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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 Presentation
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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
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
Central surface brightness vs magnitude
The Realm of Galaxies
15 mag range, 4 types, 16 mag arsec-2.range
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
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
Radial TF
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
MODEL
V traces the potential
DM emerges at large radii
Modelling the very inner circular velocities: light traces the mass
Phenomenology of spiral kinematics
The rotation curves 3200 coadded individual
PSS
C+06
RC slopes vary among galaxies and within them.
They indicate the presence and the amount of dark matter.
At 3 disk length scales
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
3.avi
../Desktop/3.avi
The URC
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
NFW Halos
Burkert Halos
cored vs cusped
VNFW fits uniquely a rotation curve
Modelling the Universal Rotation Curve
rotation velocity
stellar contribution
dark matter contribution
Stars
DM
LM
A family governed by luminosity
DM
frac
tion
core radiushalo central density
luminosity
The role of the slope of the RC
Halo central density vs core radius scaling r 0 =10-23 (r0 /kpc)-1 g/cm3
dSph
B
URCWL
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
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
DM halo density: observations vs simulations
URCL
NFW
URCH
The UNIVERSAL velocity CURVE
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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rXiv:
0906
.465
4
A test case: ESO 116-G12
gas
stars
halo
Cored halos the best fits
50 objects investigated
NFW inconsistent
Theory Obis ssw
Obs Theory
DDO 47: a decisive case
NFW
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)
DDO 47: non circular motions?
R
V (m
inor
axi
s)
Triaxial halos predictions
A Universal Mass Profile Walker et al 09Dwarf Spheroidal Galaxies
LCDM Universal Rotation Curve from NFW profile and MMW theory
➲ AN INTRIGUING PROPERTY
A matter enigma
DM in early-types: weak+strong lensing22 bright E/S0s at z ~ 0.2 (SLACS: Gavazzi et al. 2007)
DARK MATTER IS PRESENT IN GALAXIES
IT IS STRONGLY RELATED TO THE LUMINOUS MATTER
THERE IS A SOLID EMPIRICAL SCENARIO
We can uniquely mass model a RC
disk-halo components, known surf phot, reliable V(R) and dV/dR, resolution ~ 0.3 RD
A way out? angular momentum exchange between baryons and DM Tonini Lapi Salucci
cusp
core