Myung Gyoon Lee with In Sung Jang
|
|
|
- Ashlie Floyd
- 5 years ago
- Views:
Transcription
1 Myung Gyoon Lee with In Sung Jang Department of Physics & Astronomy Seoul National University, Korea Cosmological Quests for the Next Decade, Apr 16-18, 2014, KASI, Korea 1
2 Past: Two number cosmology A search for two numbers: H 0 & q 0 (Sandage) Present : Parametric cosmology (many parameters for geometry and dynamics of the universe, CMB, structures, neutrinos, grav waves, nuisance parameters ) e.g. H(z) 2 /H 02 = M (1+z) 3 + DE (1+z) 3(1+w) + 2
3 H 0 =H(t=today) : the expansion rate now The value of H 0 = f(t)? 3
4 Since 1929 of the Hubble s law, long debates among Sandage, de Vaucouleurs and more: H 0 =50 versus 100 km/s/mpc A factor of two! 4
5 A movie: compiled: by John Huchra (HSAO/cfa) made by Richard de Grijs (Beijing Univ) 5
6 HST H 0 key project. I. Freedman et al. (2001) : The final result -Cepheid distance estimate : for 8 SN Ia hosts -SN Ia in nearby universe (z~0.1): 36 SNe Ia -H 0 = 71 ± 2 ± 6 km/s/mpc (~10% error) -the most popular value until recently (N(citation)>2000) 6
7 Sandage et al. (2006) : HST key project. II. -Cepheid distance estimate : for 10 SN Ia hosts -SN Ia in nearby universe (z~0.1) : 62 SNe Ia -H 0 = 62.3 ± 1.3 ± 5.0 km/s/mpc (~10% error) <-> H 0 = 71 ± 2 ± 6 km/s/mpc (Freedman+2001) 7
8 Local measurements of H 0 with SN Ia Riess et al. (2009, 2011) SHOES Cepheid (MW,LMC) and Maser distance estimate : for 8 SN Ia SN Ia in nearby universe (z<0.1) : 140 SNe Ia H 0 = 73.8 ± 2.4 km/s/mpc (4.1% error) Freedman et al. (2012): Carnegie H 0 Project (CHP) I Method : Recalibration of Key project sample using MIR P-L relation of Galactic Cepheids SN Ia in nearby universe (z<0.1) : 36 SNe Ia H 0 = 74.3 ± 2.1 km/s/mpc (2.8% error) (2012 value) H 0 = 74 ± 2 km/s/mpc 8
9 M101: one of the nearest galaxies with SN Ia SN 2011fe: one of the best obs data Lee & Jang (2012) -Re-calibration of SN Ia with TRGB M101 -H 0 =65 6 km/s/mpc B.Fulton (2011) 9
10 CMB at z~1100 WMAP9 (Hinshaw+2013) H 0 = km/s/mpc PLANCK 2013 XVI. Cosmological parameters H 0 = km/s/mpc 10
11 Local U (SN Ia): H 0 =74 2 km/s/mpc High z (CMB, BAO): H 0 =68 2 km/s/mpc The Hubble Tension: 2-3 difference 11
12 Local U (SNe Ia): H 0 =74 2 km/s/mpc High z (CMB, BAO): H 0 =67 1 km/s/mpc Three ways to approach the problem 1) Systematic errors in each H 0 (z=0) & H 0 (high z) 2) Relation between high z and low z (Are we in a Hubble bubble?) 3) New parameters or physics, if real! 12
13 Various methods for H 0 estimation A large range of the H 0 values. * 13
14 CMB versus SN Ia based on Cepheids or TRGB The Hubble tension? * CMB SN Ia (Cep) SN Ia(TRGB) 14
15 * w0, neutrino (Ex) The effective N of neutrino species : N eff =f(ω m h 2 ) WMAP+BAO+H 0 : (Komatsu+2011) N eff = vs 3.04 (standard value) => Better H 0 Better N eff ( ) Komatsu et al (2011, ApJS, 192, 18) 15
16 * BICEP2 2014: The inflationary ration of tensor-to-scalar fluctuation, r = Dvorkin+ (2014) suggested evidence for massive sterile neutrinos from combing CMB+BICEP2+BAO+H 0 N(eff)= m = ev Dvorkin et al. (2014) 16
17 SNe Ia may be the best! Bright From low Z to high Z Small dispersion Many studies 17
18 Calibration of SN Ia is critical for H 0. Need nearby galaxies hosting SN Ia. 18
19 CHP, SHOES (<2013) SN Ia calibration with Cepheids Cepheid calibration with M106 (NGC 4258), LMC, MW N (SN Ia host) is small! Anhor: M106 (NGC 4258) 19
20 M106 has a water maser in the center, allowing a geometric distance. Herrstein+1999: d= Mpc Riess+(2011) H 0 = km/s/mpc Humphreys+2013: d= Mpc H 0 = km/s/mpc Efstathiou (2014) reanalysis with d=7.6mpc H 0 = km/s/mpc 20
21 Sne Ia used for calibration in CHP, SHOES (<2013) In 2011, a new comer in a much closer distance! M101 SN2011fe 21
