Yi-Kuan Chiang Johns Hopkins University
|
|
|
- Emery Stephens
- 5 years ago
- Views:
Transcription
1 WFIRST/Subaru Synergies for Cosmic Radiation Background and Galaxy Proto-clusters Star Light Gas 100 Mpc Illustris Visualization: Shy Genel Yi-Kuan Chiang Johns Hopkins University
2 I. Galaxy Formation in the Field Probed by Cosmic Radiation Background εν(t,ν) II. Galaxy Formation in Overdense Regions of Galaxy Protoclusters
3 I. Galaxy Formation in the Field Probed by Cosmic Radiation Background εν(t,ν) II. Galaxy Formation in Overdense Regions of Galaxy Protoclusters
4 Cosmic History average galaxy evolution circles: Cucciati+12 squares: Schiminovich+05 diamonds: Finkelstein+15 pentagons: Oesch+13 Guo+11 Model Henriques+15 Model
5 Cosmic Radiation Background εν(t,ν) - Quantifying total radiation production in the Universe (by galaxies, after CMB) - Source of IGM/CGM heating /ionization - Tracer of cosmic star formation average galaxy evolution circles: Cucciati+12 squares: Schiminovich+05 diamonds: Finkelstein+15 pentagons: Oesch+13 Guo+11 Model Henriques+15 Model
6 What do we do with the diffuse photons in WFIRST? Cosmic SED εν(t,ν) in Broad-band Intensity Mapping - Diffuse photons in space-based imaging are mostly of astrophysical origin - Should not toss them away like what is usually done in SExtractor - Pixel-based analysis without source detection > Complete census (no-thresholding) of total cosmic light SExtractor back -ground removal?? not always appropriate WFIRST
7 Technique: Spectral Tagging in Broad-band Intensity Mapping -Cosmic SED εν(t,ν) can be probed if we know the redshift PDF of the photons λem = λobs/(1+z)
8 How to Get Redshift PDF for an Intensity Map? Clustering Redshift Menard+13; Newman+08; McQuinn+13 Any Intensity Map I(ϕ) di (z) dz Redshift-Deprojected Intensity Redshift Deprojection Dec cross-correlate with external reference Nref(ϕ, z) Dec RA RA z1 z2 z3 z4 z5 Dec RA z 3D Spec-z Reference ELGs in WFIRST grism and PFS-cosmology Example: Cosmic Infrared Backgrund in Planck Schmidt et al z z
9 Cosmic SED diobs dz I dt = + I t dz ν dν dz Evolution over cosmic time Spectral features in the SED
10 Cosmic SED diobs dz I dt = + I t dz ν dν dz Evolution over cosmic time Spectral features in the SED
11 Cosmic SED diobs dz I dt = + I t dz ν dν dz Evolution over cosmic time Spectral features in the SED
12 WFIRST-HLS 4 broad-band maps (Y, J, H, F184) cross grism ELGs and spec-z ELGs in PFS SSP-cosmology - Cosmic Hα at 0.5 < z < 1.8; Cosmic [OIII] at 1 < z < 3 - Cosmic SFR for all galaxies without thresholding faint objects Hα [OIII] circles: Cucciati+12 squares: Schiminovich+05 diamonds: Finkelstein+15 pentagons: Eschew+13 Guo+11 Model Henriques+15 Model
13 I. Galaxy Formation in the Field Probed by Cosmic Radiation Background εν(t,ν) II. Galaxy Formation in Overdense Regions of Galaxy Protoclusters
14 Cosmic History average galaxy evolution circles: Cucciati+12 squares: Schiminovich+05 diamonds: Finkelstein+15 pentagons: Eschew+13 Guo+11 Model Henriques+15 Model
15 Cosmic History LCDM Universe now -10 average galaxy evolution circles: Cucciati+12 squares: Schiminovich+05 diamonds: Finkelstein+15 pentagons: Eschew+13 Guo+11 Model Henriques+15 Model
16 Cosmic History LCDM Universe Big Crunch now -10 average galaxy evolution circles: Cucciati+12 squares: Schiminovich+05 diamonds: Finkelstein+15 pentagons: Eschew+13 Guo+11 Model Henriques+15 Model
17 Clusters are Overdense Separated Universes LCDM Universe Virialized Big Crunch now -10 average galaxy evolution galaxy evolution in overdense universe "peek into the future (~field at z<0) circles: Cucciati+12 squares: Schiminovich+05 diamonds: Finkelstein+15 pentagons: Oesch+13 Guo+11 Model Henriques+15 Model
18 Cosmic History in Overdense Universe? Virialized? average galaxy evolution galaxy evolution in overdense universe "peek into the future (~field at z<0) circles: Cucciati+12 squares: Schiminovich+05 diamonds: Finkelstein+15 pentagons: Oesch+13 Guo+11 Model Henriques+15 Model
