1 / 15

Weak Lensing with the LBC

Weak Lensing with the LBC. Paul Martini The Ohio State University. Schloß Ringberg - 15 July 2008. Collaborators. Mandeep Gill Klaus Honscheid Chris Kochanek Molly Peeples Rick Pogge David Weinberg Julia Young. Motivation.

chyna
Download Presentation

Weak Lensing with the LBC

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 Lensing with the LBC Paul Martini The Ohio State University Schloß Ringberg - 15 July 2008

  2. Collaborators • Mandeep Gill • Klaus Honscheid • Chris Kochanek • Molly Peeples • Rick Pogge • David Weinberg • Julia Young

  3. Motivation • The mass function of clusters of galaxies is an important cosmological probe • Weak lensing provides the only direct measure of mass that is independent of complex baryonic physics • Other cluster observables need to be calibrated for upcoming dark energy surveys • A reasonable sample could provide a competitive measure of M and 8

  4. Cluster Mass Function M2 x (# dz-1 d-1 dM-1) Sensitivity of the cluster mass function to cosmological parameters

  5. Relation of Shear to Mass tangential shear cosmological dependence mass distribution T ~ few x 10-2 at the virial radius of a massive, z~0.3 cluster  ~ e/2Ngal1/2 For e ~ 0.3, need few x 103 galaxies for S/N~5

  6. Observations MAX3 Abell 1835 MAX5 g i

  7. 0.8” Seeing Statistics • SDT • Two clusters (Abell 611 and MS1358) • Five hours of 12 hours awarded • Or good seeing five hours out of 36 nights • OSU/RC Spring/Summer 2008 • Four clusters (Abell 1835, MAX3, MAX5, MAX8) • Six hours of 15 hours awarded • Six hours out of 18 nights

  8. Analysis g-band seeing is 0.55” 2’ x 2’ • Abell 611 at z=0.3

  9. Polar Shapelets Set of orthogonal basis functions with explicit rotational symmetry (Laguerre polynomials) Fit all candidate background galaxies Fit foreground stars to characterize PSF Massey et al. (2007)

  10. Example Decomposition Decomposition of stars and galaxies into shapelets coefficients simplifies removal of PSF anisotropies Massey & Refriegier (2005)

  11. Artifical Cluster Test

  12. rotator error to cluster center Results for Abell 611 E-mode to cluster center measures T B-mode systematics test

  13. Future Future? Potential cosmological constraints from measurements of the 50 richest, z~0.3 clusters in the SDSS equatorial stripe WMAP 3-year Yoo & Weinberg, in prep

  14. Summary • LBC is well suited to weak lensing studies of moderate redshift clusters • Preliminary analysis of Abell 611 suggests that ~0.02 can be measured with S/N>5 • Analysis of all clusters observed to date should help calibrate other cluster observables • Comparison of weak lensing measurement techniques will be valuable for future dark energy experiments

More Related