Bodo Ziegler
Bodo Ziegler
Bodo Ziegler
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FORS Deep Field<br />
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Kinematic & Structural Evolution of Field & Cluster Spirals<br />
Rotation Curve<br />
<strong>Bodo</strong> <strong>Ziegler</strong><br />
Institute for Astronomy<br />
University of Vienna<br />
Morphology<br />
Cluster MS0451<br />
z=0.5<br />
Velocity Field
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Deep photometry<br />
+ template fitting<br />
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luminosity evolution<br />
HST imaging<br />
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structure evolution<br />
spectroscopy<br />
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kinematic evolution<br />
Galaxy Evolution<br />
FORS Deep Field
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Galaxy Evolution<br />
Principal Issue: Classification of Galaxies<br />
● Colors: red or blue, green?<br />
● Structure: disk or spheroid<br />
● Surface brightness: exponential or Sersic<br />
● Star formation: emission or absorption lines<br />
● Stellar populations: young or old, intermediate?<br />
● Kinematics: rotation or dispersion<br />
Galaxy transformation!
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Morphologies of distant galaxies<br />
Fit 2dim surface brightness with your favorite<br />
➔ law (exponential, Sersic etc) for disk & bulge<br />
➔ model package (GALFIT, GIM2D, BUDDA)<br />
or use your favorite non-parametric approach<br />
➔ CAS: concentration, asymmetry, clumpiness<br />
➔ Gini & M 20<br />
⇒ structure evolution<br />
z=0.5 spiral<br />
GALFIT<br />
disk+bulge<br />
● What defines the morphology of a galaxy?
I/M<br />
S<br />
M<br />
S<br />
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Da Rocha & <strong>Ziegler</strong> 2010<br />
Morphologies of distant galaxies<br />
E<br />
E<br />
CL0016:<br />
z=0.54±.05<br />
FDF only for:<br />
0.45
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Star formation activity in distant cluster galaxies<br />
“stacking” of 6 z~0.25 clusters<br />
Verdugo, <strong>Ziegler</strong>, Gerken 2008
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Star formation activity in distant cluster galaxies<br />
[O II]3727 & H<br />
α equivalent widths and fraction of SF galaxies<br />
as f(distance) & f(density).<br />
Verdugo et al. 2008
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Star formation activity in distant cluster galaxies<br />
Verdugo et al. 2008<br />
[O II]3727 & H α equivalent widths of SF galaxies as f(density).
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Star formation activity in distant cluster galaxies<br />
Color - Magnitude Specific SFR – stellar mass<br />
SF galaxies (blue dots)<br />
within red-sequence<br />
have intermediate sSFR<br />
(green dots)
Study evol.<br />
Tully-Fisher<br />
relation and<br />
mass evol.<br />
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Rotation curves of field spirals with z=0.1 to z=1<br />
<strong>Ziegler</strong> et al. 2002<br />
Böhm et al. 2004<br />
Böhm & <strong>Ziegler</strong> 2007
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Environment: Interactions in Clusters<br />
● tidal (gravitational) interactions<br />
● merging, accretion<br />
● ram-pressure stripping by<br />
intracluster medium (hot x-ray gas)<br />
● harassment<br />
● strangulation, suffocation,<br />
starvation
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Tully-Fisher Relation of z≈0.5 Cluster & Field Galaxies<br />
<strong>Ziegler</strong> et al. 2003,<br />
Jäger et al. 2004<br />
Also: Yaffe, Aragon-<br />
Salamanca et al 2010<br />
Distribution of field & cluster spirals very similar!<br />
Effect of cluster-specific interactions? ⇒ need 2d-velocity fields
Cluster MS 1008-12<br />
(z = 0.31)<br />
FORS<br />
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Kinematics of spirals in distant clusters<br />
Hierarchical growth of structure:<br />
late cluster assembly (z≈1)<br />
merging frequency (efficiency)<br />
& infall rate increases with z<br />
Project for 7 clusters 0.3
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Velocity fields with FORS2 «3D simulation»<br />
0.25”<br />
1.0”
See my<br />
poster,<br />
please!<br />
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Velocity fields with FORS2<br />
3D-measurement:<br />
● MXU masks of VLT/FORS2<br />
➔ matched spatial coverage<br />
➔ sufficient spatial resolution<br />
➔ large wavelength coverage<br />
➔ high efficiency: large target number<br />
➔ economic exposure times<br />
● 4 nights VLT time spent<br />
●& HST/ACS imaging of all cluster fields<br />
<strong>Ziegler</strong> et al.<br />
2007 & 2009<br />
Messenger 137
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Velocity Field of Regular Spiral Cluster Member<br />
MS0451-03 z=0.53<br />
Kutdemir et al. 2008<br />
cf. with 3”x2” FLAMES IFU
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Kinemetry Analysis<br />
For flat disk galaxy, velocity profile along best fitting ellipse has cosine form:<br />
R: radius of ring, V 0 : system. velocity, V c : circular velocity, Ψ: azimuthal angle<br />
Krajnović et al. 2006
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Kinemetry of Regular Spiral Cluster Member<br />
Reconstructed map with best fitting ellipses<br />
using higher order Fourier terms & its residual map.<br />
Kutdemir, <strong>Ziegler</strong> et al. 2008<br />
R (distance from center)<br />
Position<br />
Angle<br />
Flattening<br />
(b/a)<br />
Bulk Motion<br />
Deviation<br />
from<br />
simple<br />
rotation<br />
Separate<br />
kinematic<br />
components
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Field spiral w. counter rotating core<br />
Gal20 z=0.1
Kutdemir et al. 2008<br />
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Velocity Field of Peculiar Spiral Cluster Member<br />
Simulation of minor merger<br />
(8:1 mass ratio)<br />
seen after second passage<br />
Kronberger et al. 2007
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Simulation of merger & ram-pressure stripping<br />
Kapferer et al. 2009<br />
Kapferer et al. 2006, Kronberger et al. 2006, Kronberger et al. 2007, Kronberger et al. 2008<br />
Collaboration with Kapferer, Kronberger & Schindler (Innsbruck)
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Parametrization of irregularity : Δ Φ<br />
Δ Φ : Mean difference between photometric & kinematic Position angle<br />
z=0.36
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Parametrization of irregularity σ PA & k 3,5<br />
R max<br />
R max<br />
σ PA<br />
Standard deviation<br />
kin. Position angle<br />
k 3,5 = (k 3 + k 5 )/k 1<br />
Average of<br />
higher Fourier<br />
coefficients
Limit: σ PA = 20<br />
Limit: k 3,5 = 0.15<br />
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Classification of irregularity<br />
Local sample: Daigle et al. 2006<br />
Kutdemir et al. 2008,2010<br />
Limit: Δ Φ = 25
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Abundance of irregularities<br />
Local sample<br />
Distant sample<br />
red: field<br />
yellow: clusters<br />
Kutdemir et al. 2010
<strong>Bodo</strong> <strong>Ziegler</strong>: Kinematic & Structural Evolution of Field & Cluster Spirals - Potsdam 21.9.10<br />
Based on DFG/SPP 1177 funding ZI 663/6<br />
Thanks for your attention!<br />
Have a nice afternoon!
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