22 Pop II calibration Independent of Cepheids TRGB! 22
23 (observation) The tip of the red giant branch (RGB) in the HR diagram (theory) Low mass stars in the core-he flash stage (old than a few Gyrs) TRGB Globular cluster M55 23
24 -Galaxies have stars with a large range of ages, including many old stars! (halo RGBs: source of NIR fluctuation? (Cooray+2012,today)) -TRGBs are seen in any-types of galaxies older than a few Gyr old -The TRGB is comparable to Cepheids in precision, but having a few advantages (Lee, Freedman & Madore 1993) Tolstoy (2009) 24
25 TRGB Cepheid Pros Little metallicity effect in any types of galaxies non variables no extinction can calibrate nearby EDS bright luminosity (M V,max ~-6) long history? Cons fainter (M I ~ -4.0) can be used for d<25 Mpc Metallicity effect Interstellar extinction Only in late-type galaxies Requiring much observing time
26 * SN Ia 2011 fe Discovered in 2011 The nearest SN Ia with modern data since The best calibrator for SN Ia? Optical & NIR data M101 * B.Fulton (2011) 26
27 * Resolved stars are mostly RGBs and AGBs. * Edge-detection algorithm: TRGB Lee & Jang (2012, ApJ Letter) 27
28 1) I-band luminosity function -> Edge detection 2) I(TRGB) =25.28 ±0.01 Lee & Jang (2012, ApJ Letter) 28
29 (m-m) 0 =29.30 ±0.01(random) ± 0.12(systematic) (d=7.24 ± 0.03 ± 0.40 kpc) Lee & Jang (2012, ApJ Letter) 29
30 Optical: Mv(max) = ± 0.12 (Mv(max) = ± 0.07 in Riess+2011) (Mv(max) = ± 0.05 in Gibson+2000) 30
31 Optical: Mv(max) = ± 0.12 => H 0 = 65.0 ± 0.5 ± 5.7 km/s/mpc 31
32 Three possibilities: 1) SN 2011fe (M101) may be 0.2 mag brighter than typical SNe Ia. 2) Recent calibration of SNe Ia may be 0.2mag fainter (Riess et al. 2011). 3) H 0 may be smaller than 73 km/s/mpc. (N eff is closer to the standard value). -> Need a better estimate of H 0! 32
33 *w 0 =f(h 0 ), N eff =f(ω m h 2 ) => Better H 0 Better w 0, N eff ( ) Lee and Jang (2012, ApJL) Freedman et al (2012, ApJ) 33
34 Criteria for targets -Galaxies at <30 Mpc hosting SN Ia -HST images -with modern photometry -with low extinction In 2014: N(candidates)=8 HST cycle 22 proposal : submitted. (Freedman, Madore, MGL et al) Current progress: M101 (Lee & Jang 2012) M66 and M96 (Lee & Jang 2013) NGC 1316 and others (Jang & Lee 2014, in preparation) 34
35 Three possibilities: 1) Current calibration of the TRGB (a) M101 (b) M66 (c) M96 (d) NGC 1316 (a) M101 (b) M66 (c) M96 (d) NGC
36 Lee & Jang 2014, Jang & Lee 2014 Based on 4 low reddened SNe Ia in M101 and NGC 1316 M V (max) = ±0.02 (ran) ± 0.12(sys), H 0 = 68.6 ±2.3 (ran) ± 3.7 (sys) 36
37 37
38 Three ways: 1) Reducing systematic errors of high z and local measurements -CMB, BAO, galaxy clusters, time delay of lensed quasars, -Cepheids, TRGB, RR Lyrae, maser, eclipsing binaries -age of the universe (Bond+2014, Verde+2013) 2) Understanding better the relations between local and high z measurements 3) Thinking about new parameters or new physics 38
39 H 0 in 2014: still evolving! Stay tuned! The future of the H 0 tension?? 39
Myung Gyoon Lee. Seoul National University (SNU), Korea. The 7 th Survey Science Workshop, Jan 15-17, 2018, High-1 Resort, Korea
Myung Gyoon Lee with In Sung Jang (AIP) Department of Physics & Astronomy Seoul National University (SNU), Korea The 7 th Survey Science Workshop, Jan 15-17, 2018, High-1 Resort, Korea 1 H 0 Today s Expansion
Measuring the Hubble Constant. Fundamental Cosmic Distance Scale Naples, May 3, 2011 Wendy Freedman Carnegie Observatories
Measuring the Hubble Constant Fundamental Cosmic Distance Scale Naples, May 3, 2011 Wendy Freedman Carnegie Observatories Allan Sandage (1926-2010) UnProgress in Measuring H o HST Factor of 2 Era Era of
Practice Problem!! Assuming a uniform protogalactic (H and He only) cloud with a virial temperature of 10 6 K and a density of 0.
