neutrino physics from the cmb large scale structure report
play

Neutrino Physics from the CMB & Large Scale Structure - Report - PowerPoint PPT Presentation

Sep 24, 2022 •137 likes •728 views

Neutrino Physics from the CMB & Large Scale Structure - Report - Topical Conveners: K.N. Abazajian, J.E. Carlstrom, A.T. Lee Contributors: K.N. Abazajian, B.A. Benson, J. Bock, J. Borrill, J.E. Carlstrom, C.L. Chang, S. Church, A. Cooray,

  1. Neutrino Physics from the CMB & Large Scale Structure - Report - Topical Conveners: K.N. Abazajian, J.E. Carlstrom, A.T. Lee Contributors: K.N. Abazajian, B.A. Benson, J. Bock, J. Borrill, J.E. Carlstrom, C.L. Chang, S. Church, A. Cooray, T.M. Crawford, K.S. Dawson, S. Das, S. Dodelson, J. Errard, S. Hanany, W.L. Holzapfel, K. Honscheid, M. Kamionkowski, R. Keisler, L. Knox, J. Kovac, C.-L. Kuo, C. Lawrence, A.T. Lee, E. Linder, P. Lubin, A. Miller, M.D. Niemack, C. Pryke, C. Reichardt, U. Seljak, E. Silverstein, A. Slosar, R. Stompor, A. Vieregg, E.J. Wollack, W.L.K. Wu, K.W. Yoon, and O. Zahn Paper: http://is.gd/AnSecR [arXiv on Friday (?)] Cosmic Frontier Snowmass Community Summer Study 2013 August 1, 2013

  2. The Cosmological Matter Power Spectrum Inflation: ? Perturbations enter horizon: Matter Domination Radiation Domination [ δΦ mat const] [ δΦ rad decays] horizon size P(k) → k →

  3. How does probe neutrinos? (Assuming thermal equilibrium)

  4. How does probe neutrinos? (Assuming thermal equilibrium) P(k) → k →

  5. How does probe neutrinos? (Assuming thermal equilibrium) Radiation Matter Domination Domination P(k) → k →

  6. How does probe neutrinos? (Assuming thermal equilibrium) Radiation Matter Domination Domination P(k) → k →

  7. How does probe neutrinos? (Assuming thermal equilibrium) Radiation Matter Domination Domination P(k) → Is this a coincidence? k →

  8. How does probe neutrinos? (Assuming thermal equilibrium) � Radiation Matter Domination ρ ν = m i n ν i Domination � m ν i P(k) → Ω ν ≈ 93 h 2 eV E 2 = p 2 + m 2 Is this a coincidence? k →

  9. Distinguishing Features in the Power Spectrum Σ m ν i = 0 . 14 eV P(k) → Σ m ν i = 1 . 4 eV Lesgourgues & Pastor (2006) k → 1. Shape Information: Galaxy Surveys (Future: CMB lensing, Weak Lensing) 2. Relative Amplitude Information: ∆ P ( k ) = − 8 Ω ν CMB plus Lyman-alpha Forest, Galaxy Bias P ( k ) Ω m

  10. Distinguishing Features in the Power Spectrum Σ m ν i = 0 . 14 eV P(k) → Galaxy Surveys Σ m ν i = 1 . 4 eV Lesgourgues & Pastor (2006) k → 1. Shape Information: Galaxy Surveys (Future: CMB lensing, Weak Lensing) 2. Relative Amplitude Information: ∆ P ( k ) = − 8 Ω ν CMB plus Lyman-alpha Forest, Galaxy Bias P ( k ) Ω m

  11. Distinguishing Features in the Power Spectrum Σ m ν i = 0 . 14 eV P(k) → Galaxy Surveys Σ m ν i = 1 . 4 eV Relative Amplitude:CMB+Lya Lesgourgues & Pastor (2006) k → 1. Shape Information: Galaxy Surveys (Future: CMB lensing, Weak Lensing) 2. Relative Amplitude Information: ∆ P ( k ) = − 8 Ω ν CMB plus Lyman-alpha Forest, Galaxy Bias P ( k ) Ω m

