Upcoming class schedule

Transcription

1 Upcoming class schedule Thursday March 15 2pm AGN evolution (Amy Barger) th Monday March 19 Project Presentation (Brad) nd Thursday March 22 postponed to make up after spring break.. Spring break March then back to normal as of Tuesday 3rd April th

2 GALAXIES 626 Lecture 16: The effects of environment

3 The colour magnitude diagram Red sequence Note the bimodality of galaxy colours blue sequence Sloan DSS data

4 The colour magnitude diagram Dependence on environment

5 Fraction of red galaxies depends strongly on density.. Density dependence present at all luminosities. Bright and faint galaxies show trend with density

6 Moving galaxies from the blue to the red peak What are the implications for the galaxy transformation mechanism? Blue & red peaks are correlated with density, But Density evolves. Galaxies must move from one to the other How long do they take? If they take too long, then the gap between the peaks will be filled in...

7 Timescales for Galaxy Transformation How rapid must the blue red transition be? Two gaussian model Red Peak always fits the data well there is no room for an intermediate population. colour evolves rapidly if timescale for star formation to stop is short Blue Peak if transformations occur uniformly in time: need τ<0.5 Gyr

8 Summary There are distinct populations of red ( early ) and blue ( late ) galaxies The mean colors and spread of the two populations depends only weakly on environment But the relative abundance of the populations is a strong function of environment. Blue galaxies move quickly into the red population as their environment changes Why?

9 Evolution with redshift How does the dependence on environment change with redshift?

10 Galaxy clusters: z=0 z=0.39 z=0.83 Local galaxy clusters are dominated by passively evolving galaxies with high formation redshifts How does the evolution compare with the general field? Nature or nurture: clusters are built from groups. How do groups evolve?

11 Butcher Oemler Effect Concentrated clusters at high redshift may have Blue fraction more blue galaxies than concentrated clusters at low redshift But blue fraction depends strongly on luminosity and radius so care needs to be taken to evaluate blue fraction at same luminosity limit, and within same (appropriate) radius.

12 Cluster SFR evolution Butcher Oemler effect also seen in the general field Is the effect stronger in clusters? Field 2dF Clusters Redshift 1 Nakata et al. (2005) Based on sparsely sampled [OII] Postman, Lubin & Oke 2001 spectroscopy van Dokkum et al Suggests fraction of star Fisher et al forming galaxies evolves Czoske et al relatively weakly in clusters

13 Red galaxy fraction Red galaxy fraction Evolution of the red peak High density All galaxies MV < 20 Low density Redshift

14 Tying star formation to structure growth Groups Clusters

15 Low redshift groups Relation between star formation rate and local density Field Field

16 Groups There are fewer spiral galaxies in groups than in the field, at the same redshift. No evidence for more disturbance/irregularities in group galaxies Spiral fraction Field Spiral fraction E/S0 fraction Morphologies: Field Groups Groups Vel. Dispersion (km/s)

17 The connection between star Field formation rate, morphology Groups and environment Distributions are corrected for differences in luminosity function between group and field S0 Elliptical Early spiral Late spiral Like clusters, groups contain passive spirals: disk morphology but low star formation rates

18 Evolution in groups Fraction of non SF galaxies Use [OII] equivalent width to find fraction of galaxies without significant star formation most galaxies in groups at z~0.4 have significant star formation in contrast with local groups

19 Fraction of non SF galaxies Groups Fraction of non SF galaxies Field Group SFR evolution Fraction of non SF galaxies increases with decreasing redshift for both groups and field Insensitive to aperture effects

20 Summary More star formation in groups at z=0.5 than at z=0 On average, groups at 0<z<0.5 have less star formation and fewer spiral galaxies than the field. Passive spiral galaxies are a key component of groups at z=

21 Environmental Mechanisms Why should galaxy properties depend on the environment? Collisions / harassment "Strangulation" Ram pressure (actual effects) Different history...

22 Ram Pressure Stripping Mostly important in clusters where the surrounding gas density is high...

23 Ram Pressure Stripping ICM Clusters are not empty in fact, most baryons are in a diffuse form, the intra cluster medium As a galaxy travels through the ICM, it feels a force, the ram pressure aaaaaa 2 ρh v 2 πgσ R Σ g R The gas disk will be to radius R if: Gravitational Force due to ICM restoring force

24 Ram pressure Stripping - ICM simulations

25 Galaxy NGC 4388 Expels Huge Gas Cloud NGC 4388 is a member of the the Virgo Cluster. It is classified as an active galaxy. One hypothesis holds that the gas was stripped away as NGC 4388 made its way through the intergalactic medium of the Virgo Cluster.

26 Galaxy interactions Gravitational interaction can produce major shifts in the gas and stars of the galaxy Major mergers produce massive star forming events but more minor repeated events can gradually remove the gas from a galaxy

27 Galaxy Collisions, Tides and Harassment Tidal truncation Slow encounter Depends on gradient of potential Big impact on the dark halo, but not significant for stellar component Impulsive heating Fast encounter Importance increases as relative velocity decreases Harassment The cumulative effect of repeated encounters

28 Galactic mergers Most dramatic examples: major mergers between galaxies of comparable mass. Large morphological changes as a consequence of the interaction. Observationally and theoretically, find that major mergers are uncommon - perhaps ~1 such merger in the lifetime of the Universe for a large galaxy in the field.

29 Examples of galaxy collisions in the real universe and in a simulation (Moore et al 1995)

30 The Antennae Galaxy

31 Best place for major mergers - small groups of galaxies Galaxies in rich clusters are generally less vulnerable to mergers, despite the very high density of galaxies because the velocities are higher.

32 Galaxy Collisions, Tides and Harassment Galaxy 1 size x force Perturbation to gradient Time of velocity of star encounter in galaxy 1 m Δv =2 r b V M Perturber, galaxy 2 ΔE = GM b3 2 r 2 b V 4G M m 4 3b V Change of internal energy of galaxy 1 2 r2

33 Minor mergers between galaxies of very different masses are much more common. Example: the Magellanic clouds Bound satellites orbiting within the extended halo of the Milky Way (~50 kpc distance) Eventually will spiral in and merge Sagittarius dwarf galaxy is another satellite which is now in process of merging

34 What effect does the merger have on the disk galaxy? How fast does the spiral-in and merger occur?

35 Dynamical Friction Why does the orbit of a satellite galaxy moving within the halo of another galaxy decay? Stars in one galaxy are scattered by gravitational perturbation of passing galaxy. Stellar distribution around the intruder galaxy becomes asymmetric - higher stellar density downstream than upstream. Gravitational force from stars produces a `frictional force which slows the orbital motion.

36 How quickly will the LMC merge with the Milky Way? Simple estimate - dynamical friction time: t friction» V» V km/s dv / dt 4 pg 2 Mnm ln L ~ Solar masses Galactic density at LMC for flat rotation curve estimate 3 x 10-4 Solar masses / pc3 With these numbers, estimate orbit will decay in ~3 Gyr Close satellite galaxies will merge!

37 Strangulation - removal of the gas halo Removes surrounding gas and so stops infall and star formation

38 Strangulation - removal of the gas halo

39 Summary of Mechanisms Ram pressure Needs dense ICM and high velocities clusters Collisions / harassment Mostly in groups where slow galaxy interactions are common "Strangulation" Removal of the gas halo: no more fuel supply Similar to ram pressure stripping but much easier!

40 Mechanisms Ram pressure Density too low Needs dense ICM and high velocities clusters Collisions / harassment Groups are preferred place! "Strangulation" Removal of the gas halo: no more fuel supply Similar to ram pressure stripping but much easier! Transformation too rapid

41 Mechanisms Collisions / harassment Groups are preferred place! What next? Look at individual galaxies to see if they provide evidence to support the big picture The best mechanism to explain the observational data but most effective in galaxy groups rather than clusters

42 Summary Clear bimodality of galaxy properties More dense environments... there is less star formation A higher fraction of passive/red galaxies But... Star Forming/blue galaxies have similar properties in all environments (only the fraction changes) Passive galaxies exist in all environments Galaxy transformation is rapid! Its most likely to happen in galaxy groups rather than in clusters

43 End