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The Stellar OmegaCam-ITA GTO programs

The Stellar OmegaCam-ITA GTO programs. Omecacam GTO. Total cash contribution 1.14 M€. Italian share in the Omegacam consortium 25 %. Italian Omegacam GTO: 12 night/yr × 10 yr (+ 10 VLT nights). Omecacam GTO. Allocated ~45 of the 120 nights available

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The Stellar OmegaCam-ITA GTO programs

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  1. The Stellar OmegaCam-ITA GTO programs

  2. Omecacam GTO 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 • 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. - = SN2000fc type Ia z = 0.42 V=22.4 IAUC7537

  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 Cappellaro et al. 2005 A&A 430, 93 Botticella et al. 2008 A&A 479, 49

  6. Questions to address • 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. JDEM JWST VST LBT VST + Omegacam niche Star Formation Rate History

  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 dayr 30 min detection light curve once a week g,i 30 min classificationextinction Constraints: R.A. , > 5days from full moon, seeing < 1.4” 80 r + 30 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.

  11. 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:….

  12. 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.

  13. 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

  14. 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)

  15. 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

  16. 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

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