  12. The Primordial Spectrum: Precision Determination at Large Scales P(k) → k → P ( k ) = Ak n Planck 1-Year + WMAP Pol.: (Planck Collab. 2013) A = 2 . 196 +0 . 051 (3%) − 0 . 060 n = 0 . 9603 ± 0 . 0073 (0 . 8%)

  13. Measuring P ( k ): from largest to smallest scales CMB SDSS Ly- α

  14. Upcoming High-Precision Era: Relative Change to P ( k )

  15. Ω m & Other Parameter Degeneracy Ω m

  16. Cosmological Matter Power Spectrum & CMB Constraints on N eff For LSS: Perturbations enter horizon at M/R equality Matter Domination Radiation Domination [ δΦ mat const] [ δΦ rad decays] horizon size P(k) → k → For BAO: Extra radiation changes expansion rate from perturbation evolution through baryon decoupling

  17. & N eff [Dodelson (SLAC Cosmic Frontiers)]

  18. Summary of Cosmological N eff Measures • SDSS BOSS Galaxy Clustering + BAO + WMAP 7 + SNe + H 0 (Zhao et. al 2012) N e ff = 4 . 308 ± 0 . 794 WMAP7 68% CL • SPT + WMAP 7 + H 0 (Hou et al. 2012) ... N e ff = 3 . 71 ± 0 . 35 • ACT + WMAP 7 + BAO + H 0 (Sievers et. al 2013) N e ff = 2 . 78 ± 0 . 55 • WMAP 9 + eCMB + BAO + H 0 (Hinshaw et al. 2012 v2 ) WMAP9 N e ff = 3 . 84 ± 0 . 40 Planck • Planck + high-l CMB + WMAP P + BAO (Planck Collab. 2013) N e ff = 3 . 30 ± 0 . 27

  19. Estimating Upcoming Cosmological Neutrino Mass Constraints ∆ P ( k ) ≈ 1% ≈ − 8 Ω ν Hu, Eisenstein & Tegmark 1998 P ( k ) Ω m

  20. Estimating Upcoming Cosmological Neutrino Mass Constraints ∆ P ( k ) ≈ 1% ≈ − 8 Ω ν Hu, Eisenstein & Tegmark 1998 P ( k ) Ω m � m ν i Ω ν ≈ 93 h 2 eV

  21. Estimating Upcoming Cosmological Neutrino Mass Constraints ∆ P ( k ) ≈ 1% ≈ − 8 Ω ν Hu, Eisenstein & Tegmark 1998 P ( k ) Ω m � m ν i Ω ν ≈ 93 h 2 eV ⇒ m ν . (1% / 8) × Ω m (93 h 2 eV) =

  22. Estimating Upcoming Cosmological Neutrino Mass Constraints ∆ P ( k ) ≈ 1% ≈ − 8 Ω ν Hu, Eisenstein & Tegmark 1998 P ( k ) Ω m � m ν i Ω ν ≈ 93 h 2 eV ⇒ m ν . (1% / 8) × Ω m (93 h 2 eV) = ⇒ m ν . 20 meV =

  23. Estimating Upcoming Cosmological Neutrino Mass Constraints ∆ P ( k ) ≈ 1% ≈ − 8 Ω ν Hu, Eisenstein & Tegmark 1998 P ( k ) Ω m � m ν i Ω ν ≈ 93 h 2 eV ⇒ m ν . (1% / 8) × Ω m (93 h 2 eV) = ⇒ m ν . 20 meV = Kaplinghat et al PRL 2003 (CMB WL) Wang et al PRL 2005 (WL Clusters) De Bernardis et al. 2009 (Opt. WL) Joudaki & Kaplinghat 2011 (LSST) Basse et al. 2013 (Euclid) CF5 Neutrino Report 2013

