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F225W, F336W(U), F438W(B), F555W(V) F814W(I), F 487N(H  ),F125W(J),F160W(H)

EARLY TYPE GALAXIES: proposal summary for WFC3 SOC J. Silk + SOC (+ Kaviraj, Ferreras, Kay, Yi). Low redshift (z<0.1) early-type galaxies show widespread (>30%) recent star formation, 1-5% mass fraction, 300-500 Myrs old

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F225W, F336W(U), F438W(B), F555W(V) F814W(I), F 487N(H  ),F125W(J),F160W(H)

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  1. EARLY TYPE GALAXIES: proposal summary for WFC3 SOC J. Silk + SOC (+ Kaviraj, Ferreras, Kay, Yi) • Low redshift (z<0.1) early-type galaxies show widespread (>30%) recent star formation, 1-5% mass fraction, 300-500 Myrs old • Complex dynamic history revealed by age-correlated core kinematics • Merger histories with extended SFH are needed to fit multi-wavelength photometry • Did gas-rich major mergers of intermediate mass E’s form more massive E’s? Or dry mergers? • Or many minor mergers? • Do cores trace SMBH feedback? e.g. via dynamical scouring and/or via feedback from SMBH-induced outflows during core formation • Recent population synthesis modelling with AGB prefers young and dusty SED: • gas is shed by AGB stars should be dusty, whereas IGM infall should be dust-poor • Need WFC3 angular resolution + NUV +NIR photometry to • Compute the mass fraction of young stars (<1 Gyr old) to quantify past merger ‘dryness’ • Accurately measure structural parameters to study the presence of substructure, e.g. embedded disks, to explore the mass ratios and morphologies of their progenitors • Compare the distribution of dust, young stars and age-dated substructure to simulated 2D maps to constrain characteristics of the last merger event and the gas history SNR ~10 per pixel 5-100pc resolution F225W, F336W(U), F438W(B), F555W(V) F814W(I), F 487N(H),F125W(J),F160W(H) 30-50 orbits

  2. Major mergers were important at z >1

  3. The GALEX NUV colour magnitude relation • Expected tight relation in optical (g-r) CMR • Monolithic scenario (dustless) should give similar CMR in the UV • But NUV CMR shows a spread of 6 mags - strong UV sources present in nearby early-type galaxies

  4. THE POWER OF NUV AND NIR

  5. The power of NUV (ctd)

  6. THE POWER OF NIR Maraston 2006

  7. ETGs have complex star formation historiesas viewed in their predecessors (ERGs) at z=1.5-3 old passively evolving young starburst Papovich et al. 2006

  8. Pixel-by-pixel analysis: NGC 2974 (E3 type) Far-UV Near-UV Optical (F555W) GALEX UV detects star-forming ring at r=6.2kpc Pixel-by-pixel young+old 2-comp. analysis Age of young comp Mass of young comp

  9. SAURON SF?

  10. SAURON SF

  11. Stellar ‘age-maps’ in early-type galaxies Unambiguous presence of young stars in galaxy centre coincident with KDC! Kinematically decoupled core McDermid R. M., et al., astro-ph/06022318

  12. Kinematically decoupled cores (McDermid et al. 06) SAURON-OASIS Data: Compact KDCs: • Small: 100 pc's(≤ 0.1 Re) • Lightweight • Young: distinct, increasingly young toward center • Rotators Classic KDCs: Large: kpc's(0.3-0.4 Re) Massive Coeval: homogeneous old Non-rotators

  13. CO: central disks (Young & Bureau, in prep) BIMA-SAURON Data: NGC4459 • CO cospatial with young stars and central stellar/gas disk • CO and stars/gas co-rotating SAURON CO

  14. Observing list F225W F336W(U) F438W(B) F555W(V) F814W(I) F487N(H) F125W(J) F160W(H) SNR ~10 per pixel 5-100pc resolution

  15. DO MASSIVE ELLIPTICALS FORM BY MERGERS? Conselice 2005

  16. Build-up of luminosity and star formation rate Bouwens, Illingworth et al 2006

  17. DO MASSIVE ELLIPTICALS FORM BY MINOR MERGERS? Movie by T. Naab

  18. DO MASSIVE ELLIPTICALS FORM BY DRY MERGERS?Movie by T. Naab

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