Practice Problem Assuming a uniform protogalactic (H and He only) cloud with a virial temperature of 10 6 K and a density of 0.05 cm -3 (a) estimate the minimum mass that could collapse, (b) what is the
That other way to measure H0:
That other way to measure H0: Rachael L. Beaton Carnegie Observatories Carnegie-Chicago Hubble Program A prospectus on distance measurement with Image: NASA/JPL WFIRST-AFTA Distance Ladder The distance
Measuring the Hubble Constant through Cepheid Distances
Measuring the Hubble Constant through Cepheid Distances Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant Freedman, Madore, Gibson, et al., Astrophysical Journal
The Old Stellar Population Studies with Subaru Young-Wook Lee Yonsei Univ., Seoul, Korea
(Some humble suggestions for) The Old Stellar Population Studies with Subaru Young-Wook Lee Yonsei Univ., Seoul, Korea 1. Globular cluster Dwarf galaxy Connection (Some) Globular clusters show multiple
The Next 2-3 Weeks. Important to read through Chapter 17 (Relativity) before I start lecturing on it.
The Next 2-3 Weeks [27.1] The Extragalactic Distance Scale. [27.2] The Expansion of the Universe. [29.1] Newtonian Cosmology [29.2] The Cosmic Microwave Background [17] General Relativity & Black Holes
Cosmology at a Crossroads: Tension With the Hubble Constant
Cosmology at a Crossroads: Tension With the Hubble Constant Wendy L. Freedman We are at an interesting juncture in cosmology. With new methods and technology, the accuracy in measurement of the Hubble
Sample variance in the local measurements of H 0. Heidi Wu (Caltech OSU) with Dragan Huterer (U. Michigan) arxiv: , MNRAS accepted
Sample variance in the al measurements of H 0 Heidi Wu (Caltech OSU) with Dragan Huterer (U. Michigan) arxiv:1706.09723, MNRAS accepted 1 Tension in H 0 measurements Beaton (2016); Freedman (2017) 2 H
Techniques for measuring astronomical distances generally come in two variates, absolute and relative.
Chapter 6 Distances 6.1 Preliminaries Techniques for measuring astronomical distances generally come in two variates, absolute and relative. Absolute distance measurements involve objects possibly unique
4.1 The Scale of the Universe: Basis of the Cosmological Distance Scale
4.1 The Scale of the Universe: Basis of the Cosmological Distance Scale 1 The Scale of the Universe The Hubble length, D H = c/h 0, and the Hubble time, t H = 1/H 0 give the approximate spatial and temporal
Allan Sandage and the Cosmic Expansion
Allan Sandage and the Cosmic Expansion The Fundamental Cosmic Distance Scale Conference, Naples May 2 6, 2011 G. A. Tammann Allan Sandage a mentor, a collaborator, a friend for 47 years G. A. Tammann A.
Set 5: Expansion of the Universe
Set 5: Expansion of the Universe Cosmology Study of the origin, contents and evolution of the universe as a whole Expansion rate and history Space-time geometry Energy density composition Origin of structure
The Hubble Constant. Measuring the Scale of the Universe. The Scale of the Universe. In this lecture:
Ay 127, Spring 2013 Extragalactic Distance Scale In this lecture: S. G. Djorgovski Hubble constant: its definition and history The extragalactic distance ladder The HST Key Project and the more modern
The cosmic distance scale
The cosmic distance scale Distance information is often crucial to understand the physics of astrophysical objects. This requires knowing the basic properties of such an object, like its size, its environment,
Building the cosmic distance scale: from Hipparcos to Gaia
The Fundamental Distance Scale: state of the art and the Gaia perspectives 3-6 May 2011 Building the cosmic distance scale: from Hipparcos to Gaia Catherine TURON and Xavier LURI 1 ESA / ESO-H. Heyer Fundamental
Chapter 8: Simple Stellar Populations
Chapter 8: Simple Stellar Populations Simple Stellar Population consists of stars born at the same time and having the same initial element composition. Stars of different masses follow different evolutionary
Luminosity Functions of Planetary Nebulae & Globular Clusters. By Azmain Nisak ASTR 8400
Luminosity Functions of Planetary Nebulae & Globular Clusters By Azmain Nisak ASTR 8400 Calculating Distance! m = apparent magnitude! M = absolute magnitude! r = distance in pc GLOBULAR CLUSTERS AS DISTANCE
H 0 is Undervalued BAO CMB. Wayne Hu STSCI, April 2014 BICEP2? Maser Lensing Cepheids. SNIa TRGB SBF. dark energy. curvature. neutrinos. inflation?