19 Cosmic History in Overdense Universe? Virialized? galaxy evolution in overdense universe "peek into the future (~field at z<0) circles: Cucciati+12 squares: Schiminovich+05 diamonds: Finkelstein+15 pentagons: Eschew+13 Guo+11 Model Henriques+15 Model Prediction Chiang+17
20 Cosmic History in Overdense Universe? Virialized Prediction galaxy evolution in overdense universe "peek into the future (~field at z<0) circles: Cucciati+12 squares: Schiminovich+05 diamonds: Finkelstein+15 pentagons: Eschew+13 Guo+11 Model Henriques+15 Model Prediction Chiang+17
21 Large-Deep Spectroscopic Surveys Offer the Chance to Start Probing Cluster Evolution beyond a few Gyr of Dynamical Time rest optical, [OII] Lyα, rest UV LRGs [OII] [OII] emitters
22 Proto-cluster search: 1. Biased tracer technique δgal(z) galaxy biasing δm(z) gravitational collapse z=0 cluster mass ~10 Mpc scale galaxy overdensity 1 + δgal see Chiang+ 13,15
23 Proto-cluster search: 2. Large-scale structure abundance matching δgal(z) rank order δm(z) rank order z=0 cluster mass - No need to know galaxy bias - Works only for large volume redshift surveys (WFIRST + Subaru PFS) - Can combine galaxies with different selections (WFIRST + Subaru PFS) Galaxy Overdensity CDF Dark Matter Overdensity CDF Chiang in prep.
24 Cosmic History in Overdense Universe? Virialized star formation galaxy assembly in its max. rate galaxy quenching in its max. rate galaxy evolution in overdense universe "peek into the future (~field at z<0) circles: Cucciati+12 squares: Schiminovich+05 diamonds: Finkelstein+15 pentagons: Eschew+13 Guo+11 Model Henriques+15 Model Prediction Chiang+17
25 Subaru: rest optical (4000A) for quenching signatures at 0<z<2 WFIRST: Hα, [OIII] lines for star formation signatures at 1<z<3 Stack CMB survey data (Planck, ACT, S4) for dusty star formation rest optical, [OII] LRGs [OII] Lyα, rest UV [OII] emitters
26 WFIRST HLS-grism protocluster search forecast Mocks based on 3D-HST ELGs and cosmological N-body simulations n ( M protoclusters) ~ 10-6 Mpc -3 Hα emitters [OIII] emitters Need to add PFS at z > 2 Chiang for structures detected with 90 % confidence
27 Summary: Two new science cases enabled by WFIRST-HLS + Subaru PFS-SSP I. Hα-based cosmic star formation and radiation background SED using broad band intensity mapping (Y, J, H, F184 cross spec-z) II. Cosmic star formation and galaxy evolution in protoclusters Outstanding science will be enabled by combining WFIRST and Subaru (first maximize the overlapping area) circles: Cucciati+12 squares: Schiminovich+05 diamonds: Finkelstein+15 pentagons: Eschew+13 Chiang+17
A Systematic Approach to Cluster Formation in the Early Universe - Observations, Simulations, and New Surveys
A Systematic Approach to Cluster Formation in the Early Universe - Observations, Simulations, and New Surveys Yi-Kuan Chiang Roderik Overzier Karl Gebhardt University of Texas at Austin 09/10/2012 From
Discovery of Primeval Large-Scale Structures with Forming Clusters at Redshift z=5.7
Discovery of Primeval Large-Scale Structures with Forming Clusters at Redshift z=5.7 Sadanori Okamura Department of Astronomy, and Research Center for the Early Universe, University of Tokyo Collaborators
Spectral Line Intensity Mapping with SPHEREx
Spectral Line Intensity Mapping with SPHEREx Tzu-Ching Chang (JPL/Caltech) SPHEREx Science Team Hao-Yi Heidi Wu (Ohio State) Olivier Doré Cosmology and First Light - December 2015 1 Line Intensity Mapping
The First Galaxies: Evolution drivers via luminosity functions and spectroscopy through a magnifying GLASS
Charlotte Mason (UCLA) Aspen, 7 Feb 2016 The First Galaxies: Evolution drivers via luminosity functions and spectroscopy through a magnifying GLASS with Tommaso Treu (UCLA), Michele Trenti (U. Melbourne),
The The largest assembly ESO high-redshift. Lidia Tasca & VUDS collaboration
The The largest assembly ESO high-redshift of massive Large galaxies Programme at 2
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
High-Redshift Galaxies: A brief summary
