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COSMOS (Cosmic Evolution Survey) COSMOS (cosmic evolution survey) Richard Massey with Nick Scoville, Roberto Abraham, Masaru Ajiki, Justin Alpert, Herve Aussel, Josh Barnes, Andrew Blain, Daniela Calzetti, Peter Capak, John Weak lensing results fromCarlstrom, the ChrisHST Carilli, Andrea Cimatti, Andrea Comastri, Marcella Corollo, Emannuel Daddi, Richard Ellis, Martin Elvis, COSMOS survey Amr El Zant, Shawn Ewald, Mike Fall, Alexis Finoguenov, Alberto Franceschini, Mauro Giavalisco, Richard Griffiths, Gigi Guzzo, Gunther Hasinger, Catherine Heymans, Chris Impey, Jean- Paul Kneib, Karel Nel, Jeyhan Kartaltepe, Jin Koda, Anton Koekemoer, Lisa Kewley, Alexie Leauthaud, Olivier LeFevre, Ingo Lehmann, Simon Lilly, Thorsten Lisker, Charles Liu, Henry McCracken, Yannick Mellier, Satoshi Miyazaki, Bahram Mobasher, Takashi Murayama, Colin Norman, Alex Refregier, Alvio Renzini, Jason Rhodes, Mike Rich, Dimitra Rigopoulou, Dave Sanders, Shunji Sasaki, Dave Schminovich, Eva Schinnerer, Marco Scodeggio, Kartik Sheth, Patrick Shopbell, Jason Surace, Yoshi Taniguchi, James Taylor, Dave Thompson, Neil Tyson, Meg Urry, Ludovic Van Waerbeke, Paolo Vettolani, Simon White, Lin Yan The view from Hubble QuickTime™ and a decompressor are needed to see this picture. Hubble Space Telescope data N. Scoville et al. (ApJ 2007) Largest ever HST survey • 577 contiguous ACS pointings • 1.6 square degrees in IF814W band (VSDSS at z=1) • Depth IF814W<26.6 (at 5) • 2 million galaxies • ~80 resolved galaxies/arcmin2 http://irsa.ipac.caltech.edu/Missions/cosmos.html Multicolour followup of COSMOS field P. Capak et al. (ApJ 2007), B. Mobasher et al. (ApJ 2007) Radio Δz/(1+z)= 0.05 , 0.15 X-ray Large-scale distribution of baryonic material N. Scoville et al. (ApJ 2007) Large-scale distribution of baryonic material QuickTime™ and a QuickTime™ and a YUV420 codec decompressor YUV420 codec decompressor are needed to see this picture. are needed to see this picture. Galaxy number density Weighted by stellar mass Large-scale distribution of baryonic material QuickTime™ and a TIFF (LZW) decompressor are needed to see this picture. Nick Scoville Deflection of light rays QuickTime™ and a decompressor are needed to see this picture. ESA/Hubble (M. Kornmesser & L. L. Christensen) Strong lensing NASA and A. Fruchter (STScI) Spot the difference Intrinsic galaxy shapes Gravitationally lensed galaxy shapes COSMOS mass map Gravitational lensing convergence ∝ projected mass • Each tick mark shows the averaged ellipticity of >100 galaxies • Density of resolved galaxies sets the resolution of a mass map • 71 galaxies/arcmin2 from space • ~20 galaxies/arcmin2 from ground Compare to simulations Gravitational lensing convergence ∝ projected mass • Largest ever survey with HST • 1.6 square degrees in IF814W band • Depth IF814W<26.6 (at 5σ) • 2 million galaxies, zmedian=1.2 • Small, diffraction-limited PSF • ~80 resolved galaxies/arcmin2 • Follow-up from radio to x-rays • Photo-zs from 17 optical/IR bands Dark matter simulation at z=0.5 Andrey Kravtsov and Anatoly Klypin (National Center for Supercomputer Applications) B-mode check for residual systematics R. Massey et al. (Nature 2007) Redshift tomography (palaeocosmology) z=0.7 z=0.5 z=0.3 z=1 z=0.7 3D dark matter map z=0.5 n o i t a n i =0.3 l z c e D NASA, ESA and R. Massey (California Institute of Technology) z=0 Right ascension 3D dark matter map animation QuickTime™ and a decompressor are needed to see this picture. ESA/Hubble (M. Kornmesser & L. L. Christensen) Statistical analysis of 3D mass distribution R. Massey et al. (ApJ 2007), J. Lesgourgues et al. (arXiv:0705.0533) Cosmological parameter constraints Shear-shear correlation function z=0.7 z=0.5 VHS Lyα forest Amount of power of z=0.3 SDSS Lyα forest WMAP COSMOS 3D weak lensing Angular