Lecture 21 updates. Hubble’s STIS Spectrograph Please include this image at the start of the images of STIS.

Slides:

Advertisements

Similar presentations

Chapter 15: The Milky Way Galaxy

Advertisements

ASTR-1020 Stellar Astronomy Day 26. Galaxy Classes.

Do your course evaluations. Only 10% of the class has completed the evaluations so far. I will add 5 points on your final exam if.

February 9, 11:00 am. The unusually bright centers found in some galaxies are called 1.active galactic nuclei. 2.starbursts. 3.halos. 4.supermassive.

Slide 1 Andromeda galaxy M31Milky Way galaxy similar to M31.

The Milky Way Galaxy Contains more than 100 billion stars Is one of the two largest among 40 galaxies in the Local Group Our Solar System is located.

AST101 The Evolution of Galaxies. Virgo Cluster Collisions of Galaxies Outside of Clusters (the field), most galaxies are spiral or irregular In dense.

The Milky Way PHYS390 Astrophysics Professor Lee Carkner Lecture 19.

© 2010 Pearson Education, Inc. Chapter 21 Galaxy Evolution.

Announcements Test solutions are posted Pick up graded work Homework 13 is due a week from today. A spreadsheet of the data is posted on the web. No class.

SIZE OF MILKY WAY Kapteyn all visible stars – 30,000 parsecs sun close to center Shapley globular clusters – 100,000 parsecs sun 2/3.

The Milky Way Galaxy 19 April 2005 AST 2010: Chapter 24.

ASTR100 (Spring 2008) Introduction to Astronomy Galaxy Evolution & AGN Prof. D.C. Richardson Sections

The Milky Way Center, Shape Globular cluster system

The Milky Way. Structure of the Milky Way The Milky Way.

Caty Pilachowski Mini-University 2013 Our Milky Way in Space and Time.

Galaxies With a touch of cosmology. Types of Galaxies Spiral Elliptical Irregular.

Levels of organization: Stellar Systems Stellar Clusters Galaxies Galaxy Clusters Galaxy Superclusters The Universe Everyone should know where they live:

Virtually all galaxies show a flat rotation curve.

The Universe PHYSICAL SCIENCE Our Place in the Universe Scale of the Universe.

Review for Exam 3.

Lecture 4. Big bang, nucleosynthesis, the lives and deaths of stars. reading: Chapter 1.

The Universe Chapter 20.

From Here to The Dawn of Time A. Herrold. To the edge of the solar system The orbit of Neptune is not at the edge of the solar system Past the planets.

The Big Stuff Galaxies The Universe and The Big Bang.

Our goals for learning How did Hubble prove galaxies lie beyond our galaxy? How do we observe the life histories of galaxies? How did galaxies form? Why.

STARS BY SEYMOUR SIMON. Stars are huge balls of hot gases Our sun is a star, and it is the star nearest our planets Earth and our solar system Other stars.

THE MILKY WAY Our Home Galaxy GALAXIES 3 Main Types Spiral/Barre d Elliptical Irregular.

STARS & GALAXIES JEOPARDY

Lecture 40 Galaxies (continued). Evolution of the Universe. Characteristics of different galaxies Redshifts Unusual Galaxies Chapter 18.6  18.9.

Classifying galaxies Big Bang Active galaxies Our Local Group Random $ 200 $ 200$200 $ 200 $400 $ 400$400 $ 400 $600 $ 600$600 $ 600 $ 600 $800 $

© 2010 Pearson Education, Inc. Chapter 21 Galaxy Evolution.

Astronomy Quiz #2 Jeopardy Review Game. GravityLife Cycle of Stars GalaxiesChallenge!The Big Bang and the Universe

Stars!!!! Galaxies and the Universe too!. Stars are far away! The closest star to Earth is the sun. The next closest is Proxima Centauri If you can travel.

January 2nd 2013 Objective Warm-Up

The Milky Way II AST 112. Interstellar Medium The space between stars is not empty! – Filled with the Interstellar Medium (ISM) Star formation is not.

Chapter 12 Space Exploration. Section 12.1 page 428 Explaining the Early Universe GALAXY – collection of stars, planets, gas and dust held together by.

GALAXIES By Christopher Wrobleski & Patrick Bradford Poole.

Chapter 12 Space Exploration. Section 12.1 page 428 Explaining the Early Universe GALAXY – collection of stars, planets, gas and dust held together by.

Galaxies with Active Nuclei Chapter 14:. Active Galaxies Galaxies with extremely violent energy release in their nuclei (pl. of nucleus).  “active galactic.

Active Galaxies and Supermassive Black Holes Chapter 17.

“OUR GALAXY” Definition of a Galaxy: a huge group of individual stars, star clusters, dust, and gas bound together by gravity.

Chapter 11 The Interstellar Medium

AST101 Lecture 20 The Parts of the Galaxy. Shape of the Galaxy.

Galaxies and the Universe Ch 25 Section 3. What are the objects in the sky? GALAXIES! Groups of stars, dust, and gases held together by gravity.

Copyright © 2010 Pearson Education, Inc. Clicker Questions Chapter 14 The Milky Way Galaxy.

Chapter 16 The Milky Way. Herschel “discovered” that we live in a disk of stars sun.

Chapter 12 Space Exploration. Section 12.1 page 428 Explaining the Early Universe GALAXY – collection of stars, planets, gas and dust held together by.

Warm Up 1) 1) Another name for the interstellar matter that will eventually form a star is ____. a.supernovac. red giant b.nebulad. black hole 2) 2) A.

