July 26, 2004 Part I: Galaxies and Galaxy Evolution Part II: Clusters of Galaxies and Large Scale Structures July 26, 2004

Exploring the Interstellar Medium Debrief What is the interstellar medium? What do we know about its number density? What do we know the temperature of the ISM? What do we know about its heat? What is the difference between heat and temperature? Did you prove this?

July 26, 2004 Exploring the Interstellar Medium Debrief What is the Local Bubble, and what are some possibilities for how it formed? What do we know now about the event and objects in our Universe? What else do we know? Now lets move farther out… What is a galaxy?

July 26, 2004 Now lets move farther out… What do we know about galaxies? How do they evolve or form? Why do they form? How do we know? Prove it! What do our students need to know about galaxies?

July 26, 2004 Hidden Lives of Galaxies Read the first 2 pages of the handout Get into six groups of four Every group must have access to a wall with a poster Use the poster the answer the questions that are asked on the handout. (page 6)

July 26, 2004 M31/Andromeda Our nearest spiral neighbor 2 million light years away Center of M31 has two optical nuclei

July 26, 2004 M31/Chandra X-ray Image of central part of our neighbor M31 Bright X-ray sources are binaries with black holes or neutron stars Central BH is very cool, 30 million M o Center of M31

July 26, 2004 Edge-on Spiral Galaxy NGC we think our Galaxy looks like this This is an infrared composite image from KPNO

July 26, 2004 Starburst galaxies Galaxies which are undergoing rapid phase of star formation Supernova rate about 10 times higher Many bright stars Fluorescent gas clouds GRBs are in burst region. NGC 4214 HST

July 26, 2004 Starburst Galaxy M82 Radio map is CO which traces H IR map shows proto-stars Radio IR

July 26, 2004 Starburst galaxy M82 X-ray evidence for intermediate mass black hole in M82 High supernova rate makes many smaller black holes, which may merge

July 26, 2004 Hidden Lives of Galaxies In the same groups as before… Read page 7 Read and follow the instructions on page 8

July 26, 2004 The Hubble Fork Diagram

July 26, 2004

Galaxy Formation movie Formation of galaxies in universe

July 26, 2004 Hidden Lives of Galaxies Once again in your same groups… Read page 9 Ok now based on all of the characteristics of the different types of galaxies. Now it is your turn to match the unusual galaxies with the names on the right. (page 10) Make sure you give reasons why you choose the name. Continue reading pages 11-12, 13,and 22.

July 26, 2004 Break Which came first, the galaxy or its central black hole?

July 26, 2004 Active Galaxies Now get into groups and lets talk about the GLAST Active Galaxies Poster Discussion topics: –What is it explaining? –Why does science care? –How do these objects “fit in”? –What is the scientific evidence for these objects? –What are the of the different objects on this poster? –Similar and dissimilar characteristics?

July 26, 2004 An Active Galaxy Journey

July 26, 2004 Unified Model of AGN All AGN are the same: central BH plus disk and jets Differences in lines, jets, & spectra are due to different viewing angles Also possible that BHs are being fed at different rates

July 26, 2004 Galaxies and Black Holes Zooming in to see the central torus of an Active Galaxy. Jet Accretion disk Black Hole

July 26, 2004 Radio Lobe Galaxy Radio lobes (Q-tips) Jet Accretion Disk

July 26, 2004 Two Views of an Active Galaxy View at an angle to jet View at 90  from Jet Radio Lobe GalaxySeyfert Galaxy

July 26, 2004 Seyfert Galaxy NGC 7742 Bright nucleus 3000 light years across 72 million light years away HST

July 26, 2004 Centaurus A/Optical Giant elliptical galaxy 10 million light years away Dark dust lane obscures the central region

July 26, 2004 Centaurus A/Radio Double Lobe Radio Galaxy Image shows radio lobes superposed on optical image Central black hole must be producing radio jets and lobes

July 26, 2004 Centaurus A/X-ray X-ray image from Chandra Bright nucleus can be seen in center at location of black hole Small jet to lower right ends in shocked region

