'Strong lensing'--> Measure dark matterin galaxy clusters--> Observations with HST
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- Gravitational lensing (KIDS)'Weak lensing'--> Measure dark matterall over the universe--> Need large field andvery sharp images--> OmegaCAM@VST!
KIDS Public Survey
dark energy, structure of galaxy halos,
evolution of galaxies and clusters,stellar streams and the Galactic halo.
Other science:
- synergy with VIKING (VISTA PS) covering the same area in 5 near-IR bands
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KIDS south
coverage(as of Feb’13)
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VPHAS+ Public SurveyGalactic plane survey (u,g,r,i,Hα)
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
NB_659 filter
Segmented filter purchased by members of the VPHAS+ consortium
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VPHAS+ Public SurveyGalactic 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
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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
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ATLAS coverage as of
Dec 2012
COMPLETED
REMAINING
g’-band
r’-band
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- Monitoring of Supernovae- Monitoring of stars in star clusters and dwarf galaxies- Wide-field surveys of galaxies and galaxy clusters
Science cases of OmegaCAM, GTO/Chilean:
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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 ATLASVPHAS+
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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
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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
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Data quality/QC0 at the telescope
DISTRIBUTION of IQ variation over FOV (based on ~10,000 images)
z’
g’
u’r’
i’
90% percentile
OB successfully executed if dIQ < 25%
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Performance: (based on ~10000 images)
Mean measured FWHM per filter
0.90 arcsec (r’,i’,z’)
0.95 arcsec (g’)
1.10 arcsec (u’)
Mean ellipticity 5 %
Mean dIQ 4.3%
Data quality/QC0 at the telescope
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Observing with VST/OmegaCAMhr
s/ni
ght
FM
FM
FM
Empty queues for full moon and thin conditions
that’s your niche for the near future!
~40 hrs per semester