High-Redshift Galaxies: A brief summary Brant Robertson (Caltech) on behalf of David Law (UCLA), Bahram Mobasher (UCR), and Brian Siana (Caltech/Incoming CGE) Observable Cosmological History t~3.7x10 5
Constraining Fundamental Physics with Weak Lensing and Galaxy Clustering. Roland de Pu+er JPL/Caltech COSMO- 14
Constraining Fundamental Physics with Weak Lensing and Galaxy Clustering Roland de Pu+er JPL/Caltech COSMO- 14 Galaxy Clustering: - 3D maps of galaxies - > 3D power spectrum P(k,mu) - BOSS: V = 4.4 (h-
Subaru/WFIRST Synergies for Cosmology and Galaxy Evolution
Artist s concept Subaru/WFIRST Synergies for Cosmology and Galaxy Evolution Dan Masters (JPL/California Institute of Technology) Collaborators: Peter Capak, Olivier Doré, Jason Rhodes, Shoubaneh Hemmati,
Large Scale Structure with the Lyman-α Forest
Large Scale Structure with the Lyman-α Forest Your Name and Collaborators Lecture 1 - The Lyman-α Forest Andreu Font-Ribera - University College London Graphic: Anze Slozar 1 Large scale structure The
Measuring star formation in galaxies and its evolution. Andrew Hopkins Australian Astronomical Observatory
Measuring star formation in galaxies and its evolution Andrew Hopkins Australian Astronomical Observatory Evolution of Star Formation Evolution of Star Formation Evolution of Star Formation Evolution of
The Seeds of Galaxy Clusters and their Galaxies
The Seeds of Galaxy Clusters and their Galaxies Roderik Overzier Max-Planck Institute for Astrophysics IPMU, Kashiwa, June 28 - July 2 2010 Talk Overview Motivation for Cluster Studies at z>2 Overview
Galaxies Across Cosmic Time
Galaxies Across Cosmic Time Overview: 1. Epoch of Reionization (z>6) 2. Stellar Mass Functions to z~6 3. Deep Spectroscopy at z~2-3 4. Circumgalactic Medium (z
Mapping the Universe spectroscopic surveys for BAO measurements Meeting on fundamental cosmology, june 2016, Barcelona, Spain Johan Comparat
Mapping the Universe spectroscopic surveys for BAO measurements Meeting on fundamental cosmology, june 2016, Barcelona, Spain Johan Comparat 1 Baryonic acoustic oscillations The acoustic length scale is
VARIOUS COSMIC ENVIRONMENTS OF NORTHERN HEMISPHERE SKY
IRAM/30m, NOEMA WS@Mitaka, 20180724 VARIOUS COSMIC ENVIRONMENTS OF NORTHERN HEMISPHERE SKY -FOR THE ANTICIPATED STUDIES USING NOEMA/IRAM- Minju Lee (PD) (Nagoya U. /NAOJ MPE from this November) Contents
Wide Field Camera 3: The SOC Science Program Proposal
Wide Field Camera 3: The SOC Science Program Proposal Text An extraordinary panchromatic survey efficiency covering a critical decade of frequency space combined Theme I: Star Formation at Half the Hubble
Fundamental cosmology from the galaxy distribution. John Peacock Hiroshima 1 Dec 2016
Fundamental cosmology from the galaxy distribution John Peacock Subaru @ Hiroshima 1 Dec 2016 What we learn from LSS Fundamental: Astrophysical: Matter content (CDM, baryons, neutrino mass) Properties
Quasar Absorption Lines
Tracing the Cosmic Web with Diffuse Gas DARK MATTER GAS STARS NEUTRAL HYDROGEN Quasar Absorption Lines use quasars as bright beacons for probing intervening gaseous material can study both galaxies and
Unveiling the nature of bright z ~ 7 galaxies with HST and JWST
Unveiling the nature of bright z ~ 7 galaxies with HST and JWST Rebecca Bowler Hintze Fellow, University of Oxford Nicholas Kurti Junior Fellow, Brasenose College with Jim Dunlop, Ross McLure, Derek McLeod,
Lyα-Emitting Galaxies at z=3.1: L* Progenitors Experiencing Rapid Star Formation
Lyα-Emitting Galaxies at z=3.1: L* Progenitors Experiencing Rapid Star Formation Gawiser et al., 2007 Presented on October 22, 2009 PHYS 689: Galaxy Formation Lyman-α Emitters (LAEs) Lyα line is easily
Exploiting Cosmic Telescopes with RAVEN
Exploiting Cosmic Telescopes with RAVEN S. Mark Ammons Lawrence Livermore National Laboratory Thanks to: Ken Wong (Arizona) Ann Zabludoff (Arizona) Chuck Keeton (Rutgers) K. Decker French (Arizona) RAVEN
Anatomy of an X-ray detected cluster at z = 2: low metallicities and enhanced specific star formation rates in star-forming galaxies.