H 0 is Undervalued BICEP2? 74 Maser Lensing Cepheids Eclipsing Binaries TRGB SBF SNIa dark energy curvature CMB BAO neutrinos inflation? Wayne Hu STSCI, April 2014 67 The 1% H 0 =New Physics H 0 : an end
Page # Astronomical Distances. Lecture 2. Astronomical Distances. Cosmic Distance Ladder. Distance Methods. Size of Earth
Size of Astronomical istances ecture 2 Astronomical istances istance to the Moon (1 sec) istance to the Sun (8 min) istance to other stars (years) istance to centre of our Galaxy ( 30,000 yr to centre)
Simple Stellar Populations
Stellar Objects: Simple Stellar Populations 1 Simple Stellar Populations 1 Theoretical isochrones Update date: December 14, 2010 Simple Stellar Population consists of stars born at the same time and having
The Extragalactic Distance Scale
One of the important relations in Astronomy. It lets us Measure the distance to distance objects. Each rung on the ladder is calibrated using lower-rung calibrations. Distance Objects Technique 1-100 AU
The Great Debate: The Size of the Universe (1920)
The Great Debate: The Size of the Universe (1920) Heber Curtis Our Galaxy is rather small, with Sun near the center. 30,000 LY diameter. Universe composed of many separate galaxies Spiral nebulae = island
Lecture 9. Basics Measuring distances Parallax Cepheid variables Type Ia Super Novae. Gravitational lensing Sunyaev-Zeldovich effect
Lecture 9 H 0 from the Hubble diagram Basics Measuring distances Parallax Cepheid variables Type Ia Super Novae H 0 from other methods Gravitational lensing Sunyaev-Zeldovich effect H 0 from the Hubble
The Extragalactic Distance Scale
One of the important relations in Astronomy. It lets us Measure the distance to distance objects. Each rung on the ladder is calibrated using lower-rung calibrations. Distance Objects Technique 1-100 AU
The Observable Universe: Redshift, Distances and the Hubble-Law. Max Camenzind Sept 2010
The Observable Universe: Redshift, Distances and the Hubble-Law Max Camenzind Bremen @ Sept 2010 Key Facts Universe 1. The Universe is expanding and presently even accelerating. Hubble Expansion: Space
Galaxies. The majority of known galaxies fall into one of three major classes: spirals (78 %), ellipticals (18 %) and irregulars (4 %).
Galaxies Collection of stars, gas and dust bound together by their common gravitational pull. Galaxies range from 10,000 to 200,000 light-years in size. 1781 Charles Messier 1923 Edwin Hubble The distribution
A New Measurement of the Expansion Rate of the Universe And a Path to 1% with Gaia
Johns Hopkins University Space Telescope Science Institute A New Measurement of the Expansion Rate of the Universe And a Path to 1% with Gaia based on Riess et al. 2016, ApJ, 826,56, The SH0ES Team Expanding
Astronomy from 4 Perspectives Bi-national Heraeus Sumer School Series for Teacher Students and Teachers
Astronomy from 4 Perspectives Bi-national Heraeus Sumer School Series for Teacher Students and Teachers I. Cosmology Prof. Dr. Andreas Just Zentrum für Astronomie Heidelberg University Cosmic Distances
6. Star Colors and the Hertzsprung-Russell Diagram
In addition to its brightness, light in general is characterized by its color. 6. Star Colors and the Hertzsprung-Russell Diagram http://apod.nasa.gov/apod/ Depending on the temperature of the matter at
Outline. Go over AGN problem, again, should be rotating BH Go over problem 6.6 Olber's paradox Distances Parallax Distance ladder Direct checks
Outline Go over AGN problem, again, should be rotating BH Go over problem 6.6 Olber's paradox Distances Parallax Distance ladder Direct checks Why is the night sky dark? (Olber s Paradox 1826) Or what
Relativity and Astrophysics Lecture 15 Terry Herter. RR Lyrae Variables Cepheids Variables Period-Luminosity Relation. A Stellar Properties 2
Stellar Properties Relativity and Astrophysics Lecture 15 Terry Herter Outline Spectroscopic Parallax Masses of Stars Periodic Variable Stars RR Lyrae Variables Cepheids Variables Period-Luminosity Relation
Galaxies. Lecture Topics. Lecture 23. Discovering Galaxies. Galaxy properties. Local Group. History Cepheid variable stars. Classifying galaxies
Galaxies Lecture 23 APOD: NGC 3628 (The Hamburger Galaxy) 1 Lecture Topics Discovering Galaxies History Cepheid variable stars Galaxy properties Classifying galaxies Local Group 2 23-1 Discovering Galaxies
6. Star Colors and the Hertzsprung-Russell Diagram
6. Star Colors and the Hertzsprung-Russell Diagram http://apod.nasa.gov/apod/ Supernovae Type Ia in M82 January 22, 2014 Still rising may go to m = 8 (or 10?) What we can learn about stars from their light:
6. Star Colors and the Hertzsprung-Russell Diagram.
6. Star Colors and the Hertzsprung-Russell Diagram http://apod.nasa.gov/apod/ Supernovae Type Ia in M82 January 22, 2014 Still rising may go to m = 8 (or 10?) What we can learn about stars from their light:
6. Star Colors and the Hertzsprung-Russell Diagram
What we can learn about stars from their light: II Color In addition to its brightness, light in general is characterized by its color (actually its wavelength) 6. Star Colors and the Hertzsprung-Russell
Distance measurements
Distance measurements Pierre Hily-Blant 2018-19 Contents A current issue: The Hubble constant As you know, the Universe is expanding (this expansion is currently accelerating). The Hubble's law says that
24.1 Hubble s Galaxy Classification
Chapter 24 Galaxies Units of Chapter 24 24.1 Hubble s Galaxy Classification 24.2 The Distribution of Galaxies in Space 24.3 Hubble s Law 24.4 XXActive Galactic Nuclei XXRelativistic Redshifts and Look-Back
Type II Supernovae as Standardized Candles
Type II Supernovae as Standardized Candles Mario Hamuy 1 2 Steward Observatory, The University of Arizona, Tucson, AZ 85721 Philip A. Pinto Steward Observatory, The University of Arizona, Tucson, AZ 85721
Chapter 14 The Milky Way Galaxy
Chapter 14 The Milky Way Galaxy Spiral Galaxy M81 - similar to our Milky Way Galaxy Our Parent Galaxy A galaxy is a giant collection of stellar and interstellar matter held together by gravity Billions
The Hubble Space Telescope and the Hubble Constant
The Hubble Space Telescope and the Hubble Constant Jeremy Mould Centre for Astrophysics and Supercomputing Swinburne University Telescope resolution Due to the wave nature of light (diffraction) the optical
Arguments for a Hubble Constant near H 0 =55
Arguments for a Hubble Constant near H 0 =55 H. Arp Max-Planck-Institut für Astrophysik, Garching 85741, Germany ABSTRACT Recent analyses of Cepheid distances to spiral galaxies have led to an announcement
Exam 4 Review EXAM COVERS LECTURES 22-29
Exam 4 Review EXAM COVERS LECTURES 22-29 Theoretically is there a center of the universe? Is there an edge? Do we know where Earth is on this? There is no center to the Universe, What kind of light we
Distance Measuring Techniques and The Milky Way Galaxy
Distance Measuring Techniques and The Milky Way Galaxy Measuring distances to stars is one of the biggest challenges in Astronomy. If we had some standard candle, some star with a known luminosity, then
Today in Astronomy 142: farther
Hubble s Law Active galaxies I: quasars, their rather large luminosities, and the supermassive black holes within them. Today in Astronomy 142: farther M106, a.k.a. NGC 4258: active galaxy, and lynchpin
SIM PLANETQUEST, LUMINOSITY-INDEPENDENT EXTRA-GALACTIC DISTANCES
Draft version June 4, 2008 Preprint typeset using L A TEX style emulateapj v. 10/10/03 SIM PLANETQUEST, LUMINOSITY-INDEPENDENT EXTRA-GALACTIC DISTANCES Rob P. Olling 1 Draft version June 4, 2008 ABSTRACT
The Milky Way. Finding the Center. Milky Way Composite Photo. Finding the Center. Milky Way : A band of and a. Milky Way
The Milky Way Milky Way : A band of and a The band of light we see is really 100 billion stars Milky Way probably looks like Andromeda. Milky Way Composite Photo Milky Way Before the 1920 s, astronomers
Myung Gyoon Lee. With Ho Seong Hwang (CfA) and Hong Soo Park (NAOJ) (Dept of Physics and Astronomy, Seoul National University)
Myung Gyoon Lee (Dept of Physics and Astronomy, Seoul National University) With Ho Seong Hwang (CfA) and Hong Soo Park (NAOJ) 2013. 10. 22 Dynamics of Disk Galaxies, The 7 th Korean Astrophysics Workshop,
Week 1 Introduction: GR, Distances, Surveys
Astronomy 233 Spring 2011 Physical Cosmology Week 1 Introduction: GR, Distances, Surveys Joel Primack University of California, Santa Cruz Modern Cosmology A series of major discoveries has laid a lasting
STELLAR POPULATIONS OF THE DWARF GALAXY UKS IN THE SCULPTOR GROUP. and
Draft version May 7, 1999 Preprint typeset using L A TEX style emulateapj STELLAR POPULATIONS OF THE DWARF GALAXY UKS 2323 326 IN THE SCULPTOR GROUP Myung Gyoon Lee Department of Astronomy, Seoul National
Hubble s Law. Tully-Fisher relation. The redshift. λ λ0. Are there other ways to estimate distances? Yes.
