EUCLID Strong Lensing Science Working Group Report...
|
|
|
- Archibald Chambers
- 5 years ago
- Views:
Transcription
1 EUCLID Strong Lensing Science Working Group Report... December 3, 2012
2 SLSWG will evaluate EUCLID capabilites in strong lensing. What we expect: - Over deg 2, there are cluster and group lenses, galaxy-galaxy lenses.
3 What we hope: - to use those lenses for the study of DM peaks up to redshift 1 - to probe DM substructure, time delays - cosmology related evolution of lensing statistics
4 What we need: - detect most of the candidates automatically - compute the selection function - compute the probability distribution functions wrt arc properties
5 2012/3 2013/4 2014/5 2015/6 2016/7 2017/8 2018/9 2019/0 2020/1 SLSWG participates to OU-SHE WP 8000 Euclid Reviews: July or Sept SHE Reviews: Early May or Late June and Nov/Dec SHE Implementation Plan Euclid Review Euclid Review Euclid Review Euclid Review Euclid Review Euclid Review Launch VIS WP3200: CTI Algorithm VIS in SDC Blind testing Finders (source-selected) WP1000: Requirements WP2000/2100: Shear - Theory Algorithms & Tests Validate In SDC Upgrades Upgrades WP3000: SHE SIM - Basic Complex Validate To OUSIM Upgrade OU SIM Upgrade OU SIM WP4000: Flexion - Theory Algorithms & Tests Validate In SDC Upgrades EMA VIS PSF from OU-SHE Validation + Measurement of selection function Catalogues Redshifts (s,l) Images Spectra EMA WP5000: CTI Algorithms & Tests Validate In SDC Upgrades Upgrades SHE WP6000: SHE Systematics: Methods WP7000: Code Validation Methods WP8000: Strong Lensing WP9000: Morphometry Algorithms & Tests Validate In SDC 3D Upgrades Algorithms & Tests Validate In SDC Upgrades Algorithms & Tests Validate In SDC Upgrades Finders (lens-selected) LE3 WP2000: WL power and 3-d maps WL & GC in SDC E2E Runs OU-VIS OU-NIR OU-SPE OU-PHZ OU-LE3 OU-SIM OU-EXT OU-SIR Monday, 14 May 2012
6
7 Participate to OU-LE3 Cluster WP Tasks: - Identification of clusters by strong lensing - derivation of SL cluster masses
8 SLSWG working method WG meeting each 6 months: Kick-Off April 2012 (Lausanne). Pipeline meeting October 2012 (Groningen). Next... April 2013 (Bologna). Bi-weekly teleconference (Google Hangout) All minutes and reports may be found on
9 Assignment 1: realistic strong lensing simulations: Bologna Lens Factory (B Metcalf, M Menneghetti, C. Gioccoli) EUCLID Vis (Menneghetti et al.) Cluster Simulations: NFW halos, Sersic model stellar mass and light distributions of galaxies. Real background galaxies from UDF, shapelet deconvolved Galaxies: NFW halo, Sersic model stellar mass distribution, real HST massive galaxy light distribution. Real background galaxies from UDF, shapelet deconvolved Outputs: realistic single EUCLID images of simulated clusters, with many multiple image systems
10 Assignment 1: realistic strong lensing simulations: Bologna Lens Factory (B Metcalf, M Menneghetti, C. Gioccoli) EUCLID Vis (Metcalf) Field simulations, Millenium and C. Baugh provided cone, Ray tracing of enriched background to increase SL density. Images are also on the Bologna lens factory database page - only one filter for now images are with noise and Euclid-like PSF. Source model: devaucouleur + exp disk
11 Assignment 1: realistic spectroscopic simulations (NISP): LAM, CRAL (Jullo et al.) Recycle as much as possible what has been donne for MUSE.
12 Assignment 2: Test arcfinders (Cabanac et al., Seidel et al., Gavazzi et al.) Arcfinder (More et al.) Three arc finders already exist, two based on Alard s elongation estimator (Seidel, More). One using Gavazzi s small scale ring detector. The objective is to derive detector efficiencies wrt arc properties purity/completeness tables
13 G1 G2 P1 P2 P3 P4 A1 A2 A3 A1 G3 A1
14 More/Alard G1 G2 G3
15
16
17 Assignment 3: Test strong lensing modellers (Kneib et al., Jullo, Marshall et al.) Release publicly the simulation and organize a lensing challenge (akin to GREAT challenges) Probe the potential of citizen science for detection of none obvious cases.