scale on sky Growth of structure over cosmic time R. Massey et al. (ApJ 2007) Fraction of mass on small scales Redshift-distance relation James Taylor et al. (in prep) Well-know shape as a function of angular diameter distance from simple lens geometry Cumulative signal shear Redshift Cumulative signal shear Cumulative signal shear Redshift Redshift Comparison with baryons Weak lensing mass contours (HST) Extended x-ray emission (XMM-Newton) Sensitivity falls with redshift! Galaxy number density (Subaru/CFHT) Galaxy stellar mass (Subaru/CFHT) R. Massey et al. (Nature 2007) Mass vs light tomography (z~0.3) R. Massey et al. (Nature 2007) ~19Mpc × 19Mpc Mass vs light tomography (z~0.5) R. Massey et al. (Nature 2007) ~26Mpc × 26Mpc Mass vs light tomography (z~0.7) R. Massey et al. (Nature 2007) ~31Mpc × 31Mpc “Bullet” cluster 1E0657-56 Doug Clowe, Marusa Bradac et al. (Astrophysical Journal 2006) 400 kpc Largest particle accelerator in the Universe QuickTime™ and a Sorenson Video 3 decompressor are needed to see this picture. © NASA Future prospects Shear TEsting Programme (STEP) simulations R. Massey et al. (MNRAS 2004) Simulated image Real image Weak lensing signal is really weak. Animations show 0-10% shear in 1% steps (real signal is ~2%). Shear TEsting Programme (STEP) results C. Heymans et al. (MNRAS 2006) R. Massey et al. (MNRAS 2007) Shapelets basis functions 8 6 4 2 M 0 -2 Truncation of high spatial frequencies -4 -6 -8 http://www.astro.caltech.edu/~rjm/shapelets 0 2 4 6 8 N Conclusions Remarkably fast progress since first statistical detections of cosmic shear in 2000. Gravitational lensing is now a major tool in cosmology. We can now compare the large-scale distribution of baryons to that of mass. In general, baryonic structures are built inside a dark matter scaffold. Discrepancies on small scales reveal the different (e.g. non-interacting) properties of dark matter. Statistical analyses of the mass distribution constrain cosmological parameters, trace the growth of structure, and measure the expansion history of the universe. Could not have been done from the ground. Imaging from space (+photozs) is essential for high resolution mass reconstruction and redshift tomography over wider timescales. The untimely failure of ACS is heartbreaking. Hubble provides a unique proof of concept for ambitious, dedicated missions in the future. Y|Ç Face-on bullet James Jee et al. (Astrophysical Journal 2007)) Radial mass profile Two clusters along line of sight Face-on bullet QuickTime™ and a Motion JPEG A decompressor are needed to see this picture. NASA, ESA and M. J. Jee (Johns Hopkins University) In and out of the shadow of the Earth © NASA PSF variation J. Rhodes (ApJ 2007), J. Jee (ApJ 2005) HST’s thermal “breathing” affects both size and ellipticity of PSF Effective focus changes by •3μm per orbit •12μm in ~days PSF variation J. Rhodes (ApJ 2007) HST is really simple 1 © Hergé Charge Transfer (in)Efficiency STIS image, courtesy Paul Bristow CCD readout register Trailing during CCD readout creates a spurious, coherent ellipticity. Affects photometry, astrometry and morphology of faint galaxies. Effect of CTE trailing on the mass map Ground versus space Ground vs space (mass maps) R. Massey et al. (Nature 2007), M. Kasliwal et al. (Proc. AAS 2007) SPACE GROUND Using 71 galaxies per arcmin2 Ground vs space (B-mode/noise in mass maps) R. Massey et al. (Nature 2007), M. Kasliwal et al. (Proc. AAS 2007) SPACE GROUND Using 71 galaxies per arcmin2 Ground vs space (cluster detection over z range) M. Kasliwal et al. (Proc. AAS 2007) Redshift 0.73 Redshift 0.93 GROUND GROUND SPACE SPACE Redshift 0.35 Redshift 0.22 SPACE GROUND SPACE GROUND Lensing sensitivity with redshift 1/r2 Resolved background galaxies Foreground lensing sensitivity Redshift.
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