KIAA Lectures Beijing, July 2010 Ken Freeman, RSAA, ANU

1. KIAA Lectures Beijing, July 2010 Ken Freeman, RSAA, ANU Lecture 1: Introduction

2. What does our Galaxy look like ? Near infrared image from COBE/DIRBE - dust is transparent in near-IR NGC 891: our Galaxy probably looks much like this in visible light

3. The Milky Way is a disk galaxy: the disk is the primary stellar component Also see a small central bulge We would like to understand how our Galaxy came to look like this Some galaxies have much larger bulges

4. dark halo stellar halo thick disk thin disk bulge Overview of our Galaxy

5. Each one of these components has something to tell us about its formation history Our task is to understand how the formation and evolution of the Milky Way took place: how does it compare with the predictions of CDM simulations ?

6. The thin disk is metal-rich and covers a wide age range The other stellar components are all relatively old (note similarity of [Fe/H] range for thick disk and globular clusters)

7. Total mass ~ 2 x 1012 M : Wilkinson & Evans (1999), Sakamoto et al (2003) Stellar mass in bulge 1 x 1010 M disk 6 x 1010 M stellar halo 1 x 109 M Ages of components: globular clusters ~ 10-12 Gyr thick disk : > 10 Gyr thin disk : star formation started about 10 Gyr ago and star formation in the disk has continued at a more or less constant rate to the present time

8. How did the Galaxy come to be like this ? To study the formation of galaxies observationally, we have a choice ... we can observe distant galaxies at high redshift : we see the galaxies directly as they were long ago, at various stages of their formation and evolution but not much detail can be measured about their chemical properties and motions of their stars so we cannot follow the evolution of any individual galaxy

9. or we can recognise that themain structures of our Galaxy formed long ago at high redshift. the halo formed at z > 4 the disk formed at z ~ 2 We can study the motions and chemical properties of stars in our Galaxy at a level of detail that is impossible for other galaxies, and probe into the formation epoch of the Galaxy. This is near-field cosmology

10. The ages of the oldest stars in the Galaxy are similar to the lookback time for the most distant galaxies Both give clues to the sequence of events that led to the formation of galaxies like the Milky Way

11. MOVIE Now show a numerical simulation of galaxy formation. The simulation summarizes our current view of how a disk galaxy like the Milky Way came together from dark matter and baryons • much dynamical and chemical evolution • halo formation starts at high z • dissipative formation of the disk

12. Simulation of galaxy formation • cool gas • warm gas • hot gas

13. Movie synopsis •z ~ 13 :star formation begins - drives gas out of the protogalactic mini-halos. Surviving stars will become part of the stellar halo - the oldest stars in the Galaxy • z ~ 3 :galaxy is partly assembled - surrounded by hot gas which is cooling out to form the disk • z ~ 2 :large lumps are falling in - now have a well defined rotating galaxy.

14. The movie showed the formation and evolution of a large spiral in a CDM simulation. What does each component of the Milky Way contribute to our understanding of the formation and evolution of disk galaxies in the CDM context ? Living inside the Milky Way has advantages and disadvantages. The Milky Way will be very good for assessing some CDM issues and not so good for others

15. What are the issues with galaxy formation in CDM in the context of what our Galaxy can contribute towards understanding these issues? • Structure of the inner dark halo - core or cusp • Number of predicted satellites • Forming disks with small bulges in CDM • Active accretion history • Baryonic angular momentum

16. NFW What are the issues with galaxy formation in CDM ? • Structure of the inner dark halo - core or cusp Simulations predict cusp, observers claim core Distribution of inner slope of density  ~ r Very long argument !! eg de Blok et al 2002: sample of about 60 LSB galaxies optical rotation curves give inner slope of density distribution NFW halos have  = -1 Flat cores have  = 0

17. What are the issues with galaxy formation in CDM ? • Number of predicted satellites From simulations, we would expect a galaxy like the Milky Way to have ~ 500 satellites with bound masses > 108 M. These are not seen optically or in HI. New very faint satellites are being discovered but unlikely to find 500 Are there large numbers of dark satellites ? Are some (or all) globular clusters the nuclei of accreted fragments ? B. Moore et al

18. What are the issues with galaxy formation in CDM ? • Forming disks with small or no bulges in CDM It is currently difficult for CDM to generate galaxies with small or no bulges. Understanding how the bulge of the Galaxy formed is important for this problem

