Sampling Artifact in Volume Weighted Velocity Measurement and Halo Velocity Bias Yi Zheng 郑逸 Supervisor: Pengjie Zhang Y. Zheng, P. Zhang, Y. Jing, W.

Slides:

Advertisements

Similar presentations

Lagrangian Perturbation Theory : 3 rd order solutions for general dark energy models Seokcheon Lee ( ) Korea Institute for Advanced Study ( ) Feb. 12 th.

Advertisements

The scaling of LWFA in the ultra-relativistic blowout regime: Generation of Gev to TeV monoenergetic electron beams W.Lu, M.Tzoufras, F.S.Tsung, C. Joshi,

Tidal Alignments & Large Scale Structure Christopher Hirata Edinburgh, 22 Jul 2010 C.H., MNRAS 399:1074 (2009) – Redshift space distortions Elisabeth Krause.

The Physics of Large Scale Structure and New Results from the Sloan Digital Sky Survey Beth Reid ICC Barcelona arXiv: arXiv: * Colloborators:

Important slides (Cosmological group at KASI)

Rotation of Cosmic Voids (Lee & Park 2006, ApJ in press, astro-ph/ ) Jounghun Lee & Deaseong Park (Seoul National University)

Galaxy and Mass Power Spectra Shaun Cole ICC, University of Durham Main Contributors: Ariel Sanchez (Cordoba) Steve Wilkins (Cambridge) Imperial College.

Non-linear matter power spectrum to 1% accuracy between dynamical dark energy models Matt Francis University of Sydney Geraint Lewis (University of Sydney)

An Analytic Model for the Tidal Effect on Cosmic Voids Jounghun Lee & Daeseong Park Seoul National University Lee & Park 2006, ApJ, 652, 1 Park & Lee 2006,

Christian Wagner - September Potsdam Nonlinear Power Spectrum Emulator Christian Wagner in collaboration with Katrin Heitmann, Salman Habib,

The clustering of galaxy groups in the 2dFGRS (2PIGG) The clustering of 2PIGGs Project zero: CDM predictions and parameter constraints Project one, two,..:

Quasar Clustering (A Dabbler’s Perspective) CCAPP AGN Workshop: Oct. 2, 2007 Adam Lidz (CfA) Thanks to: Phil Hopkins, Lars Hernquist, T.J. Cox, and others….

Modeling the 3-point correlation function Felipe Marin Department of Astronomy & Astrophysics University of Chicago arXiv: Felipe Marin Department.

Angular clustering and halo occupation properties of COSMOS galaxies Cristiano Porciani.

Battle of the Mass Estimators (Based on Bahcall and Tremaine, 1981) Nick Cowan UW Astronomy January 25, 2005.

Lens Galaxy Environments Neal Dalal (IAS), Casey R. Watson (Ohio State) astro-ph/ Who cares? 2.What to do 3.Results 4.Problems! 5.The future.

14 December 2006 Dark Matter Haloes in the Cosmic Web Cristiano Porciani (ETH Zurich) with OLIVER HAHN, Marcella Carollo, Avishai Dekel.

Cosmological constraints from models of galaxy clustering Abstract Given a dark matter distribution, the halo occupation distribution (HOD) provides a.

The Clipped Power Spectrum Fergus Simpson University of Edinburgh FS, James, Heavens, Heymans (2011 PRL) FS, Heavens, Heymans (arXiv: )

Tomo-gravity Yin ZhangMatthew Roughan Nick DuffieldAlbert Greenberg “A Northern NJ Research Lab” ACM.

The Theory/Observation connection lecture 3 the (non-linear) growth of structure Will Percival The University of Portsmouth.

Smoothed Particle Hydrodynamics

Galaxy bias with Gaussian/non- Gaussian initial condition: a pedagogical introduction Donghui Jeong Texas Cosmology Center The University of Texas at Austin.

Pengjie Zhang Shanghai Jiao Tong University The large scale structure and its cosmological applications The Sunyaev Zel’dovich effect (2001-present) –

Dark Matter and Dark Energy from the solution of the strong CP problem Roberto Mainini, L. Colombo & S.A. Bonometto Universita’ di Milano Bicocca Mainini.

What can we learn from galaxy clustering? David Weinberg, Ohio State University Berlind & Weinberg 2002, ApJ, 575, 587 Zheng, Tinker, Weinberg, & Berlind.

Galactic Helium-to-Metals enrichment ratio from the analysis of local main sequence stars observed by HIPPARCOS 52° Congresso SAIt – Teramo 2008 * Università.

