quasars and low surface brightness galaxies as probes of dark matter
DESCRIPTION
Quasars and Low Surface Brightness Galaxies as Probes of Dark Matter. Erik Zackrisson. Outline. Dark matter Dark matter halos Baryonic and non-baryonic dark matter Cold dark matter Quasars Gravitational lensing Redshift Low Surface Brightness Galaxies Rotation curves Summary of Results. - PowerPoint PPT PresentationTRANSCRIPT
Quasars and Low Surface Quasars and Low Surface Brightness Galaxies as Brightness Galaxies as Probes of Dark MatterProbes of Dark Matter
Erik ZackrissonErik Zackrisson
OutlineOutline Dark matterDark matter
Dark matter halosDark matter halos Baryonic and non-baryonic dark matterBaryonic and non-baryonic dark matter Cold dark matterCold dark matter
QuasarsQuasars Gravitational lensingGravitational lensing RedshiftRedshift
Low Surface Brightness GalaxiesLow Surface Brightness Galaxies Rotation curvesRotation curves
Summary of ResultsSummary of Results
Dark matter Luminous matter
Dark MatterDark Matter
First detection of dark matterFirst detection of dark matter
Fritz Zwicky (1933): Dark matter in the Coma ClusterFritz Zwicky (1933): Dark matter in the Coma Cluster
The Dark Matter ProblemThe Dark Matter Problem
~2%(Luminous)
~98% (Dark)
Dark Matter Halos IDark Matter Halos I
Galaxy Stars + Gas + Dust + Supermassive Black Hole + Dark Matter
Dark Matter Halos IIDark Matter Halos II
Luminous galaxy
Dark halo
Baryonic & Non-Baryonic Baryonic & Non-Baryonic Dark MatterDark Matter
Baryonic matter: ~15%Baryonic matter: ~15%Example: Stars, gas clouds, planets…Example: Stars, gas clouds, planets…Missing: ~ 35%Missing: ~ 35%
Non-baryonic matter: ~85%Non-baryonic matter: ~85% Example: Axions, neutralinos,Example: Axions, neutralinos, primordial black holes…primordial black holes…Missing: ~ 100%Missing: ~ 100%Best model: Cold Dark Matter (CDM)Best model: Cold Dark Matter (CDM)
Cold dark matter and Cold dark matter and the evolution of structurethe evolution of structure
Cold dark matter and Cold dark matter and the evolution of structure IIthe evolution of structure II
Cold Dark Matter HalosCold Dark Matter Halos
R
RDark matter halo
Den
sity
Central densitycusp predicted bycold dark matter
Observed
QuasarsQuasars
Gravitational lensingGravitational lensing
Gravitational lensing IIGravitational lensing II
Microlensing Made SimpleMicrolensing Made Simple
Obs! Fel bild!
Microlensing Made Simple IIMicrolensing Made Simple II
Claim: The long-term optical variability Claim: The long-term optical variability of quasars is quased by microlensingof quasars is quased by microlensing
Hawkins, M.R.S. (1993, 1996, 1997, 2000, 2001, 2002, 2003)
The dark matter puzzle solved?The dark matter puzzle solved?
Mcompact 10-3 Msolar Almost all of the dark matter in this form Primordial black holes?
Expansion of the UniverseExpansion of the Universe
RedshiftsRedshifts
High z Large distanceLow z Small distance1
emit
obs z
Claims of non-cosmological Claims of non-cosmological redshiftsredshifts
Low-z galaxy surrounded by overdensity of high-z quasars
Low-z galaxy with pairs of high-z quasars (with z1z2)
aligned along minor axis
z1
z2
Ejection scenariosEjection scenarios
Local galaxy, very low redshift (z1)
Faint quasar, high redshift (>>z1)
Bright quasar, low redshift (>z1)
New galaxy (?), very low redshift (z1)?
?
?
?
?
Low Surface Brightness GalaxiesLow Surface Brightness Galaxies
The Very Large Telescope Examples ofTarget Galaxies
The Central Mass BudgetThe Central Mass BudgetLow Surface
Brightness GalaxiesHigh Surface
Brightness Galaxies
Dark matter
Luminous matter
Dark matter
Luminous matter
Rotation CurvesRotation Curves
Radius
Vrot
Radius
Density
Spectroscopy → Rotation Curve → Density Profile
CDM prediction
Observed
ResultsResultsPaper IPaper I Uncertainties in the typical quasar size Uncertainties in the typical quasar size Quasar Quasar
variability cannot easily be used to constrain dark matter variability cannot easily be used to constrain dark matter at the current time at the current time
Paper IIPaper II Microlensing cannot explain the long-term optical Microlensing cannot explain the long-term optical
variability of quasars – Hawkins is wrong!variability of quasars – Hawkins is wrong!
Paper IIIPaper III Non-cosmological redshift scenarios involving quasar Non-cosmological redshift scenarios involving quasar
ejection can be tested with observations of quasar host ejection can be tested with observations of quasar host galaxies made a small telescopegalaxies made a small telescope
Results IIResults IIPaper IVPaper IV The bluest low surface brightness galaxies can be used The bluest low surface brightness galaxies can be used
to test hierarchical galaxy formation models – provided to test hierarchical galaxy formation models – provided that we can derive their agesthat we can derive their ages
The star formation rate of the bluest low surface The star formation rate of the bluest low surface brightness galaxies cannot have been constant or brightness galaxies cannot have been constant or increasing – unless the stellar initial mass function is increasing – unless the stellar initial mass function is unusual unusual
Paper VPaper V The density profiles of the dark halos surrounding the The density profiles of the dark halos surrounding the
bluest low surface brightness galaxies are in conflict with bluest low surface brightness galaxies are in conflict with the Cold Dark Matter predictionsthe Cold Dark Matter predictions
ErrataErrata Spikblad: Polhemssalen Spikblad: Polhemssalen Polhemsalen Polhemsalen Page v: optical long-term Page v: optical long-term long-term optical long-term optical Page 3: as the ray crossed Page 3: as the ray crossed as its ray grazed as its ray grazed Page 24 (twice): reflectance Page 24 (twice): reflectance reflection reflection Page 33: z Page 33: z 2—3 2—3 z z 2—4 2—4 Page 35: the latter variations Page 35: the latter variations these variations these variations Page 35: hoever are Page 35: hoever are are however are however Page 37: by fast rise Page 37: by fast rise by a fast rise by a fast rise Page 44: 10Page 44: 101212—10—101414 m m 10 101212—3—310101313 m m Page 56: disk by Page 56: disk by disk is given by disk is given by Page 69: ett par procent Page 69: ett par procent några få procent några få procent Page 69: välkända astronomiska objekt Page 69: välkända astronomiska objekt välkända typer av välkända typer av
astronomiska objekt astronomiska objekt Page 69: både vår och andra Page 69: både vår och andra både vår egen och andra både vår egen och andra Paper I, page 26, column 2, paragraph 1: higher angular size Paper I, page 26, column 2, paragraph 1: higher angular size
distance distance higher light travel time distance higher light travel time distance Paper V, page 8: Division line should not be dashed Paper V, page 8: Division line should not be dashed