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On the source of the diffuse background light in HUDF

On the source of the diffuse background light in HUDF. Tuguldur Sukhbold Dr.Henry C. Ferguson Timothy Dolch Space Telescope Science Institute Aug 19, 2010. HUDF. Zodiacal Light >90%. Possible Sources.

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On the source of the diffuse background light in HUDF

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  1. On the source of the diffuse background light in HUDF TuguldurSukhbold Dr.Henry C. Ferguson Timothy Dolch Space Telescope Science Institute Aug 19, 2010

  2. HUDF

  3. Zodiacal Light>90%

  4. Possible Sources Low Z Galaxies VS Low z Galaxies (e.g. Kashlinsky et al. 2005) (e.g. Thompson et al. 2007) • Zodiacal Light • Faint Structures • Data not high resolution and crowded • Detector Issues • Method of Analysis

  5. New in this Summer Work • New set of data: UDF 05-01 & UDF 05-02 (Illingworth et al. 2010) • New method of analysis: P(D) • Improved Simulation

  6. Processing • Iteratively remove detector blemishes • Combined dithered images with some masking • Transfer combined image back to original image geometries and subtract • Smooth and detect blemishes or persistence • Mask and recombine for the final image • Create pure noise images in original detector coordinates • Gaussian statistics okay for these images; match sky background • Predicted RMS matches measured RMS to within a few percent • Combine these just as for the real images • Mask the detected sources

  7. Analysis: P(D) • Create a shuffled version of the image • Unmasked pixels are randomly shuffled, removing correlations • For both the shuffled and unshuffled version: • Convolve the masked images with kernels of various sizes • Compute the histogram of pixel intensities P(D) • Subtract the shuffled P(D) from the unshuffled P(D). • Excess is amplified when kernel matches the characteristic size of the sources

  8. Simulation Inclination Position angle Tune 2 parameters: • Slope of the Galaxy count • Size of the galaxies

  9. Sample Simulation

  10. Validation The galaxy count slope and the sizes are recovered

  11. Preliminary Results • Previously result on UDF-main: • F105W: α = 0.7, r = 0.24’’ • F125W: α = 0.65, r = 0.24’’ • F160W: α = 0.65, r = 0.24’’ • New Result on UDF-main: • F160W: α = 0.6, r = 0.12’’ • New Results on UDF 05-01: • F105W: α = 0.6, r = 0.12’’ • F125W: α = 0.6, r = 0.30’’

  12. Future Directions • More sophisticated models • Galaxy redshift and SED distributions • Galaxy Clustering • Limiting magnitude variation • Change arrays • Better calibration of detector issues: hot pixels, persistence and bad cosmic ray rejections

  13. References • Abraham et al. 1998 (http://adsabs.harvard.edu/abs/1998AGM....14..E08A) • Bock et al. 2006 (http://adsabs.harvard.edu/abs/2006NewAR..50..215B) • Illingworth et al. 2010 (http://archive.stsci.edu/proposal_search.php?mission=hst&id=11563) • Kashlinksy et al. 2005 (http://adsabs.harvard.edu/abs/2005PhR...409..361K) • Thompson et al. 2007 (http://adsabs.harvard.edu/abs/2007ApJ...657..669T)

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