Intrinsic ellipticity correlation of luminous red galaxies and misalignment with their host dark matter halos The 8 th Sino – German workshop Teppei O.

Cosmological studies with Weak Lensing Peak statistics Zuhui Fan Dept. of Astronomy, Peking University.

Clustering in the Sloan Digital Sky Survey Bob Nichol (ICG, Portsmouth) Many SDSS Colleagues.

The dark universe SFB – Transregio Bonn – Munich - Heidelberg.

Measuring dark energy from galaxy surveys Carlton Baugh Durham University London 21 st March 2012.

David Weinberg, Ohio State University Dept. of Astronomy and CCAPP The Cosmological Content of Galaxy Redshift Surveys or Why are FoMs all over the map?

The coordinated growth of stars, haloes and large-scale structure since z=1 Michael Balogh Department of Physics and Astronomy University of Waterloo.

0 The numerical action method: prospects and problems Steven Phelps, the Technion, Haifa With: Adi Nusser, Vincent Desjacques, Technion January 2006.

Some progresses on peculiar velocity cosmology Zheng Yi ( 郑逸 ) Collaborators: Pengjie Zhang, Yipeng Jing, Weipeng Lin, Jun Pan, Yong-Seon Song P. Zhang,

Various Mostly Lagrangian Things Mark Neyrinck Johns Hopkins University Collaborators: Bridget Falck, Miguel Aragón-Calvo, Xin Wang, Donghui Jeong, Alex.

Baryonic signature in the large-scale clustering of SDSS quasars Kazuhiro Yahata Dept. of Phys., University of Tokyo. Issha Kayo, Yasushi Suto, Matsubara.

How accurately do N body simulations reproduce the clustering of CDM? Michael Joyce LPNHE, Université Paris VI Work in collaboration with: T. Baertschiger.

23 Sep The Feasibility of Constraining Dark Energy Using LAMOST Redshift Survey L.Sun Peking Univ./ CPPM.

Probing cosmic structure formation in the wavelet representation Li-Zhi Fang University of Arizona IPAM, November 10, 2004.

KIAS, Nov 5, 2014 Measuring the Cosmic Shear in Fourier Space Jun Zhang ( 张骏 ) (Shanghai Jiao Tong University) Collaborators: Eiichiro Komatsu (MPA), Nobuhiko.

6dF Workshop April Sydney Cosmological Parameters from 6dF and 2MRS Anaïs Rassat (University College London) 6dF workshop, AAO/Sydney,

Zheng Dept. of Astronomy, Ohio State University David Weinberg (Advisor, Ohio State) Andreas Berlind (NYU) Josh Frieman (Chicago) Jeremy Tinker (Ohio State)

Xiaohu Yang (SJTU/SHAO) With: H. Wang, H.J. Mo, Y.P. Jing, F.C van den Bosch, W.P. Lin, D. Tweed… , KIAS Exploring the Local Universe with re-

J. Jasche, Bayesian LSS Inference Jens Jasche La Thuile, 11 March 2012 Bayesian Large Scale Structure inference.

Latest Results from LSS & BAO Observations Will Percival University of Portsmouth StSci Spring Symposium: A Decade of Dark Energy, May 7 th 2008.

Peculiar velocity decomposition, redshift distortion and velocity reconstruction in redshift surveys Zheng, Yi 郑逸 Shanghai Astronomical Observatory P.

Eyal Neistein Dec 2012 MS workshop Modeling galaxy clustering and weak gravitational lensing with the Millennium simulation Eyal Neistein TMoX group, MPE.

M. Omang, S. Børve, and J. Trulsen

Probing Cosmology with Weak Lensing Effects Zuhui Fan Dept. of Astronomy, Peking University.

Holographic Dark Energy and Anthropic Principle Qing-Guo Huang Interdisciplinary Center of Theoretical Studies CAS

1 Baryon Acoustic Oscillations Prospects of Measuring Dark Energy Equation of State with LAMOST Xuelei Chen ( 陳學雷 ) National Astronomical Observatory of.

Taka Matsubara (Nagoya Univ.)

Feasibility of detecting dark energy using bispectrum Yipeng Jing Shanghai Astronomical Observatory Hong Guo and YPJ, in preparation.

Initial conditions for N-body simulations Hans A. Winther ITA, University of Oslo.

Carlos Hernández-Monteagudo CE F CA 1 CENTRO DE ESTUDIOS DE FÍSICA DEL COSMOS DE ARAGÓN (CE F CA) J-PAS 10th Collaboration Meeting March 11th 2015 Cosmology.