  24. Lensing of the CMB Hu & Okamoto 2001

  25. Lensing of the CMB Hu & Okamoto 2001

  26. Lensing of the CMB • Higher-order statistics in CMB T maps can reconstruct the lensing potential. (detected by SPT, ACT, Planck) Hu & Okamoto 2001

  27. Lensing of the CMB • Higher-order statistics in CMB T maps can reconstruct the lensing potential. (detected by SPT, ACT, Planck) • Lensing also mixes polarization E modes to B modes, providing more information. (detected by SPT) Hu & Okamoto 2001

  28. Lensing of the CMB • Higher-order statistics in CMB T maps can reconstruct the lensing potential. (detected by SPT, ACT, Planck) • Lensing also mixes polarization E modes to B modes, providing more information. (detected by SPT) • Detailed, high signal-to- noise measurements of arcminute polarization can therefore be used to reconstruct the lensing Hu & Okamoto 2001 potential C L φφ

  29. Lensing Potential Power: Relative Change over an Integrated P ( k )

  30. Σ m ν : The March of Time

  31. Σ m ν : The March of Time 2 (95% CL) m ν [eV] 1 X

  32. Σ m ν : The March of Time 2 (95% CL) m ν [eV] 1 X

  33. Σ m ν : The March of Time 2 (95% CL) m ν [eV] 1 X 2003

  34. Σ m ν : The March of Time 2 (95% CL) 2dFGRS m ν [eV] 1 X 2003

  35. Σ m ν : The March of Time 2 (95% CL) 2dFGRS m ν [eV] 1 X 2003 2006

  36. (95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time

  37. (95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS

  38. (95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010

  39. (95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone

  40. (95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone 2012

  41. (95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone SDSS BOSS + WMAP 7 2012

  42. (95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone SDSS BOSS + WMAP 7 2012 WMAP 9 + BAO

  43. (95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone SDSS BOSS + WMAP 7 2012 WMAP 9 + BAO 2013

  44. (95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone SDSS BOSS + WMAP 7 2012 WMAP 9 + BAO ACT + WMAP 7 + BAO 2013

  45. (95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone SDSS BOSS + WMAP 7 2012 WMAP 9 + BAO ACT + WMAP 7 + BAO 2013 Planck + BAO

  46. (95% CL) X m ν [eV] 1 2 Oscillations 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone SDSS BOSS + WMAP 7 2012 WMAP 9 + BAO ACT + WMAP 7 + BAO 2013 Planck + BAO

  47. Cosmological & Laboratory Complementarity

  48. CMB & LSS Complementarity: Parameter Degeneracy

  49. Stage IV CMB + DESI: Σ m ν vs. N eff

  50. Forecast Sensitivities σ ( N eff ) σ ( Σ m ν ) CF5 Neutrino Paper

  51. Forecast Sensitivities σ ( N eff ) σ ( Σ m ν ) CF5 Neutrino Paper

  52. Neutrino Mass from Cosmology: What would break if cosmology and neutrino experiment disagree? P(k) → 1. Primordial power spectrum P ( k ) is a simple power law k → 2. No other prevalent “non-vanilla” cosmological parameters and physics: w , N eff , modified gravity...

  53. Summary

Download Presentation
Download Policy: The content available on the website is offered to you 'AS IS' for your personal information and use only. It cannot be commercialized, licensed, or distributed on other websites without prior consent from the author. To download a presentation, simply click this link. If you encounter any difficulties during the download process, it's possible that the publisher has removed the file from their server.

