Lecture 18 Stellar populations. Stellar clusters Open clusters: contain 10-1000 stars loose structure Globular clusters: 1000 - 1 million stars centrally.

Slides:



Advertisements
Similar presentations
Stellar Clusters are groups of stars, smaller than and contained in galaxies NGC 6791 is one of the oldest and largest star clusters known. The open star.
Advertisements

Outline of Ch 11b: The H-R Diagram
Susan CartwrightOur Evolving Universe1 Understanding Stars n What do we know? n From observations of nearby stars: l l luminosity/absolute magnitude l.
ASTR112 The Galaxy Lecture 3 Prof. John Hearnshaw 5. Stellar populations 6. Galactic (open) clusters The Pleiades open cluster.
The Milky Way Galaxy part 2
PHYS390 (Astrophysics) Professor Lee Carkner Lecture 14
Variable Stars: Pulsation, Evolution and applications to Cosmology Shashi M. Kanbur SUNY Oswego, June 2007.
Properties of Stars II The Hurtzprung-Russell Diagram How long do stars live? Star clusters.
The Milky Way Galaxy 19 April 2005 AST 2010: Chapter 24.
Chapter 11 Surveying the Stars Properties of Stars First let see how we measure three of the most fundamental properties of stars: 1.Luminosity.
Properties of Main Sequence Stars Masses Luminosities Lifetimes Distribution.
Chapter 11c Surveying the Stars Star Clusters Our Goals for Learning What are the two types of star clusters? How do we measure the age of a star.
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide.
Galaxies Chapter 16. Galaxies Star systems like our Milky Way Contain a few thousand to tens of billions of stars. Large variety of shapes and sizes.
Galaxies Chapter 13:. Galaxies Contain a few thousand to tens of billions of stars, Large variety of shapes and sizes Star systems like our Milky Way.
Part 5: The Galaxy and the Universe In this final part of the course, we will: 1. Look at the big spatial picture: Are there organizations of stars? What.
Chapter 11 Surveying The Stars Surveying The Stars.
Another galaxy: NGC The Milky Way roughly resembles it.
End of Ch. 13 III. Cycle of Birth and Death of Stars: Interstellar Medium Ch. 14.
The Milky Way Appears as a band of light stretching across the sky There are dark regions along the band, giving the appearance of a lack of stars This.
Ch. 14. The Milky Way Ch. 14. Ch. 14 OUTLINE Shorter than book 14.1 The Milky Way Revealed 14.2 Galactic Recycling (closely related to Ch. 13) 14.3 The.
Star Clusters and their stars Open clusters and globular clusters General characteristics of globular clusters Globular cluster stars in the H-R diagram.
Measuring the Stars How big are stars? How far away are they?
Susan CartwrightOur Evolving Universe1 The Milky Way n From a dark site the Milky Way can be seen as a broad band across the sky l l What is it?   telescopes.
Lecture Outlines Astronomy Today 8th Edition Chaisson/McMillan © 2014 Pearson Education, Inc. Chapter 25.
Galaxies Astronomy 115. First, which of the following is a galaxy? Open cluster Globular cluster Nebula Interstellar medium (gas and dust) Supernova remnant.
© 2010 Pearson Education, Inc. Chapter 21 Galaxy Evolution.
Galaxies GALAXY -comes from the ancient Greeks and their word for “milk”- galactos.
Chapter 11 Surveying the Stars Properties of Stars Our Goals for Learning How luminous are stars? How hot are stars? How massive are stars?
Observing Stellar Evolution 1. How can we see stellar evolution in action? 1. Stellar Clusters, a group of coeval stars, I.e. all born at the same time,
The Milky Way – A Classic Spiral Galaxy Here’s the mystery story we’ll unfold… Fuzzy blobs in the sky – new solar systems, or “galaxies”? Observational.
When Giovanni Riccioli used a telescope like this one to observe a star in the handle of the Big Dipper, he discovered two stars that orbit each other.
Quiz #6 Most stars form in the spiral arms of galaxies Stars form in clusters, with all types of stars forming. O,B,A,F,G,K,M Spiral arms barely move,
A note on: Group Behavior Open Clusters: contain a few hundred to a few thousands of stars. Lie in the plane of the Milky Way Galaxy. A few parsecs in.
Dept. of Astronmy Comparison with Theoretical CM diagram Galactic Astronomy #6.1.3 Jae Gyu Byeon.
Stars.
Goal: To understand clusters of stars Objectives: 1)To explore Some nearby clusters 2)To understand How clusters in our galaxy form 3)To understand Globular.
Stellar Clusters Homework Problems Chapter 13
Binary stars and clusters Chapter 11. Review Properties of stars –apparent brightness (apparent magnitude) measure energy/area/second –luminosity (absolute.
Globular Clusters. A globular cluster is an almost spherical conglomeration of 100,000 to 1,000,000 stars of different masses that have practically.
Chapter 13: Star Clusters Open cluster globular cluster Stars (almost) always form in clusters The stars all formed at the same time They are all at the.
Stellar Evolution: After the Main Sequence. A star’s lifetime on the main sequence is proportional to its mass divided by its luminosity The duration.
June 5, 2006 AAS/Calgary Stellar Populations: Old Stars in the Nearest E Galaxy From Field Stars to Globular Clusters.
- HW Ch. 10, EXTENDED Mon. Nov. 8 - HW Ch. 11 & 12, due Mon. Nov HW Ch. 13 & 14 due Mon. Nov. 22 Exam 3 on Tuesday Nov. 23.
Blue stragglers in dwarf spheroidal galaxies L.Rizzi Osservatorio Astronomico di Padova In collaboration with: Enrico V. Held, Giampaolo Bertelli, Ivo.
Star Clusters. Two Main Types of Cluster 1. OPEN:  relatively young  often sparse (a few hundred stars)  scattered about, no obvious symmetry Example:
Measuring the Stars What properties of stars might you want to determine?
A105 Stars and Galaxies  Homework due today  Remote observing this weekend Today’s APODAPOD.
1 The “ Local Group ” of Galaxies Two large spiral galaxies Milky Way & Andromeda (Messier 31 or M31) Distance between them: D = 700 kpc = 2.3 x 10 6 light.
ASTR112 The Galaxy Lecture 4 Prof. John Hearnshaw 7. Globular clusters 8. Galactic rotation 8.1 From halo stars 8.2 From disk stars – Oort’s constant,
The Formation and Evolution of Galaxies Michael Balogh University of Waterloo.
Chapter 25 Galaxies and Dark Matter. 25.1Dark Matter in the Universe 25.2Galaxy Collisions 25.3Galaxy Formation and Evolution 25.4Black Holes in Galaxies.
Universe Tenth Edition Chapter 19 Stellar Evolution: On and After the Main Sequence Roger Freedman Robert Geller William Kaufmann III.
Stellar Evolution Please press “1” to test your transmitter.
Unit 2 - Cosmology Part 1: Stars Part 2: Galaxies Part 3: Origin and Evolution of the Universe.
“Globular” Clusters: M15: A globular cluster containing about 1 million (old) stars. distance = 10,000 pc radius  25 pc “turn-off age”  12 billion years.
Globular Clusters Globular clusters are clusters of stars which contain stars of various stages in their evolution. An H-R diagram for a globular cluster.
Hertzsprung–Russell diagram review. Temperature Luminosity An H-R diagram plots the luminosities and temperatures of stars.
Measuring the Stars How big are stars? How far away? How luminous?
Beyond Our Solar System – The Universe in a Nutshell!
The Milky Way Galaxy.
III. Cycle of Birth and Death of Stars: Interstellar Medium
Clusters Clusters and Age Stars are born from molecular clouds
Galaxies.
When Giovanni Riccioli used a telescope like this one to observe a star in the handle of the Big Dipper, he discovered two stars that orbit each other.
Star Clusters and their stars
When Giovanni Riccioli used a telescope like this one to observe a star in the Big Dipper, he discovered two stars that orbit each other. A group of stars.
Galaxies.
Stellar Clusters are groups of stars, smaller than and contained in galaxies The open star cluster (NGC 2244) was discovered in 1690 by English astronomer.
Stellar Clusters are groups of stars, smaller than and contained in galaxies The open star cluster (NGC 2244) was discovered in 1690 by English astronomer.
Presentation transcript:

Lecture 18 Stellar populations

Stellar clusters Open clusters: contain stars loose structure Globular clusters: million stars centrally concentrated S imple stellar populations: stars were probably all born at nearly the same time; thus have the same age and composition ~5 pc

Galaxies contains billions of stars stars generally have a variety of ages, compositions ~20,000 pc

Globular clusters Mostly found in the halo of the Milky Way  Concentrated around the Galactic centre  In fact their spatial distribution was first used to identify the centre of the Galaxy Globular clusters: Open clusters Mostly found in the disk of the Milky Way Open clusters

Stellar systems Galaxy groups: A few tens of galaxies in orbit about one another Galaxy clusters: Thousands of galaxies, trillions of stars The largest bound structures in the Universe ~5x10 5 pc ~2x10 6 pc

Review: Stellar Evolution Main sequence: Core hydrogen burning Red Giant branch: Shell-hydrogen burning Horizontal branch: Core helium burning Asymptotic Red Giant branch: Shell helium (and hydrogen) burning, around a CO, electron degenerate core

Isochrones and Evolutionary tracks For a collection of stars with a range of masses, we can plot where they will be at a given time: these are isochrones. Models for different ages For a given mass, we can model how it will evolve with time Models for different masses log 10 (age/yr)

Single-aged populations Nearby stars of all agesCluster of stars all formed at the same time.