Anatomy of an X-ray detected cluster at z = 2: low metallicities and enhanced specific star formation rates in star-forming galaxies. F. Valentino 1, E. Daddi 1, V. Strazzullo 1,2, R. Gobat 1,3, F. Bournaud
MApping the Most Massive Overdensity Through Hydrogen (MAMMOTH) Zheng Cai (UCSC)
MApping the Most Massive Overdensity Through Hydrogen (MAMMOTH) Zheng Cai (UCSC) IGM Conference From Wall to Web, Berlin, 2016 IGM tomography (Lee+ 14, 15, 16; Stark+ 15ab): IGM Tomography a reconstruction
High-Redshift Galaxies at the Epoch of Cosmic Reionization
High-Redshift Galaxies at the Epoch of Cosmic Reionization Linhua Jiang ( 江林华 ) (KIAA, Peking University) 2014 KIAA-PKU Astrophysics Forum Collaborators: F. Bian, B. Clement, S. Cohen, R. Dave, E. Egami,
Proto-clusters: searches and studies. Bram Venemans (MPIA)
Proto-clusters: searches and studies Bram Venemans (MPIA) Growing up at high redshift: from proto-clusters to galaxy clusters ESAC Madrid 10-13 September 2012 Overview Introduction Finding proto-clusters
Deep Keck Spectroscopy of High-Redshift Quiescent Galaxies
Sirio Belli Max-Planck Institute for Extraterrestrial Physics Deep Keck Spectroscopy of High-Redshift Quiescent Galaxies with Andrew Newman and Richard Ellis Introduction Schawinski et al. 2014 red sequence
Galaxy formation and evolution. Astro 850
Galaxy formation and evolution Astro 850 Introduction What are galaxies? Systems containing many galaxies, e.g. 10 11 stars in the Milky Way. But galaxies have different properties. Properties of individual
MOS: A critical tool for current & future radio surveys Daniel J.B. Smith, University of Hertfordshire, UK.
MOS: A critical tool for current & future radio surveys Daniel J.B. Smith, University of Hertfordshire, UK www.herts.ac.uk/~dsmith/ MOS: A critical tool for current & future radio surveys Outline Why study
A Search for High Redshift Galaxies behind Gravitationally Lensing Clusters
A Search for High Redshift Galaxies behind Gravitationally Lensing Clusters Ota et al.2011 submitted to Monthly Notices of the Royal Astronomical Society Kazuaki Ota (Kyoto U) Johan Richard (Obs.Lyon),
Constraining Source Redshift Distributions with Angular Cross Correlations
Constraining Source Redshift Distributions with Angular Cross Correlations Matt McQuinn (UC Berkeley) in collaboration w/ Martin White arxiv:1302.0857 Technique: Using spatial clustering to measure source
THE GAS MASS AND STAR FORMATION RATE
THE GAS MASS AND STAR FORMATION RATE OF STAR-FORMING GALAXIES AT z ~ 1.3 Nissim Kanekar National Centre for Radio Astrophysics, Pune Apurba Bera Shiv Sethi Ben Weiner K. Dwarakanath Image: B. Premkumar
Dust properties of galaxies at redshift z 5-6
Dust properties of galaxies at redshift z 5-6 Ivana Barisic 1, Supervisor: Dr. Peter L. Capak 2, and Co-supervisor: Dr. Andreas Faisst 2 1 Physics Department, University of Zagreb, Zagreb, Croatia 2 Infrared
Basic BAO methodology Pressure waves that propagate in the pre-recombination universe imprint a characteristic scale on
Precision Cosmology With Large Scale Structure, Ohio State University ICTP Cosmology Summer School 2015 Lecture 3: Observational Prospects I have cut this lecture back to be mostly about BAO because I
Cosmology on the Beach: Experiment to Cosmology
Image sky Select targets Design plug-plates Plug fibers Observe! Extract spectra Subtract sky spec. Cosmology on the Beach: Experiment to Cosmology Fit redshift Make 3-D map Test physics! David Schlegel!1
Reionization constraints post Planck-15
Reionization constraints post Planck-15 Tirthankar Roy Choudhury National Centre for Radio Astrophysics Tata Institute of Fundamental Research Pune CMB Spectral Distortions from Cosmic Baryon Evolution
Cosmology. Jörn Wilms Department of Physics University of Warwick.