19. Small bulges are thought to be generated by instability processes within disks, rather than by merger activity. If that is correct, then an even larger fraction of disk galaxies were born without bulges, and the problem of forming pure disk systems becomes even more evident (more in lecture on the bulge)

20. Sgr NGC 5907 What are the issues with galaxy formation in CDM ? • CDM predicts an active ongoing accretion history, leaving debris of accreted satellites in the stellar disk and halo. (The first stars probably came from small dense accreted systems which formed before the Milky Way itself). A very active accretion history may be inconsistent with the presence of a dominant thin disk. Epoch of last major merger is particularly important for disk survival. We are uniquely located in the Milky Way to evaluate accretion history of a large spiral and measure the distribution of its first stars Chou APOD

21. What are the issues with galaxy formation in CDM ? • Baryonic angular momentum in context of angular momentum loss from baryons to dark halo via hydrodynamical and gravitational effects. Old problem, that baryons have predicted to have less angular momentum than observed: seems to be less of a problem with higher resolution simulations (eg Kaufmann et al 2007, Governato et al 2007). Observationally probably better studied in other galaxies

22. • Baryon acquisition is needed to fuel ongoing star formation, which would exhaust the current gas supply on a timescale ~ 1 Gyr. How is this happening ? Is it related to the accretion history, high velocity HI clouds, the galactic warp ? Is it gas that was previously ejected from the disk ? Milky Way is potentially well suited to investigate baryon acquisition.

23. Reconstructing galaxy formation We would like to reconstruct the whole process of galaxy formation, as the Galaxy comes together from the CDM hierarchy. What do we mean by the reconstruction of Galaxy formation ? We want to understand the sequence of events that led to the Milky Way as it is now.Ideally, we would like to tag or associate the visible components of the Galaxy to partsof the proto-galactic hierarchy : i.e. to the baryon reservoir which fueled the stars in the Galaxy. This seems too difficult. In the process of galaxy formation and evolution from the CDM hierarchy, a lot of information about the proto-galactic hierarchy is lost. Now discuss how information is lost during galaxy formation and evolution.

24. Epochs when information about the proto-hierarchy is lost: • As dark matter virialises • As baryons dissipate within the dark halo to form the disk and bulge • As the disk restructures to form the bulge (if that is the way it formed) • Subsequent accretion of objects from the environment : information is lost, though some traces remain. • During the evolution of the stellar disk, as orbits are scattered by dynamical processes - resonances, molecular clouds … At each epoch, some information remains: what does the Galaxy remember ? What can we hope to discover with Galactic Archaeology ?

25. Signatures remembered from each epoch • Zero order: since dark matter virialised: • First order: since main baryon dissipation epoch • Second order: subsequent evolution (This is idealized: galaxy formation is an ongoing process) In later lectures, we will look at • ways in which we can derive information about the early Galaxy, and • some of the processes that cause loss of information or provide bogus information for us to misinterpet.

26. Zero order signatures (since dark matter virialization) The virialization phase is dominated by merging and violent relaxation. Early stars form in small elements of the hierarchy - some will become the stars of the metal-poor halo. The total binding energy E, mass M and angular momentum parameter where J is the angular momentum, are more or less established at this phase, although they continue to evolve slowly: E, M and J determine the gross nature of the galaxy. The globular cluster system formed around this time: its underlying structure has probably not changed much, though a lot of the clusters were destroyed. Note that old GCs in Milky Way, LMC and nearby Fornax dwarf spheroidal galaxy have similar ages within 1 Gyr. GCs in interacting systems like the Antennae indicate that GC formation is associated with interaction, as in this very early phase.

27. Some of the properties of the metal-poor stellar halo were probably established in this epoch, as small satellites which had already formed stars were accreted by the virializing halo The Tully-Fisher law which relates the rotational velocity and the baryon mass of galaxies, is also probably established at this phase.

28. Massive young clusters in NGC 4038/9

29. Massive cluster formation in NGC 4038/9

30. Sakai McGaugh HIPASS The Tully-Fisher law for disks (baryonic = stars + neutral gas) slope 3.8 ± 0.1 slope 3.2 ± 0.1 stellar baryonic Gurovich et al 2010

31. First order signatures What information remains from the epoch when baryons dissipated to form disk (and maybe the bulge) ? The scale length of the disk may be roughly constant since then. The mass of the disk continues to grow as gas falls in and stars form. Chemical gradients in old components like the thick disk may be conserved but are probably affected by radial mixing of stars by disk heating, spiral arms. The vertical scale height of the old disk evolves with disk heating, at least for a few Gyr, but is probably roughly constant after ~ 3 Gyr from birth, so we see old disk as it was about 7 Gyr ago.

32. The old thick disk may have been heated by accretion long ago, or formed long ago in a gas-rich merger (Brook et al 2007): it is probably much as it was after birth. It is one of the most important fossil remnants. Thick disk stars form rapidly in merger, thin disk stars form later Brook et al 2007

33. The bulge has probably not changed much since its formation. If it formed by disk instability, then it has probably not much changed over the last 7 Gyr. The shape of the dark halo is probably remained more or less constant, except near the disk plane

34. Second order signatures What information remains from subsequent evolution after the disk formed ? Objects fall in to halo and break up. Their stars conserve some dynamical properties. Streams like Sgr will gradually mix away structurally but some dynamical information survives. Star forming events in the disk mostly dissolve and phase-mix around the Galaxy. Some maintain their kinematical identity as moving stellar groups. A few survive as open clusters : some are almost as old as the disk. All maintain their chemical identity, so we can use chemical techniques to find the debris of old dissolved star forming events. Surviving star clusters and moving groups are chemically very homogeneous

35. Chemical abundances in two open clusters and one old moving group • Hyades • Collinder 261 • HR1614 moving group Da Silva et al, 2008

36. highly eccentric halo stars disk stars: low-e orbits The metal-poor stellar halo Carney Laird Latham (1996) survey of high proper motion stars : orbital eccentricity vs [m/H] - modern version of ELS The CLL survey shows the striking kinematical difference between disk and halo

37. rapidly rotating disk & thick disk slowly rotating halo Rotational velocity relative to the sun vs [m/H] (V = -220 km/s corresponds to zero angular momentum)

38. GCs halo stars Carney Laird Latham survey : different metallicity distributions of halo stars and globular clusters : halo stars now known down to [Fe/H] < -5

39. 40 Not all of the metal-poor stars ([Fe/H] < -1) are in the halo. A fraction belong to the thick disk. More on the thick disk later: although most of the stars in the old thick disk have abundances of [Fe/H] = - 0.7 to -1.0, the thick disk has a long metal weak tail extending down to [Fe/H] ~ -2. About 25% of the stars with [Fe/H] = -1.5 near the sun belong to the thick disk Halo & thick disk are ancient structures, very important for GA

40. Halo Streams Long orbital timescales  survival of identifiable debris eg Sgr tidal stream, discovered near the bulge, extends right around the Galaxy (probably a few times around) 2MASS M giants Ibata et al 1995 Majewski et al 2003

41. These tidal streams from the currently disrupting Sgr dwarf are interesting (the halo is still under construction) as are the ancient streams from small objects accreted long ago into the halo The long orbital periods allow these ancient streams to survive, so the metal-poor halo is the best place to attempt reconstruction of their accretion events. They are too faint to see in configuration space - may see them in phase space, eg (RG , VG ), or in integral space ie the space of integrals of the motion for stellar orbits, like energy and angular momentum (E , Lz )

42. Accretion is important for building the stellar halo, but not clear yet how much of the halo comes from discrete accreted objects (debris of star formation at high z) versus star formation during the baryonic collapse of the Galaxy At one extreme, simulations of pure dissipative collapse (eg Samland et al 2003) suggest that the halo may have formed mainly through a lumpy collapse, with only ~ 10% of its stars coming from accreted satellites In any case, we can hope to trace the debris of these lumps and accreted satellites from their phase space structure. But we can also use chemical techniques to trace their debris

43. References Binney & Tremaine: Galactic Dynamics (1987, 2008). This is the book on Galactic Dynamics: some of the material in these lectures comes from B&T Binney & Merrifield: Galactic Astronomy (1998). A more descriptive book and well worth reading for background. Sparke & Gallagher: Galaxies in the Universe (2007). Ditto : good book, with some theory Turon & Primas: ESA-ESO Working Group Report #4: Galactic Populations, Chemistry and Dynamics (2008). A very useful compendium of Galactic knowledge, problems, techniques, surveys