July 26, 2004 Centaurus A/IR IR map shows a second galaxy (barred spiral) hiding inside Cen A’s dust lanes Elliptical’s gravity helps barred spiral maintain its shape Material funneled along the spiral's bar fuels the central black hole which powers the elliptical's radio lobes Symbiotic relationship

July 26, 2004 M87 Optical Giant elliptical galaxy At center of Virgo cluster Many globular clusters surround it Little dust and gas in the galaxy 50 million light years away

July 26, 2004 M87 HST Movie

July 26, 2004 M87 Optical Jet HST IR and UV composite Globular clusters also seen Note shock waves and knot patterns in jet Bright point at central black hole

July 26, 2004 M87 Radio Jet Central black hole is making jets Jets are making bubbles of hot gas Bubbles are as big as 200,000 light years Smallest resolution VLBI image is 0.2 light years

July 26, 2004 M87 X-ray and radio X-ray contours on radio image High energy emission from central black hole ROSAT X-ray data

July 26, 2004 Another view of an Active Galaxy Looking down the Jet From this view, we see the Active Galaxy emitting gamma rays and X-rays. Blazar Galaxy Quasar 3C279

July 26, 2004 Gamma-ray Quasars 3C 279 is a very bright, repeatedly flaring gamma- ray source, seen at MeV - TeV energies 3C273 is much brighter at optical energies 3C279 3C273

July 26, 2004 Blazar movie Shows rotating black hole in the center of Active Galaxy, which is emitting relativistic jets of material Blazar is a quasar that is aiming its beams directly at us

July 26, 2004 Most distant QSOs Redshift record is now around Z=6.5 Sloan Digital Sky Survey Z = 5.0 Z = 4.75Z = 4.9

July 26, 2004 Galaxy Collision

July 26, 2004 Galaxy Collisions, Part 2

July 26, 2004 Cartwheel Galaxy Wheel shape was formed from collision of two galaxies Bright stars are forming at the edges of the wheel (10 5 light years in diameter) Intruder galaxy is no longer visible This is from HST

July 26, 2004 How the Galaxy got its jets

July 26, 2004 Active Galaxies and Jets What do Active Galaxies look like when viewed from different distances?

July 26, 2004 Reflection and Debrief Now what do we know? What are the big ideas here? What do our students need to know? Is there anything else we need to know? Misconceptions (take notes)

July 26, 2004 Reflection and Debrief What are some effective ways to teach students about galaxies and how they evolve? Standards??? (take notes)

July 26, 2004 Break Which came first the galaxy or the clusters?

July 26, 2004 Engage Examine the photograph of the Hubble Deep Field and the histogram of galaxies Fill out the worksheet Demo of the CLEA Wedge activity CLEA wedge plots

July 26, 2004 Wedge Plot Activity These data are from CLEA’s LSS lab Plot them on the wedge plot How many clusters do you see? Why is the wedge plot a better representation of the measurements than the linear plot?

July 26, 2004 “Stickman” “Slice” –style Redshift survey pioneered by Margaret Geller, Marc Davis and John Huchra  Distance is plotted vertically as given by redshifts The body of the stickman is due to the Coma cluster His arms form “walls”

July 26, 2004 Las Campanas Survey  Done by Shectman et al.  Largest redshift survey  Clearly shows walls and voids  75-80% of space is devoid of bright galaxies  Typical distance between 2 galaxies is around 7.5 Mpc  Typical distance between 2 clusters is around 20 Mpc

July 26, 2004 Clusters of Galaxies Clusters of galaxies are the largest gravitationally bound systems in the universe, with sizes of a few Mpc (a Mpc is about 3 million light-years). A typical cluster contains hundreds or thousands of galaxies Most of the mass is in the form of a hot intracluster gas, which is is heated to high temperatures ( K or several keV) Clusters are rare objects: fewer than 1 in 10 galaxies in the universe resides in clusters

