1 / 12

AGN Clustering

AGN Clustering. by Sean Lake for Astro 278 2012. Obligatory Outline Slide. Context: basic AGN review. How clustering studies can help. Clustering quantities: ξ(r), w p (r p ). What these quantities tell us. Clustering studies done. Conclusions. Basic Facts. Luminosity: ≥10 5 L ☉

pabla
Download Presentation

AGN Clustering

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. AGN Clustering • by • Sean Lake • for Astro 278 2012

  2. Obligatory Outline Slide • Context: basic AGN review. • How clustering studies can help. • Clustering quantities: ξ(r), wp(rp). • What these quantities tell us. • Clustering studies done. • Conclusions.

  3. Basic Facts • Luminosity: ≥105 L☉ • Size: < 1 pc (variability) • Location: center of galaxies • Punchline: we believe this phenomenon to arise from the accretion disk around a supermassive black hole. • Mystery: how does the gas get there?

  4. The Role of Environment • Each of the three scenarios on the right have different relative clustering w.r.t. background galaxies • Can also test Unification Figure 2 from Alexander and Hickox 2011

  5. Measuring Crowdedness

  6. but What we Really Measure.... • Galaxy / dark matter (DM) halo positions are biased: • That bias is a function of characteristic halo mass • Thus correlation length, r0, gives a measure of halo mass. Figure 5 from Sheth et al. 2001

  7. Regular Galaxy Interlude Figure 5 from Coil et al. 2009

  8. X-ray AGN Clustering Figures 10 and 11 from Coil et al. 2009

  9. IR AGN Clustering Demonstrates that there is no difference between obscured & unobscured AGN Figure 7 from Hickox et al. 2011

  10. Summing it Up Figure 5 from Alexander and Hickox 2011

  11. Summary • Clustering ∈ environment • Measures the influence of outside galaxies in feeding BHs • Differentiates feeding mechanisms based on BH type. • Clustering allows tests of selection techniques (also, potentially, unification)

  12. Questions?

More Related