Recommend

Neutrino Masses from TeV Scale New Physics -- Tests of Neutrino Masses at the LHC Mu-Chun Chen,

Neutrino Masses from TeV Scale New Physics -- Tests of Neutrino Masses at the LHC Mu-Chun Chen,

Neutrino Masses from TeV Scale New Physics -- Tests of Neutrino Masses at the LHC Mu-Chun Chen, University of California at Irvine GGI Whats Nu?, June 26, 2012 Theoretical Challenges (i) Absolute mass scale: Why m << m u,d,e ?

543 views • 29 slides
Large-Scale Cryogenic Detectors, and Sensi5vity to Solar Physics

Large-Scale Cryogenic Detectors, and Sensi5vity to Solar Physics

Large-Scale Cryogenic Detectors, and Sensi5vity to Solar Physics Dan McKinsey Yale University Future Solar Neutrino Detector at JinPing Workshop Lawrence

461 views • 20 slides
Fundamental Physics and Large-scale Structure II: Hobby-Eberly Telescope Dark Energy Experiment

Fundamental Physics and Large-scale Structure II: Hobby-Eberly Telescope Dark Energy Experiment

Fundamental Physics and Large-scale Structure II: Hobby-Eberly Telescope Dark Energy Experiment Eiichiro Komatsu (Texas Cosmology Center, UT Austin) on behalf of HETDEX collaboration Coming Opportunities in Physical Cosmology, January 27,

870 views • 60 slides
Low Scale Testable Leptogenesis Jacobo Lpez-Pavn Neutrino Physics at the High Energy

Low Scale Testable Leptogenesis Jacobo Lpez-Pavn Neutrino Physics at the High Energy

Low Scale Testable Leptogenesis Jacobo Lpez-Pavn Neutrino Physics at the High Energy Frontier ACFI, 18-20 July 2017 Outline Minimal Seesaw Model. New Physics Scale. Testable Leptogenesis. Hernandez, Kekic, JLP, Racker, Rius

1.01k views • 73 slides
Physics with Precision Time Structure in On Axis Neutrino Beams Phys. Rev. D 100, 032008. 26

Physics with Precision Time Structure in On Axis Neutrino Beams Phys. Rev. D 100, 032008. 26

Physics with Precision Time Structure in On Axis Neutrino Beams Phys. Rev. D 100, 032008. 26 August 2019. https://doi.org/10.1103/PhysRevD.100.032008 1 CPAD 2019, DEC 9 2019 Accelerator neutrino physics Kendall Mahn et. al. arXiv: 1803.08848v1

346 views • 18 slides
Solar Neutrino and Solar Neutrino and Neutrino Physics in Brazil Neutrino Physics in Brazil

Solar Neutrino and Solar Neutrino and Neutrino Physics in Brazil Neutrino Physics in Brazil

Solar Neutrino and Solar Neutrino and Neutrino Physics in Brazil Neutrino Physics in Brazil Pedro Cunha de Holanda DRCC - IFGW UNICAMP Florence, 2012 A little bit of history A little bit of history A little bit of history A little bit of

774 views • 41 slides
Current results of Neutrino-4 experiment with full-scale detector Collaboration Neutrino-4: 1.

Current results of Neutrino-4 experiment with full-scale detector Collaboration Neutrino-4: 1.

Current results of Neutrino-4 experiment with full-scale detector Collaboration Neutrino-4: 1. NRC KI Petersburg Nuclear Physics Institute, Gatchina, 2. NRC Kurchatov institute, Moscow, 3. JSC SSC RIAR, Dimitrovgrad, Russia

258 views • 23 slides
Cosmic Calibration Katrin Heitmann Statistical Challenges for Large-Scale Structure in the Era of

Cosmic Calibration Katrin Heitmann Statistical Challenges for Large-Scale Structure in the Era of

Cosmic Calibration Katrin Heitmann Statistical Challenges for Large-Scale Structure in the Era of LSST Oxford , April 18, 2018 Cosmological Constraints Large Scale Simulations Cosmic Emulation Cosmic Emulators Large Synoptic Survey Telescope

