Download - Galaxies and Cosmology
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Galaxies and Cosmology
5 points, vt-2007
Teacher: Göran Östlin
Lectures 7-9
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Theoretical cosmology
Problems with Newtonian Gravity and Mechanics:GravityInertial frames - absolute space and time
General Relativity - matter curves space (& time), EPG + g = -8G T / c4
G, g, T are tensors
Geometry: line element
Cosmological principle: isotropy, homogeneity
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Gravity can in General Relativity be regarded as a space curvature rather than a force
Orbit of earth a straight line in space-time
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Geometrical cosmology: Line elements
€
ds2 = dx 2 + dy 2
ds2 = dx 2 + dy 2 + dz2
ds2 = dr2 + r2(dθ 2 + sin2θ dφ2)
ds2 = r2(dθ 2 + sin2θ dφ2)
ds2 = dx 2 + dy 2 + dz2 − c 2dt 2
ds2 < 0
ds2 = 0
ds2 > 0
2-dim cartesian
3-dim cartesian
3-dim spherical
2-dim curved space
Special relativity
Timelike separation
Null separation (light)
Spacelike separation
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Robertson-Walker line element
€
ds2 = c 2dt 2 − R2(t)dr2
1− kr2+ r2(dθ 2 + sin2θ dφ2)
⎡
⎣ ⎢
⎤
⎦ ⎥
Simplest 4-dim (3 space, 1 time) space that fulfills the cosmological principle
Only R(t) changes with time -> homogeneously expanding or contracting space
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Redshisfts…
z = (obs - em)/ em = obs / em - 1 = /
vr = z c
z = H0 d / c => v r= H0 d
Valid up to z 0.2
NB Special relativistic formula not more accurateGeneral relativistic description of space-time required
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Redshift
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Redshifts…
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Cosmic time vs redshift
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Newtonian derivation of Friedman equations(see handwritten handouts)
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FRW-models, summary
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Properties of the Universe set by3 parameters: m, , k of Which only 2 areIndependent: m + + k = 1
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Age of universe for: closed(1), critical(2), open(3), and acellerating(4) models
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Active galaxies / Active galactic nuclei (AGN)
Compact regions in the centre of galaxies withGreat luminosity and rapid variability.
Common characteristics:Broad emission lines, high excitation, jetsflat spectral energy distribution(non thermal)
Many classses:-Seyfert 1 & 2-Quasars, QSOs-Radio galaxies-Bl Lac, Blazars
… are all the same?
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Quasars 1960’s and onwards
1963 Marten Schmidtdetermines redshiftfor the first time
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Seyfert spectraQuickTime och en
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Broad and narrow linesPermitted and forbidden lines
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Active galaxies / Active galactic nuclei (AGN)
Central enginevariability put limit on size: R ≤ c var
Schwarzschild radius: Rs = 2 G M / c2
Rs = size approx Uranus orbit for 109 M
Accretion allows conversion of 0.1mc2
(fusion only 0.7%)Radiation pressure will larger than gravity if L > LEDD
Accretion disk very hot continuum source => X-raysBroad line region, dense ionised clouds, rapid movingNarrow line region, dilute ionised clouds, slower
reverbration mappingObscuring torus with dust and molecular gas,
sublimation evacuate central part -> torusRelativistic (superluminal) Jets, and radio Lobes
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QSO spectrum
Note the broad emission lines and blue continuum
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Radio images of radio galaxiesSynchrotron emission
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M87 (radio galaxy): jets both in optical and radio
Jets often one-sided due to relativistic beaming
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F_lam vs F_lam*lam
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Blazar spectra
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Superluminal motionQuickTime och en
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SuperluminalMotions !
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QSO absorption lines
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Unified AGN models
Idea: all AGN are basically the same phenomenaDiffering due to different viewing angle and scale:
Face on view: see all components: Sy1, QSO if looking into jet: Bl Lac (Blazar)
Edge on view: see only hot torus and NLR, Sy2
Why some radio loud while others not?
Unified BH model not perfect, but nothing else works
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Unified model of AGN
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Unified Model
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Spiral seyfert2 with radio jets
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Seyfert1
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QSO evolution - where are they now?
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Debate if fall off at z>3 is real
There must be many dead QSOs around in the local universe!
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Kinematical evidence for BH in M87
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+ Grav redshifted X-ray em-lines detected in Sy1’s
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Relation between black hole mass and sigma of host galaxy: a realtion between BH and Spheroid Mass-- Black Hole doesn’t care about disk-- Co-evolves with spheroid/bulge!
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Clusters And Large Scale Structure (chapt. 4)
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M33
Sex A
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LeoI
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Tidal drag on NGC205 from M31
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Local Group
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HCG31
GalaxyEvolution/Transformation
Caught inaction
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Rich clusters: Virgo and Comairregular vs regular
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(large spiral fraction) (mostly ”early” types)) (more relaxed)
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Hot gas in clustersX-ray emitting through thermal bremsstrahlung
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Efficient way of findingclusters
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Perseus cluster central galaxy
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Butcher-Oemler effect, etc:
As we look back in time, the spiral fraction ofRich clusters become higher and higher (BO)
Cluster and Galaxy transformation
Interactions: galaxy mergerscluster mergergalaxy harassmentram pressure strippingdiffuse intracluster light: stars + gasvs Hot intracluster gas
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Masses of clusters:Virial theorem: M = RA v
2 / G
- does it apply?
X-ray gas in Hydrostatic equilibrium - does it apply?
Gravitational lensing:
it does apply but only gives mass contrast
- Methods agree fairly well (factor of 2)
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Gravitational lensing
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Einstein ring
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Abell 2218, strong lensingcf weak lensing (statistical)
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Angular distribution of Abell-clustersBrightest cluster galaxy method allows rough space distribution to be inferred
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Virgo supercluster
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LargeScaleFlows
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Distribution of galaxies on the sky
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Sponge-like topology of universe
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CfARedshiftSurveyGreat wall
Voids!
Finger of god
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SDSS
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Distribution of red and blue galaxies in space
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Intergalactic matter
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Gunn-Peterson effect
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Cosmic shear
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Challenging!- Effect on each individual galaxy tiny- Only visible through lareg and deep samples
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Measuring Clustering- Count in cells- 2-point corellation function
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Peculiar velocities
Deviations from the Hubble flow
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Basic Friedmann model universa(see handout papers)