Distances to galaxies Cepheids used by Hubble, 1924 to show that spiral nebulae like M31 were further from the Sun than any part of the Milky Way, therefore galaxies in their own right. Review of Cepheids
Lecture 7:Our Universe
Lecture 7:Our Universe 1. Traditional Cosmological tests Theta-z Galaxy counts Tolman Surface Brightness test 2. Modern tests HST Key Project (H o ) Nucleosynthesis (Ω b ) BBN+Clusters (Ω M ) SN1a (Ω M
Distance measurements
Distance measurements Pierre Hily-Blant Université Grenoble Alpes Université Grenoble Alpes // 2018-19 Contents 1 A current issue: The Hubble constant 2 2 Introduction 3 3 Trigonometric parallax 4 4 Photometric
Supernovae and the Accelerating Universe
Supernovae and the Accelerating Universe Nicholas B. Suntzeff Mitchell Institute for Fundamental Physics Department of Physics & Astronomy Texas A&M University University of Texas/Austin Second Texas Cosmology
Myung Gyoon LEE Department of Physics & Astronomy Seoul National University, Korea
Myung Gyoon LEE Department of Physics & Astronomy Seoul National University, Korea Cosmology and Structure Formation (The 4 th KIAS workshop), Nov 4-6, 2010, KIAS, Korea 1 M.G. Lee, Sungsoon Lim (SNU)
STRUCTURE AND DYNAMICS OF GALAXIES
STRUCTURE AND DYNAMICS OF GALAXIES 3., classification of galaxies Piet van der Kruit Kapteyn Astronomical Institute University of Groningen, the Netherlands www.astro.rug.nl/ vdkruit Beijing, September
Near infrared high resolution spectroscopy of variable stars G. Bono, Univ. Of Rome ToV + D. Magurno, M. Urbaneja + many others
Near infrared high resolution spectroscopy of variable stars G. Bono, Univ. Of Rome ToV + D. Magurno, M. Urbaneja + many others Near infrared high resolution spectroscopy of variable stars G. Bono, Univ.
Jason Kalirai (STScI)
Jason Kalirai (STScI) Outline An Introduction: The First Hints on How Stars Evolve. Our Current Picture of Stellar Evolution A Surprise in our Backyard: The First Discovered White Dwarf Why Search for
Cosmicflows-2. Laniakea Supercluster
Cosmicflows-2 Laniakea Supercluster Cosmic Flows Program Measure distances d Peculiar velocities: V pec = V obs - H 0 d Infer 3D velocities and density field Project to initial conditions Simulate evolution
Big Galaxies Are Rare! Cepheid Distance Measurement. Clusters of Galaxies. The Nature of Galaxies
Big Galaxies Are Rare! Potato Chip Rule: More small things than large things Big, bright spirals are easy to see, but least common Dwarf ellipticals & irregulars are most common Faint, hard to see Mostly
Chapter 7: From theory to observations
Chapter 7: From theory to observations Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle, predict the evolution of the stellar bolometric luminosity, effective
Supernovae with Euclid
Supernovae with Euclid Isobel Hook University of Oxford and INAF (Obs. Roma) Thanks to R. Nichol, M. Della Valle, F. Mannucci, A. Goobar, P. Astier, B. Leibundgut, A. Ealet Euclid Conference 17 18 Nov
2. Stellar evolution a crash course
2. Stellar evolution a crash course Extragalactic stellar distance indicators need to be bright advanced stages of stellar evolution Red Giant Star (SFB) Tip of Red Giant Branch (TRGB) Horizontal Branch
Stages of a Big Project ***
Stages of a Big Project *** The Five stages of SDSS: 1. Denial 2. Anger 3. Bargaining 4. Depression 5. Acceptance *** With apologies to Elizabeth Kubler Ross The Carnegie Supernovae Project Wendy Freedman
Name: unid: Foundations of Astronomy ASTR/PHYS Final Exam
Name: unid: Physical Constants * Foundations of Astronomy ASTR/PHYS 2500 Final Exam Gravitational constant G 6.673 x 10-11 m 3 kg - 1 s - 2 Elementary charge e 1.602 x 10-19 C Vacuum permittivity ε 0 8.854
Mapping the oxygen abundance in an elliptical galaxy (NGC 5128)
Mapping the oxygen abundance in an elliptical galaxy (NGC 5128) Jeremy R. Walsh, ESO Collaborators: George H. Jacoby, GMT Observatory, Carnegie; Reynier Peletier, Kapteyn Lab., Groningen; Nicholas A. Walton,
Zoccali et al. 2003, A&A, 399, 931. Overview of (old) Galactic components. bulge, thick disk, metal-weak halo. metallicity & age distribution
Chap.3 The nature of Galactic components Overview of (old) Galactic components bulge, thick disk, metal-weak halo Globular clusters metallicity & age distribution Satellite galaxies spatial and metallicity