944 views • 32 slides
The Formation of Vortical Motion in Cosmic Large Scale Structure Ruth Durrer Universit e de

The Formation of Vortical Motion in Cosmic Large Scale Structure Ruth Durrer Universit e de

The Formation of Vortical Motion in Cosmic Large Scale Structure Ruth Durrer Universit e de Gen` eve D epartment de Physique Th eorique and Center for Astroparticle Physics Gravity and Cosmology Workshop, Kyoto 2018 Ruth Durrer

539 views • 32 slides
Probing the large-scale structure Probing the large-scale structure with the largest photometric

Probing the large-scale structure Probing the large-scale structure with the largest photometric

Probing the large-scale structure Probing the large-scale structure with the largest photometric catalogs: with the largest photometric catalogs: today and tomorrow today and tomorrow Maciej Bilicki Leiden Observatory, Leiden University, the

1.8k views • 25 slides
Outline Review main objectives of this workshop Physics topics Neutrino physics :

Outline Review main objectives of this workshop Physics topics Neutrino physics :

Outline Review main objectives of this workshop Physics topics Neutrino physics : neutrino oscillations and masses Neutrino astronomy and astrophysics: detection of new astrophysical bodies and neutrino producing processes

543 views • 50 slides
New Physics at the TeV Scale? New Physics at the TeV Scale? A Supersymmetric and

New Physics at the TeV Scale? New Physics at the TeV Scale? A Supersymmetric and

FFD SEMINAR 2003 New Physics at the TeV Scale? New Physics at the TeV Scale? A Supersymmetric and Extra-dimensional talk Peter Skands Theoretical High Energy Physics New Physics at the TeV Scale, P . Skands p.1/47 Overview New

830 views • 72 slides
- Neutrino physics

- Neutrino physics

- Neutrino physics using quantum coherence - M. Yoshimura Okayama University, Japan Outline of this talk Introduction: remaining important questions in neutrino

823 views • 42 slides
STRUCTURE, MOTIONS AND COSMOLOGY FROM THE TAIPAN SURVEY Matthew Colless Large Scale Structure

STRUCTURE, MOTIONS AND COSMOLOGY FROM THE TAIPAN SURVEY Matthew Colless Large Scale Structure

STRUCTURE, MOTIONS AND COSMOLOGY FROM THE TAIPAN SURVEY Matthew Colless Large Scale Structure and Galaxy Flows Quy Nhon, 4 July 2016 Why measure H 0 ? (with emphasis on the 0) q H 0 , the local (i.e. zero-redshift) expansion rate, is a

739 views • 31 slides
Models of Neutrino Masses in View of the Large 13 Discovery Mu-Chun Chen, University of

Models of Neutrino Masses in View of the Large 13 Discovery Mu-Chun Chen, University of

Models of Neutrino Masses in View of the Large 13 Discovery Mu-Chun Chen, University of California at Irvine Flavor Physics and CP Violation (FPCP2013), Bzios, Brazil, May 19-24, 2013 Where Do We Stand? Exciting Time in Physics:

735 views • 51 slides
Dark Energy with Large Scale Structure Beth Reid Cosmology Data Science Fellow Berkeley Center

Dark Energy with Large Scale Structure Beth Reid Cosmology Data Science Fellow Berkeley Center

Dark Energy with Large Scale Structure Beth Reid Cosmology Data Science Fellow Berkeley Center for Cosmological Physics Lawrence Berkeley National Lab Sloan Digital Sky Survey Apache Point, New Mexico The Observable Universe SDSS-III Baryon

121 views • 10 slides
SEMANTIC IMAGE SEGMENTATION WITH DEEP CONVOLUTIONAL NETS AND FULLY CONNECTED CRFS Paper by Chen,