Cosmology Jörn Wilms Department of Physics University of Warwick http://astro.uni-tuebingen.de/~wilms/teach/cosmo Contents 2 Old Cosmology Space and Time Friedmann Equations World Models Modern Cosmology
Mapping the z 2 Large-Scale Structure with 3D Lyα Forest Tomography
Mapping the z 2 Large-Scale Structure with 3D Lyα Forest Tomography Intergalactic Matters Meeting, MPIA Heidelberg Max Planck Institut für Astronomie Heidelberg, Germany June 16, 2014 Collaborators: Joe
The Evolution of Massive Galaxies at 3 < z < 7 (The Hawaii 20 deg 2 Survey H2O)
D. Sanders, I. Szapudi, J. Barnes, K. Chambers, C. McPartland, A. Repp (Hawaii) P. Capak, I. Davidson (Caltech), S. Toft (Copenhagen), B. Mobasher (UCRiverside) The Evolution of Massive Galaxies at 3
Dwarf Galaxies as Cosmological Probes
Dwarf Galaxies as Cosmological Probes Julio F. Navarro The Ursa Minor dwarf spheroidal First Light First Light The Planck Satellite The Cosmological Paradigm The Clustering of Dark Matter The Millennium
Galaxy Formation/Evolution and Cosmic Reionization Probed with Multi-wavelength Observations of Distant Galaxies. Kazuaki Ota
Galaxy Formation/Evolution and Cosmic Reionization Probed with Multi-wavelength Observations of Distant Galaxies Kazuaki Ota Department of Astronomy Kyoto University 2013 Feb. 14 GCOE Symposium Outline
Signatures of MG on. linear scales. non- Fabian Schmidt MPA Garching. Lorentz Center Workshop, 7/15/14
Signatures of MG on non- linear scales Fabian Schmidt MPA Garching Lorentz Center Workshop, 7/15/14 Tests of gravity Smooth Dark Energy (DE): unique prediction for growth factor given w(a) Use evolution
Introduction. How did the universe evolve to what it is today?
Cosmology 8 1 Introduction 8 2 Cosmology: science of the universe as a whole How did the universe evolve to what it is today? Based on four basic facts: The universe expands, is isotropic, and is homogeneous.
Galaxies 626. Lecture 3: From the CMBR to the first star
Galaxies 626 Lecture 3: From the CMBR to the first star Galaxies 626 Firstly, some very brief cosmology for background and notation: Summary: Foundations of Cosmology 1. Universe is homogenous and isotropic
The Probes and Sources of Cosmic Reionization Francesco Haardt University of Como INFN, Milano-Bicocca
1 The Probes and Sources of Cosmic Reionization Francesco Haardt University of Insubria@Lake Como INFN, Milano-Bicocca 2 TALK OUTLINE 1. Dark Ages and Reionization 2. Observations: QSO Absorption Lines
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:
EUCLID Spectroscopy. Andrea Cimatti. & the EUCLID-NIS Team. University of Bologna Department of Astronomy
EUCLID Spectroscopy Andrea Cimatti University of Bologna Department of Astronomy & the EUCLID-NIS Team Observing the Dark Universe with EUCLID, ESA ESTEC, 17 November 2009 DARK Universe (73% Dark Energy
You may not start to read the questions printed on the subsequent pages until instructed to do so by the Invigilator.
MATHEMATICAL TRIPOS Part III Friday 8 June 2001 1.30 to 4.30 PAPER 41 PHYSICAL COSMOLOGY Answer any THREE questions. The questions carry equal weight. You may not start to read the questions printed on
Astro 501: Radiative Processes Lecture 34 April 19, 2013
Astro 501: Radiative Processes Lecture 34 April 19, 2013 Announcements: Problem Set 10 due 5pm today Problem Set 11 last one! due Monday April 29 Last time: absorption line formation Q: at high resolution,
COSMOS-CLASH:The existence and universality of the FMR at z<2.5 and environmental effects
COSMOS-CLASH:The existence and universality of the FMR at z
A mid and far-ir view of the star formation activity in galaxy systems and their surroundings
A mid and far-ir view of the star formation activity in galaxy systems and their surroundings Andrea Biviano Andrea Biviano INAF/Osservatorio Astronomico di Trieste Outline: mid-ir & multiwavelength observations
Cosmology: Building the Universe.