SUPPLEMENTARY INFORMATION
1. Identification of classical Cepheids: We identified three classical Cepheids amongst the 45 short-period variables discovered. Our sample includes classical Cepheids, type II Cepheids, eclipsing binaries
Set 1: Expansion of the Universe
Set 1: Expansion of the Universe Syllabus Course text book: Ryden, Introduction to Cosmology, 2nd edition Olber s paradox, expansion of the universe: Ch 2 Cosmic geometry, expansion rate, acceleration:
The Scale of the Universe
The Scale of the Universe The Measurement of distance in our Univers! Chapters 12.1.1 Allday; Chapter 3 Silk Measurement of Distance in the Universe Two IMPORTANT concepts that you should know well from
Myung Gyoon Lee ( 李明均 )
Myung Gyoon Lee ( 李明均 ) With Observational Cosmology Team Department of Physics & Astronomy Seoul National University, Korea Nov 1-4, 2011, The 3 rd Subaru Conference/The 1 st NAOJ Symposium, Galactic
Multiconjugate Fluctuations: Measuring SBF with GeMS
Multiconjugate Fluctuations: Measuring SBF with GeMS John Blakeslee (NRC Herzberg, Victoria) & Joe Jensen (UVU) Gemini Science Meeting 18 June 2015 HST/WFC3 F160W IC3032 HST/WFC3 F160W S/N SBF in the 90s:
80 2 Observational Cosmology L and the mean energy
80 2 Observational Cosmology fluctuations, short-wavelength modes have amplitudes that are suppressed because these modes oscillated as acoustic waves during the radiation epoch whereas the amplitude of
Red giants in the halo of the SO galaxy NGC 3115: a distance and a bimodal metallicity distribution
Mon. Not. R. Astron. Soc. 286, 771-776 (1997) Red giants in the halo of the SO galaxy NGC 3115: a distance and a bimodal metallicity distribution Rebecca A. W. Elson* Institute of Astronomy, Madingley
Astronomy 102 Lab: Distances to Galaxies
Name: Astronomy 102 Lab: Distances to Galaxies You will access your textbook for this lab. Pre-Lab Assignment: As we began to talk about stars beyond the Sun, one of the most important pieces of information
Cosmology after Planck
Cosmology after Planck Raphael Flauger Rencontres de Moriond, March 23, 2014 Looking back Until ca. 1997 data was consistent with defects (such as strings) generating the primordial perturbations. (Pen,
There are three main ways to derive q 0 :
Measuring q 0 Measuring the deceleration parameter, q 0, is much more difficult than measuring H 0. In order to measure the Hubble Constant, one needs to derive distances to objects at 100 Mpc; this corresponds
ASTRONOMY II Spring 1995 FINAL EXAM. Monday May 8th 2:00pm
ASTRONOMY II - 79202 Spring 1995 FINAL EXAM Monday May 8th 2:00pm Name: You have three hours to complete this exam. I suggest you read through the entire exam before you spend too much time on any one
Review of stellar evolution and color-magnitude diagrams
Review of stellar evolution and color-magnitude diagrams The evolution of stars can be used to study the properties of galaxies Very characteristic features pinpoint at the age (chemistry) of the stars
Today: Start Ch. 18: Cosmology. Homework # 5 due next Wed. (HW #6 is online)
Today: Start Ch. 18: Cosmology Homework # 5 due next Wed. (HW #6 is online) Dark Matter! A rotation curve is a graph of how fast a something is rotating, as a function of distance from the center.! We
Astronomy C SSSS 2018
Astronomy C SSSS 2018 Galaxies and Stellar Evolution Written by Anna1234 School Team # Names 1 Instructions: 1. There are pictures of a number of galaxies in this test. However, as the DSO list for 2019
Stellar Evolution & issues related to the post Turn-Off evolution
Stellar Evolution & issues related to the post Turn-Off evolution Santi Cassisi INAF - Astronomical Observatory of Teramo, Italy The point of view of Population Synthesis users What do they want? Magnitudes
Supernova Explosions. Novae
Supernova Explosions Novae Novae occur in close binary-star systems in which one member is a white dwarf. First, mass is transferred from the normal star to the surface of its white dwarf companion. 1
The Milky Way, Hubble Law, the expansion of the Universe and Dark Matter Chapter 14 and 15 The Milky Way Galaxy and the two Magellanic Clouds.