SEMANTIC IMAGE SEGMENTATION WITH DEEP CONVOLUTIONAL NETS AND FULLY CONNECTED CRFS Paper by Chen,

SEMANTIC IMAGE SEGMENTATION WITH DEEP CONVOLUTIONAL NETS AND FULLY CONNECTED CRFS Paper by Chen, Papandreou, Kokkinos, Murphy, Yuille Slides by Josh Kelle (with graphics from the paper) Semantic Segmentation Goal: Partition the image into

520 views • 22 slides
Radiative Forcing Efficiency of a Forest Fire Smoke Plume at the Surface and TOA John A. Augustine

Radiative Forcing Efficiency of a Forest Fire Smoke Plume at the Surface and TOA John A. Augustine

Radiative Forcing Efficiency of a Forest Fire Smoke Plume at the Surface and TOA John A. Augustine 1 , Robert S. Stone 1,2 , David Rutan 3 , and Ellsworth G. Dutton 1 1 Earth System Research Laboratory, Global Monitoring Division, Boulder, CO 2

649 views • 26 slides
Battle of the Accelerator Stars Xipeng Shen The College of William and Mary & MIT Top500

Battle of the Accelerator Stars Xipeng Shen The College of William and Mary & MIT Top500

Battle of the Accelerator Stars Xipeng Shen The College of William and Mary & MIT Top500 6/2012 source: top500.org 2 Xipeng Shen xshen@cs.wm.edu Green500 (6/2012) What is the role of accelerator? source: green500.org 3 Xipeng

892 views • 14 slides
QTRAN: Learning to Factorize with Transformation for Cooperative Multi-Agent Reinforcement

QTRAN: Learning to Factorize with Transformation for Cooperative Multi-Agent Reinforcement

QTRAN: Learning to Factorize with Transformation for Cooperative Multi-Agent Reinforcement Learning Kyunghwan Son , Daewoo Kim, Wan Ju Kang, David Hostallero, Yung Yi School of Electrical Engineering, KAIST Cooperative Multi-Agent Reinforcement

662 views • 8 slides
R. Kelly Crace, Ph.D. R. Kelly Crace, Ph.D. College of William & Mary College of William

R. Kelly Crace, Ph.D. R. Kelly Crace, Ph.D. College of William & Mary College of William

R. Kelly Crace, Ph.D. R. Kelly Crace, Ph.D. College of William & Mary College of William & Mary College of William & Mary College of William & Mary kelly.crace@wm.edu kelly.crace@wm.edu Perceived Evaluation Perceived

580 views • 10 slides
Sequence Labeling Markov Models Many information extraction tasks can be formulated as

Sequence Labeling Markov Models Many information extraction tasks can be formulated as

Information Extraction Information Extraction Sequence Labeling Markov Models Many information extraction tasks can be formulated as sequence A Markov Chain is a finite-state automaton that has a probability labeling tasks. Sequence

1.32k views • 3 slides
reduction without rule Randy Pollack and Masahiko Sato Version of September 7, 2017 Syntax

reduction without rule Randy Pollack and Masahiko Sato Version of September 7, 2017 Syntax

Syntax Operations on preterms reduction Generalized instantiation Reduction without reduction without rule Randy Pollack and Masahiko Sato Version of September 7, 2017 Syntax Operations on preterms reduction Generalized

433 views • 19 slides
Meet User Generated Lists Da Cao 1,2 , Liqiang Nie 3 , Xiangnan He 4 , Xiaochi Wei 5 , Shunzhi Zhu

Meet User Generated Lists Da Cao 1,2 , Liqiang Nie 3 , Xiangnan He 4 , Xiaochi Wei 5 , Shunzhi Zhu

Individual Items Meet User Generated Lists Da Cao 1,2 , Liqiang Nie 3 , Xiangnan He 4 , Xiaochi Wei 5 , Shunzhi Zhu 2 , Shunxiang Wu 1 , Tat-Seng Chua 4 1. Xiamen University; 2. Xiamen University of Technology; 3. Shandong University; 4. National

748 views • 27 slides

More recommend