html5-img
1 / 13

Dark Matter Substructure Probed by Strong Gravitational Lenses

Dark Matter Substructure Probed by Strong Gravitational Lenses. Aliza Malz Leonidas Moustakas and Jason Rhodes SURF 2007. Gravitational Lensing. Mass bends spacetime Light distorted near mass Observe image caused by gravity Learn about dark matter. Strong vs. Microlensing.

mandell
Download Presentation

Dark Matter Substructure Probed by Strong Gravitational Lenses

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. Dark Matter Substructure Probed by Strong Gravitational Lenses Aliza Malz Leonidas Moustakas and Jason Rhodes SURF 2007

  2. Gravitational Lensing • Mass bends spacetime • Light distorted near mass • Observe image caused by gravity • Learn about dark matter

  3. Strong vs. Microlensing • Strong lensing multiplies images • Microlensing distorts magnification of images

  4. The Lens Equation •  =  -  •  = -  x DS/DLS •  =  -  x DLS/DS • DS = DS - DL

  5. Caustic Maps * 2 * 4 Cusp Weak Fold • Map in source plane • Determines type of gravitational lensing

  6. Display caustic maps Process magnification data Convolution Methods

  7. Caustic Crossings • Motion of source over caustic map • Magnification over time or space reveals nature of dark matter • Identified by second derivative threshold on lightcurve • Learn nature of dark matter from caustic crossing

  8. Observations

  9. Source Size • α = 4GM/(c2b) • α(θ) = 4GM/(c2θdl) • θds = θsds + αdls • α(θ) = ds/dls (θ – θs) • θ - θs = 4GM/(θc2) dls/dsdl • θE = (4GM/c2 dls/dlds)1/2

  10. Variations in Source Size • Ideally small = 0.001 Re • Observations = 0.1 – 1.0 Re • Simulations = 0.01 – 0.1 Re

  11. Threshold Adjustment

  12. Future Research • Eliminate convolution method • Average microlensing events to equate with strong lensing effect • Remove microlensing from strong lensed image

  13. Acknowledgments • Leonidas Moustakas, Jason Rhodes • SFP, SURF, and Carol Casey • IDL • NASA’s IDLAstro Library • Leonidas Moustakas’ lamlib and eidol Libraries • Fanning Consulting’s coyote Library • Aaron Barth’s ATV Library • John Moustakas’ RED Library • Craig Markwardt’s CM Library • Chuck Keeton’s dma.100 software

More Related