Tom Theuns Institute for Computational Cosmology, Durham, UK Department of Physics, Antwerp, Belgium Munich 2005 Reionization And the thermal history of.

Slides:

Advertisements

Similar presentations

Halo Metallicity in NGC 891 An X-ray/UV Perspective Edmund Hodges-Kluck Joel Bregman University of Michigan.

Advertisements

Tom Theuns Institute for Computational Cosmology, Durham, UK Department of Physics, Antwerp, Belgium Groningen 2005 Reionization And the thermal history.

Challenges for the Standard Cosmology Tom Shanks Durham University.

Metals at Highish Redshift And Large Scale Structures From DLAs to Underdense Regions Patrick Petitjean Institut d’Astrophysique de Paris B. Aracil R.

Elements of observational cosmology Integalactic medium:  in clusters  between clusters.

First Stars, Quasars, and the Epoch of Reionization Jordi Miralda Escudé Institut de Ciències de l’Espai (IEEC-CSIC, ICREA), Barcelona. Instituto de Astrofísica.

21cm Lines and Dark Ages Naoshi Sugiyama Department of Physics and Astrophysics Nagoya University Furlanetto & Briggs astro-ph/ , Zaldarriaga et.

End of Cosmic Dark Ages: Observational Probes of Reionization History Xiaohui Fan University of Arizona New Views Conference, Dec 12, 2005 Collaborators:

Cosmological Reionization Nick Gnedin. Co-starring Gayler Harford Katharina Kohler Peter Shaver Mike Shull Massimo Ricotti.

Nick Gnedin. Epigraph Why is reionization interesting? I think the way to think about it is that it was the last time when most baryons got together and.

A hot topic: the 21cm line II Benedetta Ciardi MPA.

A New Constraint on the Intergalactic HeII Fraction at z~3 Matt McQuinn Einstein Fellows Symposium.

Theoretical work on Cosmology and Structure Formation Massimo Ricotti.

Simulating the ionisation and metal enrichment history of the Intergalactic Medium Tom Theuns Institute for Computational Cosmology, Durham, UK Department.

Simona Gallerani Constraining cosmic reionization models with QSOs, GRBs and LAEs observational data In collaboration with: A. Ferrara, X. Fan, T. Choudhury,

GRBs as Probes of First Light and the Reionization History of the Universe D. Q. Lamb (U. Chicago) Conference on First Light and Reionization Irvine, CA,

Probing dark matter clustering using the Lyman-  forest Pat McDonald (CITA) COSMO06, Sep. 28, 2006.

The metallicity of the intergalactic medium and its evolution Anthony Aguirre UCSC.

The physics of intergalactic gas Serena Bertone March 9 th 2009.

Large Scale Simulations of Reionization Garrelt Mellema Stockholm Observatory Collaborators: Ilian Iliev, Paul Shapiro, Marcelo Alvarez, Ue-Li Pen, Hugh.

Post GP-WMAP Reionization: the morning after We need quantitative measures of Epoch of reionization (Z reion ) Neutral fractions Volume fraction of ionized/neutral.

WMAP Implications for Reionization Columbia University The Davis Meeting on Cosmic Inflation March, 2003 Zoltán Haiman.

Galaxy Formation and Evolution Chris Brook Modulo 15 Room 509

Simona Gallerani Constraining reionization through quasar and gamma ray burst absorption spectra In collaboration with: T. Roy Choudhury, P. Dayal, X.

The Current State of Observational Cosmology JPO: Cochin(05/01/04)

Sources of Reionization Jordi Miralda Escudé Institut de Ciències de l’Espai (IEEC-CSIC, ICREA), Barcelona. Beijing,

Nick Gnedin (Once More About Reionization)

Lecture 5: Matter Dominated Universe: CMB Anisotropies and Large Scale Structure Today, matter is assembled into structures: filaments, clusters, galaxies,

Andrea Ferrara SISSA/International School for Advanced Studies, Trieste Cosmic Dawn and IGM Reionization.

Low Frequency Background and Cosmology Xuelei Chen National Astronomical Observatories Kashigar, September 10th 2005.

Introduction to the modern observational cosmology Introduction/Overview.

MATTEO VIEL THE LYMAN-  FOREST AS A COSMOLOGICAL PROBE Contents and structures of the Universe – La Thuile (ITALY), 19 March 2006.

1 / 31 Reionization of Universe: 3D Radiative Transfer Simulations T. Nakamoto (Univ. of Tsukuba) 1. Why Reionization ? 2. TsuCube Project 3. Toward a.

Evidence for Feedback in the IGM at High Redshift Barlow (CIT), Becker (CIT), Boksenberg(IoA), Sargent (CIT), Simcoe (MIT), Rauch (OCIW) (based on QSO.

Radiation backgrounds from the first sources and the redshifted 21 cm line Jonathan Pritchard (Caltech) Collaborators: Steve Furlanetto (Yale) Marc Kamionkowski.

Collaborators Blair Savage, Bart Wakker (UW-Madison) Blair Savage, Bart Wakker (UW-Madison) Ken Sembach (STScI) Ken Sembach (STScI) Todd Tripp (UMass)

With: Joop Schaye Leiden (as of last week) Simulation provided by: Tom Theuns, Volker Springel, Lars Hernquist, Scott Kay QSO spectra by: T.-S. Kim, W.

The impact of He II reionisation on the H I Ly-  forest Jamie Bolton Peng Oh (UCSB), Steve Furlanetto (UCLA)

The z > 5 Lyα forest at high resolution George Becker (Caltech) Wal Sargent (Caltech), Michael Rauch (OCIW), Rob Simcoe (MIT) IAU 199 March 18, 2005.

The Distributions of Baryons in the Universe and the Warm Hot Intergalactic Medium Baryonic budget at z=0 Overall thermal timeline of baryons from z=1000.

Complete Ionisation of the Neutral Gas in the Hosts of High Redshift AGN As Traced Through HI and MgII Absorption.

AGN Surveys Phil Outram University of Durham 17 th February 2005.

Simulations of Lyα emission: fluorescence, cooling, galaxies Jordi Miralda Escudé ICREA University of Barcelona, Catalonia Berkeley, Collaborators:

THE LYMAN-  FOREST AS A PROBE OF FUNDAMENTAL PHYSICS MATTEO VIEL Shanghai, 16 March Cosmological significance of the Lyman-  forest 2. LUQAS:

Lyman- Emission from The Intergalactic Medium

From Avi Loeb reionization. Quest to the Highest Redshift.

Probing the Reionization Epoch in the GMT Era Xiaohui Fan (University of Arizona) Seoul/GMT Meeting Oct 5, 2010.

Lyman-  quasar spectra as cosmological probes MATTEO VIEL INAF & INFN – Trieste.

1 Astroparticle Physics in Intergalactic Space Matteo Viel – INAF Trieste APP14 – Amsterdam, 24 th June 2014.

1 / 16 Numerical Simulations for Reionization of the Universe Nakamoto, T. (Univ. of Tsukuba) Hiroi, K. Umemura, M. 1. Why Reionization by 3-D RT ? 2.

T. Ohashi (Tokyo Metropolitan University)

The Twilight Zone of Reionization Steve Furlanetto Yale University March 13, 2006 Steve Furlanetto Yale University March 13, 2006 Collaborators: F. Briggs,

Lyman Alpha Spheres from the First Stars observed in 21 cm Xuelei Chen (Beijing) Jordi Miralda Escudé (IEEC, Barcelona).

OWLS: OverWhelmingly Large Simulations The formation of galaxies and the evolution of the intergalactic medium.

Big Bang f(HI) ~ 0 f(HI) ~ 1 f(HI) ~ History of Baryons (mostly hydrogen) Redshift Recombination Reionization z = 1000 (0.4Myr) z = 0 (13.6Gyr) z.

Constraint on Cosmic Reionization from High-z QSO Spectra Hiroi Kumiko Umemura Masayuki Nakamoto Taishi (University of Tsukuba) Mini Workshop.

Lyα Forest Simulation and BAO Detection Lin Qiufan Apr.2 nd, 2015.

FUSE and HST Observations of Helium II Absorption in the IGM: Implications for Seeing HI Re-ionization Gerard Kriss STScI.

Cosmological Structure with the Lyman Alpha Forest. Jordi Miralda Escudé ICREA, Institut de Ciències del Cosmos University of Barcelona, Catalonia Edinburgh,

Michael Murphy Elisa Boera Collaborators: Supervisor : G. Becker J. Bolton.

WMAP Implications for Reionization

Cosmology With The Lyα Forest

Martin Haehnelt, Matteo Viel, Volker Springel

Jill Bechtold (University of Arizona)

ALMA and Cosmology The high-redshift Universe Advantages of mm/submm

Probing Reionization with Lyman Alpha Emitters Pratika Dayal

Lyman α – impact of the intergalactic medium

Recovery of The Signal from the Epoch of Reionization

STRUCTURE FORMATION MATTEO VIEL INAF and INFN Trieste

High Resolution Spectroscopy of the IGM: How High

Presentation transcript:

Tom Theuns Institute for Computational Cosmology, Durham, UK Department of Physics, Antwerp, Belgium Munich 2005 Reionization And the thermal history of the IGM Tom Theuns Institute for Computational Cosmology, Durham, UK Department of Physics, Antwerp, Belgium

Tom Theuns: IGM thermal history The intergalactic medium can be observed in absorption towards distant bright sources (QSOs, GRBs)

Tom Theuns: IGM thermal history UVES+VLT and HiRes+Keck have revolutionised these data in terms of S/N and resolution

Tom Theuns: IGM thermal history The filamentary pattern of the cosmic web produces absorption lines very similar to those seen in QSO spectra. Cen & Ostriker ‘94 Gas density contours in a cosmological box of size 4Mpc Hubble volume simulation

Tom Theuns: IGM thermal history Increased CPU power has made the simulations more realistic Simulated versus observed high-resolution spectrum. Which is which?

Tom Theuns: IGM thermal history Voigt profile fits can be used to characterise the statistics of lines

Tom Theuns: IGM thermal history The evolution of the column-density fits well with observations for an ionising background dominated by QSOs

Tom Theuns: IGM thermal history Other flux statistics fit well as too. Flux PDFFlux PS

Tom Theuns: IGM thermal history Simulations with feedback produce metal lines not unlike the observed ones, without drastically altering the HI lines

Tom Theuns: IGM thermal history shocked gas unshocked, photo-ionised gas Most of the volume is filled with warm photo-ionised gas, with shocks occupying a small volume around haloes and large filaments

Tom Theuns: IGM thermal history When the IGM is highly ionised, the (photo)-heating rate becomes small.

Tom Theuns: IGM thermal history

Photo-ionisation heating produces a well-defined  -T relation in the low-density IGM that produces the Ly  -forest. (Hui & Gnedin 1997) Temperature of the IGM

Tom Theuns: IGM thermal history

The IGM temperature affects the widths of the Lyman-  lines TT, Schaye & Haehnelt

Tom Theuns: IGM thermal history Line-width (b) and temperature are related Column-density (NH) and density are related Hence can determine  -T relation Schaye et al, Ricotti et al, McDonald et al

Tom Theuns: IGM thermal history IGM temperature as function of redshift. Schaye et al.

Tom Theuns: IGM thermal history Photo-heating rate is less than adiabatic cooling rate

Tom Theuns: IGM thermal history If no other heat sources, HI reionization late? Theuns et al.

Tom Theuns: IGM thermal history (Perceived?) Tension: z reion =17 (WMAP) or z reion around 6 (quasars)?

Tom Theuns: IGM thermal history Tom Abel Ciardi et al.

Tom Theuns: IGM thermal history Wavelets are also sensitive to line-widths Theuns & Zaroubi

Tom Theuns: IGM thermal history Observed QSO looks similar to simulation with HeII reionisation, but without evidence for T fluctuations. Theuns et al. Zaldarriaga.

Tom Theuns: IGM thermal history IGM temperature also affects optical depth (because recombination rate depends on T)

Tom Theuns: IGM thermal history Sloan D A too noisy to see anything? Bernardi et al.

Tom Theuns: IGM thermal history To do list: better constrain T evolution better constrain fluctuations other heating sources? (cosmic rays? X-rays? dust?) Thank you.