Cosmology: Building the Universe. The term has several different meanings. We are interested in physical cosmology - the study of the origin and development of the physical universe, and all the structure
Isotropy and Homogeneity
Cosmic inventory Isotropy and Homogeneity On large scales the Universe is isotropic (looks the same in all directions) and homogeneity (the same average density at all locations. This is determined from
Physical conditions of the interstellar medium in star-forming galaxies at z~1.5
Physical conditions of the interstellar medium in star-forming galaxies at z~1.5 Abstract Masao Hayashi (NAOJ, Mitaka) Subaru seminar @ Subaru Telescope, NAOJ 10 March 2015 To be re-submitted soon to PASJ
Outline. Walls, Filaments, Voids. Cosmic epochs. Jeans length I. Jeans length II. Cosmology AS7009, 2008 Lecture 10. λ =
Cosmology AS7009, 2008 Lecture 10 Outline Structure formation Jeans length, Jeans mass Structure formation with and without dark matter Cold versus hot dark matter Dissipation The matter power spectrum
Illuminating the Dark Ages: Luminous Quasars in the Epoch of Reionisation. Bram Venemans MPIA Heidelberg
Illuminating the Dark Ages: Luminous Quasars in the Epoch of Reionisation Bram Venemans MPIA Heidelberg Workshop The Reionization History of the Universe Bielefeld University, March 8-9 2018 History of
Really, really, what universe do we live in?
Really, really, what universe do we live in? Fluctuations in cosmic microwave background Origin Amplitude Spectrum Cosmic variance CMB observations and cosmological parameters COBE, balloons WMAP Parameters
Structure Formation and Evolution"
Structure Formation and Evolution" From this (Δρ/ρ ~ 10-6 )! to this! (Δρ/ρ ~ 10 +2 )! to this! (Δρ/ρ ~ 10 +6 )! How Long Does It Take?" The (dissipationless) gravitational collapse timescale is on the
UV/optical spectroscopy of Submilliimeter Galaxies
UV/optical spectroscopy of Submilliimeter Galaxies Scott C. Chapman (Caltech), A. Blain (Caltech), I. Smail (Durham), M. Swinbank (Durham) R. Ivison (Edinburgh) SFR_Hα = SFR_FIR SFR_Hα = 1/10 SFR_FIR Outline:
Massively Star-Forming Dusty Galaxies. Len Cowie JCMT Users Meeting
Massively Star-Forming Dusty Galaxies Len Cowie JCMT Users Meeting The luminous dusty star-formation history: We are using SCUBA-2 to address three questions What fraction of the SF is in luminous dusty
Test #1! Test #2! Test #2: Results!
High-Redshift Galaxies II - Populations (cont d) - Current Redshift Frontier - Gravitational Lensing I will hand back Test #2 HW#10 will be due next Monday. Nov 18, 2015 Test #1 Test #2 Test #2: Results
The Cosmic History of Star Formation. James Dunlop Institute for Astronomy, University of Edinburgh
The Cosmic History of Star Formation James Dunlop Institute for Astronomy, University of Edinburgh PLAN 1. Background 2. Star-formation rate (SFR) indicators 3. The last ~11 billion years: 0 < z < 3 4.
11:00-11:25 A. Renzini Massive galaxy growth and quenching: what did we learn and what we would like to know Observations
Monday Setting the stage: Physical processes in galaxy evolution Chair: S. Mei 9:00-9:15 S. Mei Welcome 9:15-9:40 P. Madau Unsolved Problems in Galaxy Formation 9:40-10:05 C. Hayward Galaxy evolution from
What Can We Learn from Galaxy Clustering 1: Why Galaxy Clustering is Useful for AGN Clustering. Alison Coil UCSD
What Can We Learn from Galaxy Clustering 1: Why Galaxy Clustering is Useful for AGN Clustering Alison Coil UCSD Talk Outline 1. Brief review of what we know about galaxy clustering from observations 2.
BAO errors from past / future surveys. Reid et al. 2015, arxiv:
BAO errors from past / future surveys Reid et al. 2015, arxiv:1509.06529 Dark Energy Survey (DES) New wide-field camera on the 4m Blanco telescope Survey started, with first year of data in hand Ω = 5,000deg
Cosmic Web, IGM tomography and Clamato
The mystery figure Cosmic Web, IGM tomography and Clamato Martin White with K-G Lee, J. Hennawi, E. Kitanidis, P. Nugent, J. Prochaska, D. Schlegel, M.Schmittfull, C. Stark, et al. http://clamato.lbl.gov
Cross-correlations of CMB lensing as tools for cosmology and astrophysics. Alberto Vallinotto Los Alamos National Laboratory
Cross-correlations of CMB lensing as tools for cosmology and astrophysics Alberto Vallinotto Los Alamos National Laboratory Dark matter, large scales Structure forms through gravitational collapse......