The Milky Way, Hubble Law, the expansion of the Universe and Dark Matter Chapter 14 and 15 The Milky Way Galaxy and the two Magellanic Clouds. Image taken from the European Southern Observatory in Chile
Science Olympiad Astronomy C Division Event Golden Gate Invitational February 11, 2017
Science Olympiad Astronomy C Division Event Golden Gate Invitational February 11, 2017 Team Name: Team Number: Directions: ~Answer all questions on the answer sheet provided. ~Please do NOT access the
AS1001: Galaxies and Cosmology
AS1001: Galaxies and Cosmology Keith Horne kdh1@st-and.ac.uk http://www-star.st-and.ac.uk/~kdh1/eg/eg.html Text: Kutner Astronomy:A Physical Perspective Chapters 17-21 Cosmology Today Blah Title Current
Galaxies Guiding Questions
Galaxies Guiding Questions How did astronomers first discover other galaxies? How did astronomers first determine the distances to galaxies? Do all galaxies have spiral arms, like the Milky Way? How do
Determining distance. L 4π f. d = d = R θ. Standard candle. Standard ruler
Determining distance Standard candle d = L 4π f 1 2 d L Standard ruler d = R θ θ R Determining distance: Parallax RULER tanπ = R d π R d π R = 1AU = 1.5 10 13 cm Define new distance unit: parsec (parallax-second)
distance modulus of ^ 0.20 (Capaccioli et al. 1989), while Cepheid variables suggest that k \ ^ 0.06
THE ASTRONOMICAL JOURNAL, 115:1916È192, 1998 May ( 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE DISTANCE TO THE M31 GLOBULAR CLUSTER SYSTEM STEPHEN HOLLAND Institut
The Extragalactic Distance Scale
The Extragalactic Distance Scale Gemini Preprint #95 J. B. Jensen a, J. L. Tonry b, and J. P. Blakeslee c a. Gemini Observatory, 670 N. A ohoku Place, Hilo, HI 96720 b. University of Hawaii, Institute
arxiv:astro-ph/ v1 5 Jan 1996
A&A manuscript no. (will be inserted by hand later) Your thesaurus codes are: 01 (08.05.3; 08.08.2; 08.22.3; 11.04.1; 11.13.1) ASTRONOMY AND ASTROPHYSICS 1.2.2008 The distance modulus of the Large Magellanic
The Milky Way. Mass of the Galaxy, Part 2. Mass of the Galaxy, Part 1. Phys1403 Stars and Galaxies Instructor: Dr. Goderya
Foundations Chapter of Astronomy 15 13e Our Milky Way Seeds Phys1403 Stars and Galaxies Instructor: Dr. Goderya Selected Topics in Chapter 15 A view our Milky Way? The Size of our Milky Way The Mass of
2. Correlations between Stellar Properties
Hertzsprung-Russell (Colour-Magnitude) Diagram 2. Correlations between Stellar Properties 2.1 Mass-luminosity relationship (ZG: 12.2; CO: 7.3) Most stars obey L s = constant M s 3 < < 5 Exercise 2.1: Assuming
- M31) Biggest is Andromeda (Sb. On Galaxy Evolution Lane. Large & Small Magellanic Clouds. ASTR 1040 Accel Astro: Stars & Galaxies
ASTR 1040 Accel Astro: Stars & Galaxies Prof. Juri Toomre TA: Nicholas Nelson Lecture 24 Thur 7 Apr 2011 zeus.colorado.edu/astr1040-toomre toomre Stefan s Quintet On Galaxy Evolution Lane Look at our local
Name Midterm Exam October 20, 2017
Name Midterm Exam October 20, 2017 This test consists of three parts. For the first and second parts, you may write your answers directly on the exam, if you wish. For the other parts, use separate sheets
EVOLUTION OF DUST EXTINCTION AND SUPERNOVA COSMOLOGY
To Appear in ApJ Letters Preprint typeset using LATEX style emulateapj v. 04/03/99 EVOLUTION OF DUST EXTINCTION AND SUPERNOVA COSMOLOGY Tomonori Totani 1 and Chiaki Kobayashi 2 1 National Astronomical
The Milky Way Galaxy Guiding Questions
The Milky Way Galaxy Guiding Questions 1. What is our Galaxy? How do astronomers know where we are located within it? 2. What is the shape and size of our Galaxy? 3. How do we know that our Galaxy has
The Milky Way Galaxy
The Milky Way Galaxy Guiding Questions 1. What is our Galaxy? How do astronomers know where we are located within it? 2. What is the shape and size of our Galaxy? 3. How do we know that our Galaxy has
Phys333 - sample questions for final
Phys333 - sample questions for final USEFUL INFO: c=300,000 km/s ; AU = 1.5 x 10 11 m ; 1000 nm hc/ev ; ev/k 10 4 K; H-ionization energy is 13.6 ev Name MULTIPLE CHOICE. Choose the one alternative that
4/10/18. Our wide world (universe) of Galaxies. Spirals ~80% of galaxies
ASTR 1040: Stars & Galaxies Prof. Juri Toomre TAs: Peri Johnson, Ryan Horton Lecture 23 Tues 10 Apr 2018 zeus.colorado.edu/astr1040-toomre Our wide world (universe) of Galaxies The rich range of galaxies: