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E-ELT Spectropolarimetry of Type Ia Supernovae in the Coma Supercluster

Dietrich Baade – ESO, Garching Lifan Wang – Texas Ferdinando Patat – ESO, Garching Others - Welcome. E-ELT Spectropolarimetry of Type Ia Supernovae in the Coma Supercluster. An E-ELT should want to have a high (higher than AO) spatial-resolution mode There will be no E-ELTI facility

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E-ELT Spectropolarimetry of Type Ia Supernovae in the Coma Supercluster

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  1. Dietrich Baade – ESO, Garching Lifan Wang – Texas Ferdinando Patat – ESO, Garching Others - Welcome E-ELT Spectropolarimetry of Type Ia Supernovae in the Coma Supercluster ESO Science Day

  2. An E-ELT should want to have a high (higher than AO) spatial-resolution mode There will be no E-ELTI facility Polarimetry attains a spatial resolution of ~3 Spectropolarimetry measures the shape of regions with different velocity and/or composition separately Contrary to E-ELTI and AO, this resolution does not depend on angular size (distance) but on flux only Spectropolarimetry requires TONS of photons Current E-ELT design permits polarimetry at no extra cost Cash expenditures at the instrument level below the noise The case for E-ELT spectropolarimetry ESO Science Day

  3. SNe Ia are (used as) standard candles Justification by physical models is patchySNe Ia are polarized (in lines and continuum)► Calibration depends on aspect angle Type Ia SNe ESO Science Day

  4. A relation between structure and absolute luminosity • 17 SNe Ia observed well before Vmax (the outliers are `special΄) • Trend: slower (brighter) SNe seem to be less polarized in Si II 635.5 • Delayed detonation as kind of an after-burner may • a) smooth out clumpy structures • b) burn more fuel and so make • SNe brighter Wang et al. 2006 ► Want to observe SNe at same distance: go to massive clusters ESO Science Day

  5. Distance modulus: -34.5 mag Absolute magnitude at maximum: -18.5 mag Apparent magnitude at maximum: 16 mag VLT (FORS1) limit for spectropolarimetry at m=16: 0.2% accuracy in 80 minutes ► Observations just barely possible at maximum E-ELT limit (@42m): can go 3.5 mag fainter SNe Ia in the Coma supercluster (I) ESO Science Day

  6. Stellar mass of Abell 1667: ~0.2 1015 M☺ Supernova rate: ~0.05/century/1010 M☺ ► Expect >1 SN/year One wide-angle camera can easily monitor many clusters and still detect SNe well before maximum light. ► Enough SNe to schedule flexibly with normal priority SNe in the Coma supercluster (II) ESO Science Day

  7. Quantitative measurement of effects of asphericity on luminosity calibration of SNe Ia Radial and angular chemical structure of ejecta Constraints on explosion mechanism (deflagration vs. delayed detonation) Immediate objectives ESO Science Day

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