July 26, 2004 Types of Galaxy Clusters Regular clusters – concentrated central core – well-defined spherical structure – often dominated by a giant galaxy – usually quite rich, M~10 15 M o –most galaxies are elliptical or lenticular Irregular clusters –no well-defined center –~half the galaxies are spirals –Often contain subclusters –Probably not steady state

July 26, 2004 Distances to Galaxy Clusters Going beyond Cepheid Variables to the next rungs on the Cosmic Distance Ladder Brightest Cluster Galaxies: The brightest galaxy in a cluster of galaxies has been used as a standard candle. But: rich clusters with many galaxies will probably have the most luminous galaxies even though these galaxies are very rare, while the brightest galaxy in less rich clusters are probably not as bright

July 26, 2004 X-ray emission from Clusters  Gas in clusters of galaxies is held by mass where:  Mass of hot gas is more than 3 times the mass of the visible light galaxies in the Virgo cluster  Strongest X-rays are around M87 Virgo/ROSAT M = V 2 R G

July 26, 2004 Cluster Formation Formation and evolution of a galaxy cluster (from T6 group at Los Alamos)  Evolution of a Cd galaxy cluster (from John Dubinski at CITA) movies

July 26, 2004 Galaxy Harassment Spirals merge to form ellipticals Biggest elliptical cannibalizes the others to form one giant elliptical in the center of the cluster Dwarf ellipticals are formed by harassment (high velocity encounters) of low-mass spirals Detectable arcs of debris are left over – providing fuel for quasars

July 26, 2004 Virgo cluster of galaxies  The Virgo cluster of galaxies is about 65 million light years away  It contains about 2500 galaxies  It is dominated by M87 M87

July 26, 2004 Virgo Cluster It is the nearest rich cluster of galaxies Classification - irregular Covers about 100 o of sky or at its distance it spreads out over tens of millions of light years Recessional velocity is about 0.3% of velocity of light X-ray emission concentrated around individual galaxies, particularly M84 and M86 The strong radio galaxy M87 in the Virgo cluster is also a strong source of X-rays

July 26, 2004 Perseus Cluster  One of the closest galaxy clusters at a distance of 300 million light years  Part of the Perseus Pisces supercluster which is 15 degrees across and has over 1000 galaxies

July 26, 2004 Hydra Cluster  Distance of 840 million light years  Several hundred galaxies in the cluster  35 million degree gas in center rising to 40 million in the outside  Several million light years across the gas cloud Optical/La Palma

July 26, 2004 Hydra Cluster Radio/NRAO X-ray/Chandra

July 26, 2004 Coma Cluster  Coma cluster has about 1000 galaxies  It is located near the north galactic pole  It is about 250 million light years away (80 Mpc)  Large bright central cluster is merging with smaller galaxy group at the lower right 3 Mpc

July 26, 2004 Small Cluster  X-rays from this smaller cluster were discovered by ROSAT  Hot gas engulfs the two bright elliptical galaxies  It is about 500 million light years away

July 26, 2004 Very Distant Cluster  This is a very red cluster, located at Z~1  It is the most distant cluster discovered by HST  It may be too far away to have formed in a dense universe

July 26, 2004 Very Distant Cluster  This cluster is 8 billion light years away, so it formed when the universe was half its present age  It is also very red  It should not exist if the Universe is dense

July 26, 2004 How clusters affect galaxy evolution Ram pressure and turbulent stripping of gas from a spiral galaxy as it falls through the hot ICM of a rich galaxy cluster (by Vicent Quilis with Ben Moore) The galaxy model is 3d with a stellar disk, bulge + dark matter halo. The colours show the gas density in a thin slice centered on the disk movie

July 26, 2004 Merging Clusters  A2142 cluster  The 50 million degree gas is coolest in the center where two clusters have finished merging  The gas outside the center is 100 million degrees – heated by the collision  Chandra image

July 26, 2004 Cannibal Cluster  A3827 is about 1.5 billion light years away  The central dominant galaxy is eating five smaller galaxies ESO/Optical