Star clusters The colour-magnitude diagram of a cluster contains information about the age and composition of a cluster. Evolutionary tracks for stars of different masses HB RGB MS

Star clusters The colour-magnitude diagram of a cluster contains information about the age and composition of a cluster. Isochrones for stars of a fixed age

Theoretical Isochrones Age The main sequence turnoff is a good indicator of cluster age.

Theoretical Isochrones Stars with more heavy elements (metal-rich) tend to be redder. Metallicity Distance The magnitude of the turnoff depends on distance The colour depends on metallicity

Theoretical Isochrones Stars with more heavy elements (metal-rich) tend to be redder. Metallicity Distance Oxygen abundanceAge The magnitude of the turnoff depends on distance The colour depends on metallicity The main sequence turnoff is a good indicator of cluster age.

Colour-magnitude diagrams A young cluster:  The main sequence is the most prominent structure.  There has not been enough time for stars to leave the main sequence

Open clusters Example: The Hyades cluster Spectral type B-VAge (10 9 yr) O-0.4<0.001 B A F0.54 G0.710 K1.060 M1.6>100 The colour of the brightest main sequence stars is (B-V)~0.1 This corresponds to an A0 star.

Open clusters typically young, and metal-rich <1 billion years old Mostly found in the disk of the Milky Way NameAge (Myr) Distance (pc) [Fe/H] Collinder Melotte n Melotte Mamajek Melotte Platais Melotte IC Platais Platais The ten nearest known open clusters

Globular clusters 47 Tucanae Old clusters:  Only the faintest (low-mass) stars are still on the main sequence.  Most of the stars on the CMD are in post-main sequence phases of evolution

NGC2419 In old clusters, the bright blue stars are horizontal branch stars, while the yellow-red stars are giants

Globular clusters For a given composition and distance, find the model age that gives the best fit to the data. Here, isochrones are shown for ages of 8,10,12,14,16,18 Gy.

Globular clusters Example: M92  Best fit model:  age=14 Gyr.  [Fe/H]=-2.31

Globular clusters Isochrones for 8,10,12,14,16,18 Gyr ages in each panel, shown for different compositions and distances.

Cluster ages Model isochrone fits to various different open and globular clusters Shows the range of ages and HR-diagram morphologies spanned by these objects

Observational Difficulties

Observational difficulties Finite width of the main sequence and turn-off Presence of blue- stragglers  Probably binary mergers

Break

Other galaxies The Milky Way and Andromeda are the largest members of the Local Group of Galaxies  There are about ~30 smaller galaxies, with distances of up to about 1 Mpc away.

Local Group galaxies For some galaxies in the Local Group, it is possible to measure the colours and magnitudes of individual stars Consider an intermediate age stellar population, 4 Gyr old. Assuming a solar metallicity, what is the absolute magnitude of the main-sequence turnoff? What would be the apparent magnitude of the turnoff, in the Andromeda galaxy (~800 kpc away)?

Local Group galaxies Most main sequence stars are too faint to be seen, so the colour-magnitude diagrams are dominated by evolved stars It is not usually a good approximation that all stars formed at the same time

Composite stellar populations Need a range of model ages, metallicities to match the width of the main- sequence turnoff.

Outside the Local Group For more distant galaxies, we can only measure the integrated luminosity and colour of all stars. How will the colour and luminosity of a single burst of star formation changes with time?

Outside the Local Group For more distant galaxies, we can only measure the integrated luminosity and colour of all stars. How will the colour and luminosity of a single burst of star formation changes with time?

Elliptical galaxies The easiest ones to model Pretty well modeled by single age, metallicity Models which use high-resolution spectra of stars do a good job of reproducing features in the galaxy spectrum These models show elliptical galaxies tend to be old  Have formed most of their stars at least ~10 billion years ago  Metallicities are about solar or a bit less

Spiral galaxies Generally have stars with a wide range of ages and metallicites  Usually modeled with continuous star formation (the rate may increase or decrease with time).  Different components (bulge, disk, halo) have different stellar populations.