Elliptical galaxies as gravitational lenses
Elliptical galaxies as gravitational lenses Raphaël Gavazzi UC Santa Barbara R. Gavazzi, Séminaire IAP, 22/12/06, 1 Outline Issues on Early-Type Galaxies (ETGs) Gravitational lensing, the basics SLACS:
Euclid and MSE. Y. Mellier IAP and CEA/SAp.
Euclid and MSE Y. Mellier IAP and CEA/SAp www.euclid-ec.org Euclid and MSE CFHT Users Meeting, Nice 02 May, 2016 Euclid Primary Objectives: the Dark Universe Understand The origin of the Universe s accelerating
Strong Lensing with Euclid and SKA The future of strong lensing with 100,000+ lenses
Strong Lensing with Euclid and SKA The future of strong lensing with 100,000+ lenses Léon Koopmans (Kapteyn Astronomical Institute) Vegetti et al. McKean et al. Euclid-SKA Synergy - Oxford, Sept.16 2013
Cosmological simulations for Euclid
Cosmological simulations for Euclid Pablo Fosalba (Barcelona) Robert Smith (Zürich) Stéphane Colombi (Paris) Carlton Baugh (Durham) Marco Baldi (Münich) and many others 1 Outline 1. Computing the matter
Euclid cosmological simulations WG: the Flagship mock
Euclid cosmological simulations WG: the Flagship mock P.Fosalba (ICE, CSIC) on behalf of the CosmoSim-SWG Simulated Skies meeting, Madrid, April 2018 1 CosmoSim-SWG in a nutshell Objectives: Develop simulations
Durham Lightcones: Synthetic galaxy survey catalogues from GALFORM. Jo Woodward, Alex Merson, Peder Norberg, Carlton Baugh, John Helly
Durham Lightcones: Synthetic galaxy survey catalogues from GALFORM Jo Woodward, Alex Merson, Peder Norberg, Carlton Baugh, John Helly Outline 1. How are the lightcone mocks constructed? 2. What mocks are
Euclid Data Processing
Euclid Data Processing Martin Kümmel, on behalf of the Euclid Consortium LUDWIGMAXIMILIANSUNIVERSTITÄT MÜNCHEN Faculty of Physics Chair for Cosmology and Structure Formation Asterics Kümmel 28. June 2018
Cluster strong lensing as a probe of the high redshift Universe
Cluster strong lensing as a probe of the high redshift Universe Jean-Paul KNEIB Laboratoire Astrophysique de Marseille (LAM) now on leave at: LASTRO - EPFL Mont-Blanc 1 Chapters Introduction on cluster
Mapping Baryonic & Dark Matter in the Universe
Mapping Baryonic & Dark Matter in the Universe Jean-Paul KNEIB Laboratoire d Astrophysique de Marseille, France A. Leauthaud, R. Massey, J. Rhodes, the COSMOS team, and many others Outline Motivation Basics
Clusters of Galaxies with Euclid
Clusters of Galaxies with Euclid Figure by L. Caridà A. Biviano (INAF-OATS) largely based on Sartoris, AB, Fedeli et al. 2016 Euclid: ESA medium class A&A mission, selected Oct 2011, to be launched in
A Spectroscopically-Confirmed Double Source Plane Lens in the HSC SSP Tanaka, Wong, et al. 2016, ApJ, 826, L19
A Spectroscopically-Confirmed Double Source Plane Lens in the HSC SSP Tanaka, Wong, et al. 2016, ApJ, 826, L19 Kenneth Wong EACOA Fellow National Astronomical Observatory of Japan Masayuki Tanaka (NAOJ)
EIC Simulations. Thomas Kitching, EIC Weak Lensing & Simulation Working Groups
EIC Simulations Thomas Kitching A. Amara, S. Bridle, O. Boulade, B. Dobke, A. Fontana, A. Grazian, A. Heavens, A. Kiessling, M. Meneghetti, S. Paulin-Henriksson, J. Rhodes, A. Refregier, A. Taylor, R.
Galaxy morphology. some thoughts. Tasca Lidia Laboratoire d Astrophysique de Marseille
Galaxy morphology some thoughts Tasca Lidia Laboratoire d Astrophysique de Marseille Hubble tuning fork Elliptical Spiral Irregular Morphological evolution Local Galaxies, z~0 Distant galaxies, z~1 High-z
Euclid Legacy Science
Euclid Legacy Science Simona Mei GEPI Observatory of Paris University of Paris 7 Denis Diderot James G. Bartlett APC - University of Paris 7 Denis Diderot on the basis of the work of legacy coordinators
Dark Energy with the Euclid Space Mission. Y. Mellier On behalf of the Euclid Consortium. Euclid Consortium.
Dark Energy with the Space Mission Y. Mellier On behalf of the http://www.euclid-ec.org Instrument Overall WP Breakdown VG :1 Itzykson, IPhT-CEA Saclay June 18-20, 2012 Objective of the Mission Instrument
Study of environment in galaxy surveys
Post-doc Days DIFA+INAF(Bo) 5-6 February 2015 Study of environment in galaxy surveys Olga Cucciati Universita' di Bologna - DIFA INAF-Osservatorio Astronomico di Bologna My Gelmini countdown: 1 year and
COSMOS : Strong Lens Candidate
COSMOS 5921+0638: Strong Lens Candidate Timo Anguita Astronomisches Rechen-Institut Zentrum für Astronomie der Universität Heidelberg with: C. Faure (EPFL) J.-P. Kneib (LAM) J. Wambsganss (ARI/ZAH) C.
Extending Robust Weak Lensing Masses to z~1. Douglas Applegate, Tim Schrabback & the SPT-Lensing Team
Extending Robust Weak Lensing Masses to z~1 Douglas Applegate, Tim Schrabback & the SPT-Lensing Team 1 SPT Lensing Team Bonn Tim Schrabback Douglas Applegate Fatimah Raihan Chicago Brad Benson Lindsay
The Concentration-Mass relation from CLASH
The Concentration-Mass relation from CLASH Snowcluster 2015 Snowbird March 16, 2015 Julian Merten Marie Curie Fellow University of Oxford The CLASH One of three HST/MCT programs ~550 orbits Science Drivers
Euclid. Mapping the Geometry of the Dark Universe. Y. Mellier on behalf of the. Euclid Consortium.
Mapping the Geometry of the Dark Universe Y. Mellier on behalf of the http://www.euclid-ec.org Instrument Overall WP Breakdown VG :1 The ESA mission: scientific objectives Understand the origin of the
Cosmology with the ESA Euclid Mission
Cosmology with the ESA Euclid Mission Andrea Cimatti Università di Bologna Dipartimento di Astronomia On behalf of the Euclid Italy Team ESA Cosmic Vision 2015-2025 M-class Mission Candidate Selected in
A New Window of Exploration in the Mass Spectrum Strong Lensing by Galaxy Groups in the SL2S
A New Window of Exploration in the Mass Spectrum Strong Lensing by Galaxy Groups in the SL2S Marceau Limousin Strong Lensing Legacy Survey Collaboration (SL2S) Laboratoire d Astrophysique de Marseille
Probing the slope of cluster mass profile with gravitational Einstein rings: application to Abell 1689
Mon. Not. R. Astron. Soc. 386, 1169 1178 (2008) doi:10.1111/j.1365-2966.2008.12929.x Probing the slope of cluster mass profile with gravitational Einstein rings: application to Abell 1689 H. Tu, 1,2,3
Source plane reconstruction of the giant gravitational arc in Abell 2667: a condidate Wolf-Rayet galaxy at z 1
Source plane reconstruction of the giant gravitational arc in Abell 2667: a condidate Wolf-Rayet galaxy at z 1 Speaker: Shuo Cao Department of Astronomy Beijing Normal University Collaborators: Giovanni
Warm dark matter with future cosmic shear data
Workshop CIAS Meudon, Tuesday, June 7, 2011 Warm dark matter with future cosmic shear data Katarina Markovic (University Observatory Munich) markovic@usm.lmu.de in collaboration with Jochen Weller and
EUCLID Cosmology Probes
EUCLID Cosmology Probes Henk Hoekstra & Will Percival on behalf of the EUCLID The presented document is Proprietary information of the. This document shall be used and disclosed by the receiving Party
arxiv: v3 [astro-ph.co] 25 Feb 2014
![arxiv: v3 [astro-ph.co] 25 Feb 2014](/thumbs/89/98776822.jpg "arxiv: v3 [astro-ph.co] 25 Feb 2014")
Mon. Not. R. Astron. Soc., () Printed October 1, 218 (MN LATEX style file v2.2) A seven square degrees survey for galaxy-scale gravitational lenses with the HST imaging archive R.S. Pawase 1, F. Courbin
MSE: a «Velocity Machine» for Cosmology
Proposal: MSE: a «Velocity Machine» for Cosmology C. Schimd, S. de la Torre, E. Jullo, L. Tresse (LAM, Marseille), H. Courtois, Y. Copin (IPNL Lyon), T. Buchert, J. Richard (CRAL, Lyon), J.-P. Kneib (EPFL,
CAULDRON: dynamics meets gravitational lensing. Matteo Barnabè
CAULDRON: dynamics meets gravitational lensing Matteo Barnabè KIPAC/SLAC, Stanford University Collaborators: Léon Koopmans (Kapteyn), Oliver Czoske (Vienna), Tommaso Treu (UCSB), Aaron Dutton (MPIA), Matt
Weak Gravitational Lensing
Weak Gravitational Lensing Sofia Sivertsson October 2006 1 General properties of weak lensing. Gravitational lensing is due to the fact that light bends in a gravitational field, in the same fashion as
Cooking with Strong Lenses and Other Ingredients
Cooking with Strong Lenses and Other Ingredients Adam S. Bolton Department of Physics and Astronomy The University of Utah AASTCS 1: Probes of Dark Matter on Galaxy Scales Monterey, CA, USA 2013-July-17
What Gravitational Lensing tells us
What Gravitational Lensing tells us Catherine Heymans Institute for Astronomy, University of Edinburgh Six Six things lensing has has told told us us about Dark Matter How How lensing works First First
Strong Gravitational-Lensing by Galaxies: 30 years later...
Strong Gravitational-Lensing by Galaxies: 30 years later... Léon Koopmans ( Institute (Kapteyn Astronomical Stellar Dynamics Gravitational lensing JENAM - April 22, 2009 Some Applications of Galaxy Lensing
Today. Lookback time. ASTR 1020: Stars & Galaxies. Astronomy Picture of the day. April 2, 2008
ASTR 1020: Stars & Galaxies April 2, 2008 Astronomy Picture of the day Reading: Chapter 21, sections 21.3. MasteringAstronomy Homework on Galaxies and Hubble s Law is due April 7 th. Weak Lensing Distorts
Neutrinos as Probes. of Dark Matter. Hasan Yüksel The Ohio State University
Neutrinos as Probes of Dark Matter Institute for Gravitation and Cosmos, Inaugural Conference, Penn State University, August 9 - August 11, 2007 Hasan Yüksel The Ohio State University arxiv:0707.0196 [astro-ph]
LSST Cosmology and LSSTxCMB-S4 Synergies. Elisabeth Krause, Stanford
LSST Cosmology and LSSTxCMB-S4 Synergies Elisabeth Krause, Stanford LSST Dark Energy Science Collaboration Lots of cross-wg discussions and Task Force hacks Junior involvement in talks and discussion Three
Astronomy. Astrophysics. A PCA-based automated finder for galaxy-scale strong lenses
A&A 566, A63 (2014) DOI: 10.1051/0004-6361/201423365 c ESO 2014 Astronomy & Astrophysics A PCA-based automated finder for galaxy-scale strong lenses R. Joseph 1, F. Courbin 1, R. B. Metcalf 2, C. Giocoli
Dark Energy. Cluster counts, weak lensing & Supernovae Ia all in one survey. Survey (DES)
Dark Energy Cluster counts, weak lensing & Supernovae Ia all in one survey Survey (DES) What is it? The DES Collaboration will build and use a wide field optical imager (DECam) to perform a wide area,
arxiv: v1 [astro-ph.ga] 13 May 2016
![arxiv: v1 [astro-ph.ga] 13 May 2016](/thumbs/83/88355419.jpg "arxiv: v1 [astro-ph.ga] 13 May 2016")
Astronomy & Astrophysics manuscript no. DanutaParaficz arxiv c ESO 2018 May 2, 2018 The PCA Lens-Finder: application to CFHTLS D. Paraficz 1, F. Courbin 1, A. Tramacere 2, R. Joseph 1, R.B. Metcalf 3,
Testing the cold dark matter model with gravitational lensing
Testing the cold dark matter model with gravitational lensing Priyamvada Natarajan Departments of Astronomy & Physics Yale University In Memoriam: Vera Rubin New Directions in Theoretical Physics, January
Quantifying Secular Evolution Through Structural Decomposition
Quantifying Secular Evolution Through Structural Decomposition University of St Andrews / ICRAR (UWA) o How do structures form? bulge disk bar pseudo-bulge disk bulge??? o Are ellipticals and bulges essentially
Marco Gullieuszik INAF - Osservatorio Astronomico di Padova
Exploring the stellar population of nearby and high redshift galaxies with ELTs INAF - Osservatorio Astronomico di Padova The team R. Falomo L. Greggio M. Uslenghi INAF Osservatorio Astronomico di Padova
Weak Lensing: Status and Prospects
Weak Lensing: Status and Prospects Image: David Kirkby & the LSST DESC WL working group Image: lsst.org Danielle Leonard Carnegie Mellon University Figure: DES Collaboration 2017 for LSST DESC June 25,
Statistics of flux ratios in strong lenses: probing of dark matter on small scales
Statistics of flux ratios in strong lenses: probing of dark matter on small scales Daniel Gilman (UCLA) With: Simon Birrer, Tommaso Treu, Anna Nierenberg, Chuck Keeton, Andrew Benson image: ESA/Hubble,
Gravitational Lensing: Strong, Weak and Micro
P. Schneider C. Kochanek J. Wambsganss Gravitational Lensing: Strong, Weak and Micro Saas-Fee Advanced Course 33 Swiss Society for Astrophysics and Astronomy Edited by G. Meylan, P. Jetzer and P. North
Line-of-sight effects in strong lensing: Putting theory into practice
Prepared for submission to JCAP arxiv:1610.01599v2 [astro-ph.co] 28 Apr 2017 Line-of-sight effects in strong lensing: Putting theory into practice Simon Birrer, Cyril Welschen, Adam Amara, Alexandre Refregier
TMT and Space-Based Survey Missions
TMT and Space-Based Survey Missions Daniel Stern Jet Propulsion Laboratory/ California Institute of Technology 2014 California Institute of Technology TMT Science Forum 2014 July 17 Outline Summary of
Crurent and Future Massive Redshift Surveys
Crurent and Future Massive Redshift Surveys Jean-Paul Kneib LASTRO Light on the Dark Galaxy Power Spectrum 3D mapping of the position of galaxies non-gaussian initial fluctuations Size of the Horizon:
The sizes of z ~ 6-8 lensed galaxies from the Hubble Frontier Fields data of Abell 2744
The sizes of z ~ 6-8 lensed galaxies from the Hubble Frontier Fields data of Abell 2744 Kawamata+15, ApJ, 804, 103 Ryota Kawamata The University of Tokyo With: Masafumi Ishigaki, Kazuhiro Shimasaku, Masamune
Cosmology with weak-lensing peak counts
Durham-Edinburgh extragalactic Workshop XIV IfA Edinburgh Cosmology with weak-lensing peak counts Chieh-An Lin January 8 th, 2018 Durham University, UK Outline Motivation Why do we study WL peaks? Problems
The phenomenon of gravitational lenses
The phenomenon of gravitational lenses The phenomenon of gravitational lenses If we look carefully at the image taken with the Hubble Space Telescope, of the Galaxy Cluster Abell 2218 in the constellation
Multiwavelength Analysis of CLASH Clusters
The Galaxy Cluster MACSJ 1206.2 From Umetsu et al. 2012 2' N E Multiwavelength Analysis of CLASH Clusters Seth Siegel Collaboration Bolocam Team: Sunil Golwala, Jack Sayers, Nicole Czakon, Tom Downes,
The Euclid Mission. Konrad Kuijken on behalf of the Euclid Consortium.
