1 / 21

Weak Gravitational Flexion from HST GEMS and STAGES

Weak Gravitational Flexion from HST GEMS and STAGES. Barnaby Rowe with David Bacon (Portsmouth), Andy Taylor (Edinburgh), Catherine Heymans (U.B.C.), Richard Massey (Caltech), Dave Goldberg (Drexel). STAGES TEAM. Meghan Gray (PI) (Nottingham) David Bacon (Portsmouth)

hagop
Télécharger la présentation

Weak Gravitational Flexion from HST GEMS and STAGES

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. Weak Gravitational Flexionfrom HST GEMS and STAGES Barnaby Rowe with David Bacon (Portsmouth), Andy Taylor (Edinburgh), Catherine Heymans (U.B.C.), Richard Massey (Caltech), Dave Goldberg (Drexel)

  2. STAGES TEAM Meghan Gray (PI) (Nottingham) David Bacon (Portsmouth) Michael Balogh (Waterloo) Marco Barden (MPIA) Fabio Barazza (UTexas) Eric Bell (MPIA) Asmus Boehm (AIP) John Caldwell (UTexas) Boris Häußler (MPIA) Catherine Heymans (UBC) Knud Jahnke (MPIA) Shardha Jogee (UTexas) Eelco van Kampen (Innsbruck) Sergey Koposov (MPIA) Kyle Lane (Nottingham) Daniel McIntosh (UMass) Klaus Meisenheimer (MPIA) Chien Peng (STScI) Hans Walter Rix (MPIA) Sebastian Sanchez (CAHA) Rachel Somerville (MPIA) Andy Taylor (Edinburgh) Lutz Wisotzki (AIP) Christian Wolf (Oxford) Xianzhong Zheng (PMO) GEMS TEAM Hans Walter Rix (PI) (MPIA) Marco Barden (MPIA) Steven Beckwith (STScI) Eric Bell (MPIA) Andrea Borch (MPIA) John Caldwell (UTexas) Boris Häußler (MPIA) Catherine Heymans (UBC) Knud Jahnke (MPIA) Shardha Jogee (UTexas) Sergey Koposov (MPIA) Daniel McIntosh (UMass) Klaus Meisenheimer (MPIA) Chien Peng (STScI) Sebastian Sanchez (CAHA) Rachel Somerville (MPIA) Lutz Wisotzki (AIP) Christian Wolf (Oxford) Xianzhong Zheng (MPIA)

  3. Simulations exhibit an abundance of dark matter substructure at a wide range of scales… Cluster halo …they also suggest that halos follow a certain profile (e.g. the NFW density profile – see Navarro, Frenk & White 1997) Galaxy halo Detailed predictions exist for halo properties and substructure as a function of mass, formation time and environment… (Moore et al. 1999) …but these predictions remain untested

  4. “Traditional” weak lensing source Image transformations can often be described by a simple, locally linearized mapping: lens observer g =g1 + ig2

  5. Spin 1 Spin 2 Spin 3 Weak lensing to higher order: flexion

  6. Flexion is sensitive to matter variations at smaller scales than shear – it’s like a high pass filter for mass structure k x Cosmological predictions (see Bacon et al. 2006) show that flexion is particularly sensitive to dark matter structure at small scales

  7. Flexion from space We are using the GEMS and STAGES surveys for a combined shear-flexion weak lensing analysis • The fields each offer: • >800 arcmin2 of deep (~60 galaxies per arcmin2) space imaging from theHST-ACS. • >8 000 high-quality photometric redshifts from the COMBO-17 survey (see Wolf et al.2004).

  8. Measuring galaxy shapes We can make accurate measurements of galaxy shapes using the Shapelet formalism (see e.g. Refregier 2003, Massey & Refregier 2005) • Using this method we can decompose each image into a sum of orthogonal 2D basis functions • All shape information can then be easily quantified Massey et al. 2006

  9. PSF correction We built a detailed shapelet model of each star Using these models we can estimate the PSF across the survey images– then deconvolve our galaxies in shapelet space

  10. Shear and flexion measurements g G F

  11. Quick and dirty “STEP”

  12. lens galaxy q Galaxy-galaxy lensing is a useful tool for studying galaxy halo mass distributions source galaxy For shear, we may first look at the mean tangential shear within angular bins around foreground lenses… For flexion the median provides a better statistic, being less sensitive to the broad wings in F and G

  13. Galaxy-galaxy shear

  14. Galaxy-galaxy F

  15. Galaxy-galaxy G

  16. Flexion correlation statistics Massive foreground halo In a Universe in which matter is correlated (clumpy) we also expect correlations between the shears and flexions of pairs of galaxies, varying as a function of angular separation. Background galaxy Predictions for lensing correlation functionsC(q) (for gg, FF, GGetc.) exist, and can be used to constrain cosmological parameters.

  17. Cosmic flexion F G

  18. Summary • Flexion is a promising tool for studying dark matter structure on small scales • Measurements of flexion from HST GEMS and STAGES demonstrate that the signal can be accurately recovered • Maximum-likelihood analysis of galaxy-galaxy and cosmic flexion signals is underway; these will place new constraints upon small-scale dark matter structure

More Related