dark matter in galaxies
DESCRIPTION
DARK MATTER IN GALAXIES. Paolo Salucci (SISSA). Dennis: Rotation Curves, Dark Matter, Nature of, Role of Baryons. Importance of the topics but low interest from Scientific Community. Persic , M ., S. P ., 1988, MNRAS, 234 131 Dark and visible matter in spiral galaxies - PowerPoint PPT PresentationTRANSCRIPT
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DARK MATTER IN GALAXIES
Paolo Salucci (SISSA)
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Dennis: Rotation Curves, Dark Matter, Nature of, Role of Baryons.
Importance of the topics but low interest from Scientific Community
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Persic, M., S. P., 1988, MNRAS, 234 131
Dark and visible matter in spiral galaxies
Persic, M.; S. P., Stel, F. 1996 MNRAS, 281, 27
The universal rotation curve of spiral galaxies - I. The dark matter connection
Gentile, G.; S. P., Klein, U. 2004 MNRAS, 351, 903
The cored distribution of dark matter in spiral galaxies
S.P + 2007 MNRAS
The universal rotation curve of spiral galaxies out the virial radius II
S.P. ...... ADS reviews
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Central surface brightness vs magnitude
The Realm of Galaxies
15 mag range, 4 types, 16 mag arsec-2.range
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Stellar distribution L(R/RD)/LT is independent of luminosity
The light surface profile I(r) = I0exp (-R/RD).
A mass lenght-scale
luminosity independent?
1000 objects
Colo
rs a
re ra
dial
ly c
onst
ant
3RD
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RTF: magnitude vs log velocity @ different radii xi RD, [ xi=0.5,1,…5]
3 samples (600, 89, 78) M =ai + bi log V(xi)
No relationship ↔ V does not trace the mass
Vmax
Does the kinematics probe the mass distribution of galaxies ? Yes.
• Radial Tully Fisher
• Inner mass distribution
0.0 0.5 1.0 1.5 2.0 2.5 3.0
0
50
100
150
200
250
V
R/Rd
UGC2405
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Radial TF
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Slope and scatter of the TF-relations:MB = ai + bi log V(xi)
The slope increases from -4 to -8.
No change in slope ↔ no DM or a constant fraction of DM
The minimum scatter 0.2 mag at 2.2 RD
0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0-1
-2
-3
-4
-5
-6
-7
-8
-9
86 galaxies (Courteau) 967 galaxies (Mathewson)
Slo
pe
R/Rd
0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0
0.15
0.20
0.25
0.30
0.35
0.40
0.45
0.50
86 galaxies (Courteau) 967 galaxies (Mathewson)
scat
ter
R/Rd
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MODEL
V traces the potential
DM emerges at large radii
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Modelling the very inner circular velocities: light traces the mass
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Phenomenology of spiral kinematics
The rotation curves 3200 coadded individual
PSS
C+06
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RC slopes vary among galaxies and within them.
They indicate the presence and the amount of dark matter.
At 3 disk length scales
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The URC concept ➲ @ fixed L and x=R/RD, the Cosmic Variance of V(x,L) is
one order of magnitude smaller than the variations that:
➲in each galaxy, V(x) shows as x varies.
➲V(x) shows, @ each x, in galaxies of different L
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3.avi
../Desktop/3.avi
The URC
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Rotation curve modelling.
V d is k R➲ : from I-band photometry
➲ : from HI observations
➲
• dark halos with constant density cores
• dark halos with “cusps” (NFW, Moore)
• HI-scaling
• MOdified Newtonian Dynamics
..t4bt5b
V h a lo R
V g a s R
V tot2 V DM
2 V disk2 V gas
2
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NFW Halos
Burkert Halos
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cored vs cusped
VNFW fits uniquely a rotation curve
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Modelling the Universal Rotation Curve
rotation velocity
stellar contribution
dark matter contribution
Stars
DM
LM
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A family governed by luminosity
DM
frac
tion
core radiushalo central density
luminosity
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The role of the slope of the RC
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Halo central density vs core radius scaling r 0 =10-23 (r0 /kpc)-1 g/cm3
dSph
B
URCWL
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Virial halo masses
andHMF M h dM h A M h1.84 dM h
HMF M h dM h dM b dM b BMF M b dM b
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Christiane Frigerio Martins
Weak lensingWith a density profile we model the tangential shear Obtain the structural free parameters.
Same results as those obtained from RCs.
Burkert profile provides excellent fit, better than NFW.
NFW
B
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DM halo density: observations vs simulations
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URCL
NFW
URCH
The UNIVERSAL velocity CURVE
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Dark halos from simulations
Halos form hierarchically bottom-up via grav. amplifications of initial density flucts. Most
evident property: CENTRAL CUSP
NFW r s
r r s 1 r r s2
M vir43 vir u Rvir
3 cvir Rvir r s 9.7 M vir 1012 M un0.09V vir
2 GM vir Rvir
cuspy NFW density profiles disagree with observed kinematics.
comparison galaxy by galaxy and of coadded kinematics.
The cusp vs core issue
NFW HALOS
• Fit badly the RCs
• Unphysically too low stellar mass-to-light ratios
• Unphysically too high halo masses
Navarro, Frenk & White, ApJ 462, 563 (1996)
Bullock et al., MNRAS 321, 559 (2001)
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A test case: ESO 116-G12
gas
stars
halo
Cored halos the best fits
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50 objects investigated
NFW inconsistent
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Theory Obis ssw
Obs Theory
DDO 47: a decisive case
NFW
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Results fromTrieste: analysis of highquality RCs
URC fits to RCs
DDO 47
Borriello & Salucci, MNRAS 323, 285 (2001)
Gentile, Tonini & Salucci, A&A 467, 925 (2007)Gentile et al., ApJ 634, L145 (2005)
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DDO 47: non circular motions?
R
V (m
inor
axi
s)
Triaxial halos predictions
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A Universal Mass Profile Walker et al 09Dwarf Spheroidal Galaxies
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LCDM Universal Rotation Curve from NFW profile and MMW theory
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➲ AN INTRIGUING PROPERTY
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A matter enigma
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DM in early-types: weak+strong lensing22 bright E/S0s at z ~ 0.2 (SLACS: Gavazzi et al. 2007)
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DARK MATTER IS PRESENT IN GALAXIES
IT IS STRONGLY RELATED TO THE LUMINOUS MATTER
THERE IS A SOLID EMPIRICAL SCENARIO
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We can uniquely mass model a RC
disk-halo components, known surf phot, reliable V(R) and dV/dR, resolution ~ 0.3 RD
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A way out? angular momentum exchange between baryons and DM Tonini Lapi Salucci
cusp
core