The Euclid Mission Konrad Kuijken on behalf of the Euclid Consortium www.euclid-ec.org The Euclid Mission Photo-z meeting Sendai, 17/5/2017 SN Ia Mohr 2004 Observational probes of Dark Energy Clusters
Some issues in cluster cosmology
Some issues in cluster cosmology Tim McKay University of Michigan Department of Physics 1/30/2002 CFCP Dark Energy Workshop 1 An outline Cluster counting in theory Cluster counting in practice General
Gravitational Lensing. Y. Mellier - IAP
Gravitational Lensing Y. Mellier - IAP Gravitational deflection of light Source D LS Lens D OS D OL Observer Gravitational deflection of light Source Projected gravitational potential D LS Lens D Angular
Shape Measurement: An introduction to KSB
Shape Measurement: An introduction to KSB Catherine Heymans Institute for Astronomy, University of Edinburgh, UK DUEL Weak Lensing School September 2009 at the end of the week you ll be able to... Use
Cecilia Fariña - ING Support Astronomer
Cecilia Fariña - ING Support Astronomer Introduction: WHT William Herschel Telescope 2 Introduction: WHT WHT located in La Palma, Canary Islands, Spain William Herschel Telescope l 2 3 Introduction: WHT
Mapping Dark Matter in Galaxy Clusters: Gravitational Lensing & Numerical Simulations
Mapping Dark Matter in Galaxy Clusters: Gravitational Lensing & Numerical Simulations Marceau Limousin Laboratoire d Astrophysique de Toulouse-Tarbes, Université de Toulouse, CNRS 57 avenue d Azereix,
Shear Power of Weak Lensing. Wayne Hu U. Chicago
Shear Power of Weak Lensing 10 3 N-body Shear 300 Sampling errors l(l+1)c l /2π εε 10 4 10 5 Error estimate Shot Noise θ y (arcmin) 200 100 10 6 100 1000 l 100 200 300 θ x (arcmin) Wayne Hu U. Chicago
arxiv: v1 [astro-ph.co] 17 Jul 2013
![arxiv: v1 [astro-ph.co] 17 Jul 2013](/thumbs/72/66544179.jpg "arxiv: v1 [astro-ph.co] 17 Jul 2013")
Draft version July 19, 2013 Preprint typeset using L A TEX style emulateapj v. 5/2/11 THE SL2S GALAXY-SCALE LENS SAMPLE. III. LENS MODELS, SURFACE PHOTOMETRY AND STELLAR MASSES FOR THE FINAL SAMPLE Alessandro
ELTs for Cluster Cosmology
ELTs for Cluster Cosmology Anja von der Linden Stony Brook University UCLA, April 4th, 2018 Cosmology only ~5% of the Universe in a form we understand (stars, planets, atoms baryons ) what is dark energy?
The Gravitational Microlensing Planet Search Technique from Space
The Gravitational Microlensing Planet Search Technique from Space David Bennett & Sun Hong Rhie (University of Notre Dame) Abstract: Gravitational microlensing is the only known extra-solar planet search
Galaxy Group Masses: Lensing, Dynamics & Xrays
Galaxy Group Masses: Lensing, Dynamics & Xrays Laura Parker Michael Balogh Richard Bower Ray Carlberg Jennifer Connelly Alexis Finoguenov Robbie Henderson Annie Hou Mike Hudson Sean McGee John Mulchaey
Cosmology and Large Scale Structure
Cosmology and Large Scale Structure Alexandre Refregier PASCOS13 Taipei 11.22.2013 Matter Baryons Dark Matter Radiation Inflation Dark Energy Gravity Measuring the Dark Universe Geometry Growth of structure
The Caustic Technique An overview
The An overview Ana Laura Serra Torino, July 30, 2010 Why the mass of? Small scales assumption of dynamical equilibrium Mass distribution on intermediate scales (1 10 Mpc/h) Large scales small over densities
Reduced data products in the ESO Phase 3 archive (Status: 02 August 2017)
Reduced data products in the ESO Phase 3 archive (Status: 02 August 2017) The ESO Phase 3 archive provides access to reduced and calibrated data products. All these data are stored in standard formats
SUPPLEMENTARY INFORMATION
doi:10.1038/nature12001 Sample Selection The dusty-spectrum sources targeted for the ALMA observations described here were found in the SPT survey. The full survey comprises 2540 deg 2 of mapped sky, but
Gravitational Lensing. A Brief History, Theory, and Applications
Gravitational Lensing A Brief History, Theory, and Applications A Brief History Einstein (1915): light deflection by point mass M due to bending of space-time = 2x Newtonian light tangentially grazing
Lensing by (the most) massive structures in the universe
Lensing by (the most) massive structures in the universe today: basics of lensing tomorrow: how can we investigate the matter content of galaxy clusters using lensing (strong and weak) Wednesday: cosmology
The shapes of faint galaxies: A window unto mass in the universe
Lecture 15 The shapes of faint galaxies: A window unto mass in the universe Intensity weighted second moments Optimal filtering Weak gravitational lensing Shear components Shear detection Inverse problem:
PHY323:Lecture 7 Dark Matter with Gravitational Lensing
PHY323:Lecture 7 Dark Matter with Gravitational Lensing Strong Gravitational Lensing Theory of Gravitational Lensing Weak Gravitational Lensing Large Scale Structure Experimental Evidence for Dark Matter
Introduction to SDSS-IV and DESI
Introduction to SDSS-IV and DESI Ho Seong HWANG (KIAS) 2015 January 27 The 4th Survey Science Group Workshops SDSS-I: 2000-2005 SDSS-II: 2005-2008 SDSS-III: 2008-2014 SDSS-IV: 2014-2020 SDSS-IV: Project
Probing Dark Matter Halos with Satellite Kinematics & Weak Lensing
Probing Dark Matter Halos with & Weak Lensing Frank C. van den Bosch (MPIA) Collaborators: Surhud More, Marcello Cacciato UMass, August 2008 Probing Dark Matter Halos - p. 1/35 Galaxy Formation in a Nutshell
Plato, Euclid and the New Hard X-Ray mission
Schiaparelli and his Legacy Meeting on Future planetary, scientific and robotic space missions Biblioteca Nazionale Universitaria, Torino, 21/10/2010 Template reference : 100181670S-EN Plato, Euclid and
Gravitational Lensing of the Largest Scales
What is dark matter? Good question. How do we answer it? Gravitational lensing! Gravitational lensing is fantastic Why Clusters of Galaxies Because they are cool!! Studying empirical properties of dark
The Early Universe John Peacock ESA Cosmic Vision Paris, Sept 2004
The Early Universe John Peacock ESA Cosmic Vision Paris, Sept 2004 The history of modern cosmology 1917 Static via cosmological constant? (Einstein) 1917 Expansion (Slipher) 1952 Big Bang criticism (Hoyle)
Cluster Multi-Wavelength Studies: HSC/SC-WL + SL+ SZE + X-ray + Dynamics
J-P-T T HSC WS (Jan. 19, 2009) Cluster Multi-Wavelength Studies: HSC/SC-WL + SL+ SZE + X-ray + Dynamics Keiichi Umetsu (ASIAA, LeCosPA/NTU) Contents 1. Importance of Cluster Multi-Wavelength Studies for
Mapping Dark Matter with the Dark Energy Survey
Mapping Dark Matter with the Dark Energy Survey Tim Eifler On behalf of many people in the DES collaboration DaMaSC IV: Beyond WIMP Dark Matter Aug. 30, 2017 Disclaimer DES has recently published Year
LSST, Euclid, and WFIRST
LSST, Euclid, and WFIRST Steven M. Kahn Kavli Institute for Particle Astrophysics and Cosmology SLAC National Accelerator Laboratory Stanford University SMK Perspective I believe I bring three potentially
Planck was conceived to confirm the robustness of the ΛCDM concordance model when the relevant quantities are measured with much higher accuracy
12-14 April 2006, Rome, Italy Francesco Melchiorri Memorial Conference Planck was conceived to confirm the robustness of the ΛCDM concordance model when the relevant quantities are measured with much higher
Firenze (JPO: 28/07/17) Small Scale Crisis for CDM: Fatal or a Baryon Physics Fix
Firenze (JPO: 28/07/17) Small Scale Crisis for CDM: Fatal or a Baryon Physics Fix CBR Spectrum Planck and all-a Perfect Fit to the CDM Expectation Precise measurements of the CBR specify the cosmological
High Redshift Universe
High Redshift Universe Finding high z galaxies Lyman break galaxies (LBGs) Photometric redshifts Deep fields Starburst galaxies Extremely red objects (EROs) Sub-mm galaxies Lyman α systems Finding high
Large Imaging Surveys for Cosmology:
Large Imaging Surveys for Cosmology: cosmic magnification AND photometric calibration Alexandre Boucaud Thesis work realized at APC under the supervision of James G. BARTLETT and Michel CRÉZÉ Outline Introduction
Results from the 2500d SPT-SZ Survey
Results from the 2500d SPT-SZ Survey Lindsey Bleem Argonne National Laboratory! March 15, 2015 SnowCluster 2015 The South Pole Telescope Collaboration Funded By: Funded by: 2 The South Pole Telescope (SPT)!
