1. The Stellar OmegaCam-ITA GTO programs
Sudare: the evolution of a program conducted at the (examples shown)

2. Omecacam GTO Italian share in the Omegacam consortium 25 %
Total cash contribution 1.14 M€
Italian share in the Omegacam consortium
25 %
Italian Omegacam GTO: 12 night/yr × 10 yr
(+ 10 VLT nights)

3. Omecacam GTO Allocated ~45 of the 120 nights available
Title PI
duration
total
10 yr
20 yr
SUDARE: Supernova diversity and rate evolution
Cappellaro 3
120 40
OMEGA-WINGS: galaxy transformations in the infalling regions of galaxy clusters
Poggianti 2 60 30
Photometry and astrometry of the Galactic globular cluster Omega Centauri
Piotto 5 46 23
The structure of the Galactic external disk at low latitude
Momany 35
An Omegacam survey of Local Group dwarf galaxies
Held 4
128 32
TOTAL
389
125
137
Allocated ~45 of the 120 nights available
First two years over-subscribed by ~ 20-30%

4. Supernova diversity and rate evolution
Cappellaro E., Benetti S., Greggio L., Zampieri L.
Bufano F., Agnoletto, I. Turatto M., Inserra C., Pumo M.L.,
Botticella M.T., Valenti S., Pastorello A., Patat F. - =
Sudare: the evolution of a program conducted at the (examples shown)
SN 2000fc
type Ia z = 0.42 V=22.4
IAUC7537 4

5. SN rate evolution
Can be used to constrain the star formation history, models of
galaxy chemical evolution, and supernova progenitor scenarios
Thermonuclear (type Ia)
Core Collapse
A number of measurements of the SN Ia rate evolution have been collected in the last 5 year. They have been used to test different model of progenitor evolution
There are still discrepancies that need to be addressed.
Core collapse rate are still very few (only two groups) with no distinction as far as subtype (eg. it would be very interesting to measure the rate of Ib/c for their link with GRBs)
Cappellaro et al A&A 430, 93
Botticella et al A&A 479, 49

6. Questions to address Our aim: measure properties of the events
SN Ia diversity with cosmic age (prompt vs. tardy events)  cosmological distance scale
Core-Collapse diversity 
massive star evolution
nucleo-synthesis
collapsed remnants
SN Ic  hypernovae  GRBs
Our aim: measure properties of the events
and their rates. Relate them to the parent galaxies

7. Star Formation Rate History
VST + Omegacam niche
Star Formation Rate History
VST
LBT
JWST
JDEM
Misure con altri traccianti c’è un enorme dispersione
Funzione di salpiter errore 40per cento sull’assunzione delle masse

8. SUDARE Goal: Supernova detection and monitoring of ~200 SNe
3 yr monitoring of 1sqdeg field at limiting magnitude 25
frequency filter exposure purpose
every other day r min detection light curve
once a week g, i min classification extinction
Constraints: R.A. , > 5 days from full moon, seeing < 1.4”
80 r g, i exposures/yr  8 nights/yr

9. Requirements 4 night/yr × 3 yr from Omegacam/GTO
4 night/yr × 3 yr from VST/GTO
time allocation
scheduling requirements
service mode distributed over all year
data delivery
within 5-7 days (to allow for follow-up)

10. OMEGA-WARP
Momany Y., Zaggia S., Piotto G., Ortolani S., Carraro G., Bedin L., De angeli F.

12. Warp maximum: 240 or 270 ?
What is the best stellar tracer to probe the warp ?
Comparison with models
Comparison of the stellar warp with that found for the gas and dust
A Mon.Ring—Flare connection ?
Details: peculiar distance-Vrad of CMa (Martin et al. 2005) ?
Details: PM of CMa vs warp (Dinescu et al. 2005)
Details: the FWHM of CMa (Martinez-DelGado et al. 2005)
Details: RR Lyrae in CMa ?
Conclusion:….

14. Conclusions: CMa is almost surely of Galactic origin.
CMa is warp max. at 240
Gas-dust-stars show similar warping (amplitude & phase), arguing against an accretion
warp amplitude differences depend on tracer distance and contam.

15. OMEGACAM: address the origin and evolution of the warp Observations of old (10 Gyr stars) & comparison with 2MASS results.
Warp origin: (i) accretion of satellites; (ii) cosmic infall; (iii) intergalactic magnetic field; (iv) accretion of intergalactic medium
Revaz & Pfenniger

18. OMEGACAM
3 stripes 2x20 degrees long across the disk
2 colors g, i down to g=23.5.
along the path of the Carina orbit.
requested 65 hours to complete (35 omegacam + 35 STEP)

19. WFI Observations already done
by other groups in the last years
With a baseline of 5-7 years
It will be possible to do ~5mas
Precision PROPER MOTIONS

21. GOALS:
extend the knowledge of the stellar population and star formation history of the disk out to its outer edge (15-20kpc from us) in the direction of the south warp
have a clear view of the vertical and structure of the outer disk
understand the origin of the warp.
35 hours assigned on the second year.
REVISIONS
sinergies with the VISTA surveys and VHPAS