Xi An, May 20, 2014 Measuring the Cosmic Shear in Fourier Space Jun Zhang ( 张骏 ) (Shanghai Jiao Tong University) Collaborators: Eiichiro Komatsu (MPA),

Spherical Collapse and the Mass Function – Chameleon Dark Energy Stephen Appleby, APCTP-TUS dark energy workshop 5 th June, 2014 M. Kopp, S.A.A, I. Achitouv,

Some bonus cosmological applications of BigBOSS ZHANG, Pengjie Shanghai Astronomical Observatory BigBOSS collaboration meeting, Paris, 2012 Refer to related.

3D Matter and Halo density fields with Standard Perturbation Theory and local bias Nina Roth BCTP Workshop Bad Honnef October 4 th 2010.

Gamma-ray emission from warm WIMP annihilation Qiang Yuan Institute of High Energy Physics Collaborated with Xiaojun Bi, Yixian Cao, Jie Liu, Liang Gao,

Clustering and environments of dark matter halos

Dept of Physics and Astronomy University of Glasgow, UK

Accuracy of Cosmological N-body Simulations

An Analytic Approach to Assess Galaxy Projection Along A Line of Sight

Gamma-ray emission from warm WIMP annihilation

Intrinsic Alignment of Galaxies and Weak Lensing Cluster Surveys Zuhui Fan Dept. of Astronomy, Peking University.

The impact of non-linear evolution of the cosmological matter power spectrum on the measurement of neutrino masses ROE-JSPS workshop Edinburgh.

Fig. 1 Fluctuation-induced dynamic response patterns.

Presentation transcript:

Sampling Artifact in Volume Weighted Velocity Measurement and Halo Velocity Bias Yi Zheng 郑逸 Supervisor: Pengjie Zhang Y. Zheng, P. Zhang, Y. Jing, W. Lin, and J. Pan, Phys. Rev. D 88, (2013), P. Zhang, Y. Zheng, Y. Jing, (2014, paperSI), in preparation Y. Zheng, P. Zhang, Y. Jing, (2014, paperSII), in preparation Y. Zheng, P. Zhang, Y. Jing, (2014, paperB), in preparation

Outline We want to measure halo velocity bias, volume- weighted. (Y. Zheng, P. Zhang, Y. Jing, (2014, paperB), in preparation) We find non-negligible systematic error in volume- weighted velocity measurement! ( ; Y. Zheng, P. Zhang, Y. Jing, (2014, paperB), in preparation) We try to understand this systematic error theoretically and by simulation. (P. Zhang, Y. Zheng, Y. Jing, (2014, paperSI), in preparation; Y. Zheng, P. Zhang, Y. Jing, (2014, paperSII), in preparation) Now we have achieved several percent level accuracy, but not enough, O(1%)! (paperSII)

Motivation: Why halo velocity bias matters? In linear theory: Desjacques & Sheth Weak equivalence principle Environmentally dependent evolution halos galaxies Lagrangian velocity bias: non-negligible! Desjacques , Desjacques & Sheth Relation between Lagrangian and Eularian space: complicated! e.g. Colberg et al. MNRAS 313, 229 Eularian velocity bias: ?

How to measure the halo velocity bias? Power spectrum of volume weighted velocity of dark matter particles Power spectrum of volume weighted velocity of dark matter halos ‘volume-weighted’: For a given grid point, we assign the velocity of its nearest dark matter particle/halo/galaxy to it. ‘volume-weighted’: For a given grid point, we assign the velocity of its nearest dark matter particle/halo/galaxy to it. Nearest Particle (NP) method: Simulation speculation:

An example of sys. Err.: 128^3 grids 512^3 grids Non-neglectable >10% systematic errors! YZ et al. paperB, in preparation preliminary

More clues: 1. grid size induced sys. Err. Fair comparison demands the same grid numbers for dark matter particles and halos. Velocity decomposition, see PJZ et al

More clues: 2. number density induced sys. Err. Velocity decomposition, see PJZ et al Fair comparison demands the same number density for dark matter particles and halos or we quantify and correct the numerical artifacts.

Systematic errors of NP method: theory For dark matter velocity field, we could work in the limit of But for halos, the number density is low and fixed. So we have to work in the case of This distinguishes our work from existing ones. PJZ et al. paperSI, in preparation

Systematic errors of NP method: theory More details see PJZ et al. paperSI, in preparation 1. Shot noise correction: 2. Sampling effect correction (first order): Directly measurable!

Systematic errors of NP method: simulation 2. Sampling effect correction (first order): Already several percent accuracy! Halo set A1 preliminary

Discussion Other velocity assignment methods suffer from this systematic error too. We need higher order correction to archive O(1%) systematic errors ?