The cosmic background radiation II: The WMAP results. Alexander Schmah
The cosmic background radiation II: The WMAP results Alexander Schmah 27.01.05 General Aspects - WMAP measures temperatue fluctuations of the CMB around 2.726 K - Reason for the temperature fluctuations
Lecture #24: Plan. Cosmology. Expansion of the Universe Olber s Paradox Birth of our Universe
Lecture #24: Plan Cosmology Expansion of the Universe Olber s Paradox Birth of our Universe Reminder: Redshifts and the Expansion of the Universe Early 20 th century astronomers noted: Spectra from most
Two-halo Galactic Conformity as a Test of Assembly Bias
Two-halo Galactic Conformity as a Test of Assembly Bias Angela Berti UC San Diego GalFRESCA 2018 1 Galactic Conformity Correlation between star formation rates (SFRs) of central galaxies and their satellites/neighbors
Cross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background
Cross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background Masato Shirasaki (Univ. of Tokyo) with Shunsaku Horiuchi (UCI), Naoki Yoshida (Univ. of Tokyo, IPMU) Extragalactic Gamma-Ray Background
The First Appearance of the Red Sequence of Galaxies in Proto-Clusters at 2<z<3
Subaru User s Meeting 2007 (Mitaka, 30/01/2007) The First Appearance of the Red Sequence of Galaxies in Proto-Clusters at 2
Physical properties of high-z star-forming galaxies with FMOS-COSMOS
Physical properties of high-z star-forming galaxies with FMOS-COSMOS John Silverman Kavli IPMU Daichi Kashino, Alvio Renzini, Emanuele Daddi, Giulia Rodighiero, Nobuo Arimoto, Tohru Nagao, Dave Sanders,
BUILDING GALAXIES. Question 1: When and where did the stars form?
BUILDING GALAXIES The unprecedented accuracy of recent observations of the power spectrum of the cosmic microwave background leaves little doubt that the universe formed in a hot big bang, later cooling
Observations and Inferences from Lyman-α Emitters
Observations and Inferences from Lyman-α Emitters Christopher J. White 6 March 2013 Outline 1 What Are Lyα Emitters? 2 How Are They Observed? 3 Results and Inferences 4 HSC 5 Conclusion The Lyα Line n
An extremely dense group of massive galaxies at the centre of the protocluster at z=3.09 in the SSA22 field
An extremely dense group of massive galaxies at the centre of the protocluster at z=3.09 in the SSA22 field 2015/9/7-11 In the Footsteps of Galaxies @Soverato Mariko Kuob (ICRR Univ Tokyo), Toru Yamada,
Formation of z~6 Quasars from Hierarchical Galaxy Mergers
Formation of z~6 Quasars from Hierarchical Galaxy Mergers Yuexing Li et al Presentation by: William Gray Definitions and Jargon QUASAR stands for QUASI-stellAR radio source Extremely bright and active
Probing the End of Dark Ages with High-redshift Quasars. Xiaohui Fan University of Arizona Dec 14, 2004
Probing the End of Dark Ages with High-redshift Quasars Xiaohui Fan University of Arizona Dec 14, 2004 High-redshift Quasars and the End of Cosmic Dark Ages Existence of SBHs at the end of Dark Ages BH
Highlights from the VIMOS VLT Deep Survey
Highlights from the VIMOS VLT Deep Survey Olivier Le Fèvre, LAM, Marseille On behalf of the VVDS team An unbiased survey of the Universe 0
Dusty Starforming Galaxies: Astrophysical and Cosmological Relevance
Dusty Starforming Galaxies: Astrophysical and Cosmological Relevance Andrea Lapi SISSA, Trieste, Italy INFN-TS, Italy INAF-OATS, Italy in collaboration with F. Bianchini, C. Mancuso C. Baccigalupi, L.
The Intergalactic Medium: Overview and Selected Aspects
The Intergalactic Medium: Overview and Selected Aspects Draft Version Tristan Dederichs June 18, 2018 Contents 1 Introduction 2 2 The IGM at high redshifts (z > 5) 2 2.1 Early Universe and Reionization......................................