WFIRST and JWST synergies in the study of First Light. M. Stiavelli STScI, Baltimore
WFIRST and JWST synergies in the study of First Light M. Stiavelli STScI, Baltimore 1 WFIRST and JWST synergies in the study of First Light Plan: - Detecting the First Stars WFIRST-AFTA as an object finder
Exploring the Depths of the Universe
Exploring the Depths of the Universe Jennifer Lotz Hubble Science Briefing Jan. 16, 2014 Hubble is now observing galaxies 97% of the way back to the Big Bang, during the first 500 million years 2 Challenge:
Evidence for/constraints on dark matter in galaxies and clusters
Nov 11, 2015 Evidence for/constraints on dark matter in galaxies and clusters HW#9 is due; please hand in your summaries; then you get to talk (I have slides of the different facilities/telescopes. HW#10
Gravitational Lensing. Einstein deflection angle Lens equation, magnification Galaxy lenses Cluster lenses Weak lensing Time delays in lenses
Gravitational Lensing Einstein deflection angle Lens equation, magnification Galaxy lenses Cluster lenses Weak lensing Time delays in lenses Einstein's deflection angle In General Relativity, light is
Status of QSO absorption cosmology
Status of QSO absorption cosmology Mat Pieri LAM QSO absorption cosmology team Lead: Mat Pieri DESI absorption cosmology WG chair DESI Science Committee member WEAVE QSO survey lead Isabelle Paris BOSS
The Dark Matter - Galaxy Connection: HOD Estimation from Large Volume Hydrodynamical Simulations
The Dark Matter - Galaxy Connection: HOD Estimation from Large Volume Hydrodynamical Simulations J. CASADO GÓMEZ (UAM) R. DOMÍNGUEZ-TENREIRO J. OÑORBE (UCA/Irvine) F. MARTINEZ - SERRANO (UMH) A. KNEBE
EFFECT OF MERGERS ON THE SIZE EVOLUTION OF EARLY-TYPE GALAXIES
EFFECT OF MERGERS ON THE SIZE EVOLUTION OF EARLY-TYPE GALAXIES CARLO NIPOTI BOLOGNA UNIVERSITY Getting a Grip on Galaxy Girths, Tokyo, February 2015 NGC 474(Credit: Duc Atlas3D) Dry and wet galaxy mergers
Synergies between and E-ELT
Synergies between and E-ELT Aprajita Verma & Isobel Hook 1) E- ELT Summary 2) E- ELT Project Status 3) Parameter space 4) Examples of scientific synergies The World s Biggest Eye on the Sky 39.3m diameter,
Galaxy Clusters in Stage 4 and Beyond
Galaxy Clusters in Stage 4 and Beyond (perturbation on a Cosmic Visions West Coast presentation) Adam Mantz (KIPAC) CMB-S4/Future Cosmic Surveys September 21, 2016 Galaxy clusters: what? Galaxy cluster:
Constraints on dark matter annihilation cross section with the Fornax cluster
DM Workshop@UT Austin May 7, 2012 Constraints on dark matter annihilation cross section with the Fornax cluster Shin ichiro Ando University of Amsterdam Ando & Nagai, arxiv:1201.0753 [astro-ph.he] Galaxy
The gas-galaxy-halo connection
The gas-galaxy-halo connection Jean Coupon (University of Geneva) Collaborators: Miriam Ramos, Dominique Eckert, Stefano Ettori, Mauro Sereno, Keiichi Umetsu, Sotiria Fotopoulou, Stéphane Paltani, and
Keck/Subaru Exchange Program Subaru Users Meeting January 20, 2011
Keck/Subaru Exchange Program Subaru Users Meeting January 20, 2011 Taft Armandroff, Director W. M. Keck Observatory With science results from: Drew Newman and Richard Ellis, Caltech A. Romanowsky, J. Strader,
Euclid theory working group ~ Marseille presentation
Euclid theory working group ~ Marseille presentation Task of theory WG: provide vision for the future direction of mission forecast which will be the main questions in 5+ years, set up framework to answer
Deciphering the origin of globular clusters near the Galactic bulge + more. Masashi Chiba (Tohoku University)
Deciphering the origin of globular clusters near the Galactic bulge + more Masashi Chiba (Tohoku University) ULTIMATE-Subaru in Galactic Archaeology Resolved stars provide important information on galaxy
THE SUNYAEV-ZELDOVICH EFFECT
THE SUNYAEV-ZELDOVICH EFFECT Etienne Pointecouteau IRAP (Toulouse, France) THE SUNYAEV-ZELDOVICH EFFECT Inverse Compton scattering of CMB photons by intracluster electrons R. A. Sunyaev Ya. B. Zeldovich
GAMA-SIGMA: Exploring Galaxy Structure Through Modelling
GAMA-SIGMA: Exploring Galaxy Structure Through Modelling University of St Andrews / ICRAR (UWA) Science Goals Do galaxies form in two phases: bulge disk? Are ellipticals and bulges essentially the same?