A Novel SIM- -BASED Technique for the BASED Technique for the A - PowerPoint PPT Presentation

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A Novel SIM- -BASED Technique for the BASED Technique for the A Novel SIM Precise Determination of Absolute Stellar Fluxes Precise Determination of Absolute Stellar Fluxes Jay B. Holberg LPL, University of Arizona Absolute Stellar Fluxes

A Novel SIM- -BASED Technique for the BASED Technique for the A Novel SIM Precise Determination of Absolute Stellar Fluxes Precise Determination of Absolute Stellar Fluxes Jay B. Holberg LPL, University of Arizona
Absolute Stellar Fluxes How Absolute Fluxes are Traditionally Measured 1. Pick a Bright Flux Standard - say Vega 2. Com pare the Observed Flux of Vega with a Calibrated Laboratory Standard – say a Black Body – using the Sam e Telescope. 3. Account for and Correct all System atic Errors Current Status 1. On an absolute physical scale stellar fluxes are uncertain at the level of 1% at optical wavelengths. 2. In the UV and the Near IR uncertainties are considerably higher.
Absolute Fluxes – DA White Dwarfs - SIM The basic idea: 1. Use White Dwarf Physics to Determine the Relative Fluxes of DA White Dwarfs. 2. Use Highly Accurate SIM Parallaxes to Convert These Relative Fluxes to Absolute Fluxes.
DA White Dwarfs • Pure-Hydrogen Photospheres • Fully Radiative Atm ospheres • Sim ple, Continuum -Dom inated Spectra
Spectral Fitting for T eff and log g Sirius B
Synthetic Photometry Sirius B Barstow et al. (2005) T eff = 25,193 (±37) K Log g = 8.556 (±0.010)
Stellar Photom etry ( ) 2 / π 2 = f 4 H ( T , log g ) R D λ λ eff f λ = Observed flux at the top of the Earth’s Atmosphere H λ ( T eff , log g) = Eddington Flux at the Stellar Surface R = Stellar Radius D = Stellar Distance H λ - Radiative Transfer – Physics of Hydrogen Atom R - White Dwarf Interior Physics – Mass-Radius Relation and White Dwarf Cooling
Correlation of Photometric Parallaxes with Trigonometric Parallaxes Fig. 2 Holberg et al. 2008
DA White Dwarfs can be used as absolute flux standards – if accurate parallaxes can be determined. Remaining Questions How accurately can we compute white dwarf synthetic fluxes? What residual uncertainties are associated with emergent fluxes? How well can we determine white dwarf radii?
Holberg et al. 2006

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