Space Notes 3A Covers Objectives 6,7,8, and 9. Think About this Question: You should be able to answer this at the end of todays lesson How are the Solar.

A Long Time Ago in a Galaxy Far, Far Away…. The Milky Way Galaxy: Home Sweet Home!! Our home Galaxy is called the MILKY WAY (like the candy bar ) Our.

© 2010 Pearson Education, Inc. Galaxies. © 2010 Pearson Education, Inc. Hubble Deep Field Our deepest images of the universe show a great variety of galaxies,

AST101 Lecture 20 Our Galaxy Dissected. Shape of the Galaxy.

Chapter 21 Galaxy Evolution Looking Back Through Time Our goals for learning How do we observe the life histories of galaxies? How did galaxies.

How We See Ourselves In The Universe: A Look At The Galaxies That Surround Us.

Stars. Nebulae A nebula is a cloud of dust, hydrogen gas and plasma. The material clumps together to form a protostar. This is the first stage in the.

Chapter 20 Cosmology. Hubble Ultra Deep Field Galaxies and Cosmology A galaxy’s age, its distance, and the age of the universe are all closely related.

GALAXIES & BEYOND. What is a galaxy? A galaxy is a very large group of stars held together by gravity. Size: 100,000 ly+ Contain Billions of stars separated.

STARS!. Gravity is a force that pulls objects with mass toward each other. Gravity increases as mass increases, so the Sun has stronger gravity than the.

Stellar Evolution Continued…. White Dwarfs Most of the fuel for fusion is used up Giant collapses because core can’t support weight of outer layers any.

How fast would a galaxy 2,000 megaparsecs away be moving with respect to us, according to Hubble’s Law? Hint: H0 = 70 km/s/Mpc 1,400 km/s 14,000 km/s 140,000.

© 2017 Pearson Education, Inc.

HUBBLE DEEP FIELD:.

The “Milky Way”.

© 2017 Pearson Education, Inc.

12-3,4 Evolution of Stars.

Presentation transcript:

Lecture 21 updates

Hubble’s STIS Spectrograph Please include this image at the start of the images of STIS

Two big nearby elliptical galaxies M86 M84 Area shown on next image

title Orbit speed (km/s) Towards Blue shift Away Red shift

The Galactic Center Next Slide Check sizes 5 arcsec = 0.6 lyr Sagittarius (teapot) Galactic Center 1 deg = 450 lyr

Black Hole and Bulge Masses Correlate Black Hole Mass (M sun ) Bulge Mass (M sun ) Milky Way M32 M

Strong Gravity Near Black Holes 8000 miles kg 1 / 2 inch kg Strong gravity near black hole Modest gravity at surface crush

Accretion disks transport gas to the black hole Video-1 Milky Way black hole From Hubble Source 2005 Video-2 M84 accretion disk around black hole Also Hubble Source 2005

Quasars Show singly and fade from one to the next

Radio Galaxies Show singly and fade from one to the next

Interactions Send Gas to Center Stars and Dark Matter Only Gas Only Gas Only: Central Region

More Quasars Far Away (Long Ago) We Are Here

The Rise and Fall of Quasars Relative Number Time (Byr) Big Bang Now

The Web of Dark Matter Halos Few big More medium Many small

Halo and Galaxy Mass Distributions Dark Matter Halos (simulation) 66 Mass (solar masses) Relative Number Milky Way Giant Galaxy Dwarf Galaxy Group Galaxy Cluster

Halo and Galaxy Mass Distributions Dark Matter Halos (simulation) 66 Mass (solar masses) Relative Number Milky Way Giant Galaxy Dwarf Galaxy Group Galaxy Cluster Galaxies (data)

Halo Gravity and Suppression of Galaxy Formation Mass (solar masses) Gravity of Halo Milky Way Giant Galaxy Dwarf Galaxy Group Galaxy Cluster Gas can’t cool Active Galaxies keep gas hot Gas blown out by supernovae Gas pressure prevents collapse

Largest Dark Matter Halos text Three images stacked

Halo Gravity and Suppression of Galaxy Formation Mass (solar masses) Gravity of Halo Milky Way Giant Galaxy Dwarf Galaxy Group Galaxy Cluster Gas can’t cool Active Galaxies keep gas hot Gas blown out by supernovae Gas pressure prevents collapse

Black Hole Jets Heat the Cluster Gas Two images stacked

Halo Gravity and Suppression of Galaxy Formation Mass (solar masses) Gravity of Halo Milky Way Giant Galaxy Dwarf Galaxy Group Galaxy Cluster Gas can’t cool Active Galaxies keep gas hot Gas blown out by supernovae Gas pressure prevents collapse

Halo Gravity and Suppression of Galaxy Formation Mass (solar masses) Gravity of Halo Milky Way Giant Galaxy Dwarf Galaxy Group Galaxy Cluster Gas can’t cool Active Galaxies keep gas hot Gas blown out by supernovae Gas pressure prevents collapse

“Semi-Analytic” Galaxy Evolution Simulations 2 Byr Grey : dark matter Colored dots : galaxies

3 Byr “Semi-Analytic” Galaxy Evolution Simulations high low young old star birth rate population age 6 Byr Today Three images stacked

Simulations Include Gas Physics Dark Matter Halos (simulation) Mass (solar masses) Relative Number Milky Way Giant Galaxy Dwarf Galaxy Group Galaxy Cluster Galaxies (data) Galaxies: (simulation with gas physics)