Astro-2: History of the Universe
Astro-2: History of the Universe Lecture 8; May 7 2013 Previously on astro-2 Wherever we look in the sky there is a background of microwaves, the CMB. The CMB is very close to isotropic better than 0.001%
Solving. Andrey Kravtsov The University of Chicago Department of Astronomy & Astrophysics Kavli Institute for Cosmological Physics
Solving Constraining galaxy formation with gaseous halos Andrey Kravtsov The University of Chicago Department of Astronomy & Astrophysics Kavli Institute for Cosmological Physics X-ray Vision workshop:
Galaxies 626. Lecture 10 The history of star formation from far infrared and radio observations
Galaxies 626 Lecture 10 The history of star formation from far infrared and radio observations Cosmic Star Formation History Various probes of the global SF rate: ρ* (z) M yr 1 comoving Mpc 3 UV continuum
Galaxy mass assembly in KiDS: dynamics and gravitational lensing
Galaxy mass assembly in KiDS: dynamics and gravitational lensing r-band Crescenzo Tortora KiDS SDSS KiDS@VST aims to image 1500 square degrees in 4 optical bands (complemented in the NIR with VIKING@VISTA).
Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines!
Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines Idealized 21cm spectra Example observed 21cm spectra HI densities
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
Cosmology with Peculiar Velocity Surveys
Cosmology with Peculiar Velocity Surveys Simulations Fest, Sydney 2011 Morag I Scrimgeour Supervisors: Lister Staveley-Smith, Tamara Davis, Peter Quinn Collaborators: Chris Blake, Brian Schmidt What are
Exploring massive galaxy evolution with deep multi-wavelength surveys
Exploring massive galaxy evolution with deep multi-wavelength surveys Ross McLure, Henry Pearce, Michele Cirasuolo, Jim Dunlop (Edinburgh) Omar Almaini (Nottingham), Chris Simpson (Liverpool) Outline 1.
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
Illustris vs Real Universe: Satellite LF, ksz Effect,
Illustris vs Real Universe: Satellite LF, ksz Effect, Hyunbae Park (KASI), + Many people SFR of High-z Galaxies 2017. 06. 02 (Uleung-Do) Simulation Setup Simulation code : AREPO (moving mesh code) Parameter
Present and future redshift survey David Schlegel, Berkeley Lab
Present and future redshift survey David Schlegel, Berkeley Lab David Schlegel, COSMO-17 @Paris, 30 Aug 2017 1 Redshift surveys = one of ~few probes of inflationary epoch Inflation-era parameters: non-gaussianity,
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,
Benjamin Weiner Steward Observatory November 15, 2009 Research Interests
Benjamin Weiner Steward Observatory November 15, 2009 Research Interests My recent research projects study galaxy evolution with emphasis on star formation histories, gas accretion and outflow, and galaxy
Million Element Integral Field Unit Design Study
Million Element Integral Field Unit Design Study Simon Morris, Robert Content, Cedric Lacey (University of Durham, UK) AURA contract No. 9414257-GEM00303 Milestone 1 Prepare and present a PowerPoint presentation
The ALMA z=4 Survey (AR4S)
The ALMA z=4 Survey (AR4S) ALMA studies of massive z~4-5 galaxies Corentin Schreiber Leiden University October 21 2016 In collaboration with: Maurilio Pannella, David Elbaz, Roger Leiton, Tao Wang, and
X name "The talk" Infrared
X name "The talk" Infrared 1 Cosmic Infrared Background measurement and Implications for star formation Guilaine Lagache Institut d Astrophysique Spatiale On behalf of the Planck collaboration Cosmic Infrared
Dusty star-forming galaxies at high redshift (part 5)
Dusty star-forming galaxies at high redshift (part 5) Flow of story 4.1.1 4.1.2 4.1.3 Millimetric Spectroscopic Redshifts Millimetric Photometric Redshifts Redshift Distributions of 24 μm selected DSFG
Interpreting Galaxies across Cosmic Time with Binary Population Synthesis Models
Interpreting Galaxies across Cosmic Time with Binary Population Synthesis Models Elizabeth Stanway Warwick (UK) with J J Eldridge (Auckland, NZ) and others Putting Warwick on the Map WARWICK! London @WarwickAstro
Simulating non-linear structure formation in dark energy cosmologies
Simulating non-linear structure formation in dark energy cosmologies Volker Springel Distribution of WIMPS in the Galaxy Early Dark Energy Models (Margherita Grossi) Coupled Dark Energy (Marco Baldi) Fifth
Cosmic Microwave Background
Cosmic Microwave Background Following recombination, photons that were coupled to the matter have had very little subsequent interaction with matter. Now observed as the cosmic microwave background. Arguably