July 26, 2004 Large Scale Structure Distribution of matter in the Universe on scales at or above 10 Mpc Can be determined by –Galaxy surveys –Lyman-alpha forest studies –Quasar clustering studies Superclusters are largest structures seen – but they are not gravitationally bound

July 26, 2004 Local Supercluster  The Local supercluster contains the Virgo cluster of galaxies as well as about 50 galaxy groups

July 26, 2004 Superclusters Superclusters usually have 3-10 clusters of galaxies They are not gravitationally bound Our local supercluster contains the Virgo cluster (at 16 Mpc) and extends about Mpc Local Supercluster

July 26, 2004 Walls and Voids Universe looks like soap bubbles in 3D Galaxies occur on the bubble surfaces Superclusters are formed where bubbles merge Walls are made of elongated superclusters – the largest is the “Great Wall” - about 100 Mpc in length at a distance of 100 Mpc Voids are about 100 Mpc in diameter – are 90% of space Clusters of galaxies are bright spots on the walls

July 26, 2004 Flyby universe movie Las Campanas data – notice the walls and voids as you fly by

July 26, 2004 Formation of Large Scale Structure Simulation by Martin White shows the evolution of structure starting with fluctuations in the Cosmic Microwave Background movie

July 26, 2004 The End of Greatness Most recent surveys are so large that the largest structures (about 100 Mpc) are smaller than the survey size This is a 200 Mpc simulation from Ben Moore (using  CDM)

July 26, 2004 Where are we going?  The Milky Way Galaxy is falling towards the Virgo cluster at ~300 km/s  The Virgo cluster is falling towards the Hydra- Centaurus supercluster also at ~300 km/s But the Hydra- Centaurus cluster is also falling towards something…..

July 26, 2004 Great Attractor  ~10 16 solar masses concentrated 65 Mpc away in the direction of Centaurus Abell 3627 near the Great Attractor  The “Great Attractor” seems to be pulling in the Hydra-Centaurus super-cluster  But only 10% that amount of visible matter can be seen!

July 26, 2004 What do we know about our Universe? Using the chart found on page 23 of the handouts fill in the blanks to all the components of a galaxy. What do we know about the Universe now?

July 26, 2004 Reflection and Debrief Now what do we know? What are the big ideas here? What do our students need to know? Is there anything else we need to know? Misconceptions (take notes)

July 26, 2004 Reflection and Debrief What are some of the effective ways to teaching these topics? Standards??? (take notes)

July 26, 2004 Web Resources (galaxies) A. Ptak’s intermediate mass black hole in M82 T. di Matteo’s X-ray quiet AGN glast.sonoma.edu/HEADmeeting/tuesday/index.html ROSAT X-ray images 000/oct 000/oct NCSA’s Unveiling the Hidden Universe ml#Unveiling

July 26, 2004 Web Resources (galaxies) Astronomy picture of the Day Imagine the Universe M87 radio images Space Telescope Science Institute Sloan Digital Sky Survey

July 26, 2004 Web Resources (galaxies) NCSA M82 images Gal.html Galaxy Formation Movie from NCSA eWorksMovies.html

July 26, 2004 Web Resources (LSS) On-line Journey through Astronomy J. C. Evans Astronomy 103 Course Notes/Html/Lec08/Lec08_pt1_universeClusters.htm Notes/Html/Lec08/Lec08_pt1_universeClusters.htm Martin White’s Large Scale Structure XMM-Newton Large Scale Structure Survey

July 26, 2004 Web Resources (LSS)  Ned Wright’s ABCs of Distance  Ray White’s Cluster of Galaxies Mug Shots  Cambridge Cosmology Pages  Greg Bothun’s Cosmology Book ntents.html ntents.html  J. Cohn’s Lyman alpha Forest pages

July 26, 2004 Web Resources (LSS)  T-6 Group at LANL animations and picture  John Dubinski’s Big cluster simulations  2DF redshift survey project  Ben Moore’s N-body simulations