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GEPI, Obs. Paris: F. Hammer, H. Flores, & C. Balkowski LAM : P. Amram MPE, Garching : M. Lehnert Stockholm Obs. : G. Östlin, T. Marquart Galaxy kinematics.

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Presentation on theme: "GEPI, Obs. Paris: F. Hammer, H. Flores, & C. Balkowski LAM : P. Amram MPE, Garching : M. Lehnert Stockholm Obs. : G. Östlin, T. Marquart Galaxy kinematics."— Presentation transcript:

1 GEPI, Obs. Paris: F. Hammer, H. Flores, & C. Balkowski LAM : P. Amram MPE, Garching : M. Lehnert Stockholm Obs. : G. Östlin, T. Marquart Galaxy kinematics at z ~ 1 Mathieu PUECH Post-Doc GEPI – Obs. Paris

2 FLAMES/GIRAFFE on the UT2 MEDUSE, 132 mono-fibers, 1.2 IFU, IFU, 15 x 3x2arrays (20 sq. lenses, 0.52) ARGUS, ARGUS, 11x7 array (300 sq. lenses) 3 modes 15 IFUs deployable over a 20 arcmin FoV with R~10000

3 35 galaxies with Å: T int ~ hrs 32 galaxies with enough S/N (at least 4 pixels with S/N([OII]) > 5) CFRS , z=0.46, (3x2) Preliminary program : 6 nights on distant galaxies R> at rest: the [OII] doublet can be resolved All but 6 galaxies show a well resolved [OII] doublet. Only pixels with S/N > 3 5x5 linear interpolation

4 Also sigma maps… Provided by: the absence of cross-talk between individual spectra. from Blais-Ouellete, Amram et al, 2002 (Fabry-Perot/Halpha) GIRAFFE z=0.6 pixel = random_motions V large_scale_motions

5 Also sigma maps… pixel = random_motions V large_scale_motions At low spatial resolution, dispersion maps of rotating disks do show a peak in their dynamical center Velocity map Dispersion or map

6 And we find rotating disks at z ~ 0.6 HST/F814W Velocity field sigma map Maps from Puech et al (2006a) & Flores et al (2006) Rotating disks : 31 % of the sample Rotation is seen in the VF and the sigma map is peaked in the dynamical center

7 but also « perturbed » rotations HST/F814W Velocity fieldsigma map Maps from Puech et al (2006a) & Flores et al (2006) Perturbed rotations: 20% of the sample Rotation is seen in the VF but the sigma map is perturbed

8 and much complex kinematics HST/F814WVelocity fieldsigma map Maps from Puech et al (2006a) & Flores et al (2006) Complex kinematics: 40% of the sample

9 FP velocity field ESO 400-G43 (Ostlin et al, 2001) Simulated Giraffe IFU observation (degraded spatial resolution, z=0.6) Perturbed/complex VFs are real!! - FP observations of 20 GHASP galaxies (Amram et al, 2002) simulations of 60 data-cubes at different z rotating disks are recovered - FP observations of complex velocity fields: Comparison to local (Fabry-Perot)

10 CFRS CFRS CFRS HDFS4070 observée modélisée A simple test of the classification We assume all galaxies to be rotating disks, i.e. their large scale motions to be rotational We can simply compared the derived maps to the observed ones: Amplitude ratio versus peak distances

11 Galaxy kinematics at z ~ 0.6: some numbers A (small) complete sample of 35 galaxies: I AB 22.5 ; W 0 (OII) > 15A and 0.4 z 0.75 ==> representative of emission line galaxies at z= 0.6 (M B representative of emission line galaxies at z= 0.6 (M B < -19.5) - Simple classification using VF+sigma+ HST morphology: rotating disks: 31%; perturbed/complex: 60%; undetermined: 9% - Accounting for all IAB< 22.5 (i.e. including quiescent E/S0/…): we do find that 26-40% of them are not relaxed systems ! GIRAFFE/multiple IFUs: unique tool to study the kinematics of distant galaxies

12 Conselice et al (2005) KECK/LRIS (long slit) Conselice et al (2005) Tully-Fischer relation at z ~ 0.6 (K band) VLT/GIRAFFE-IFUs Flores et al (2006)

13 Conselice et al (2005) KECK/LRIS (long slit) Conselice et al (2005) VLT/GIRAFFE-IFUs Flores et al (2006) Complex Kinematics Perturbed Rotations Rotating Disks

14 Conselice et al (2005) KECK/LRIS (long slit) Conselice et al (2005) VLT/GIRAFFE-IFUs Flores et al (2006) Scatter is related to interlopers (non relaxed kinematics)

15 Local TF (Verjeinhen 2001)TF at z=0.6 (Flores et al, 2006) Tully-Fischer not evolving ? We need statistics !!!

16 Specific Angular Momentum Evidence for a non linear growth of j disk Evidence for through merging ? Robustness of the dynamical classification Puech et al. 2006, in revision j disk =2R d V max

17 Comparison with simulations * perturbed rotations = minor mergers ? * complex kinematics = major mergers ? to be compared with hydrodynamical codes (Simulations by T.J. Cox) Puech s PhD thesis Puech et al., in preparation

18 Conclusion 1- Since z=0.4, galaxy dynamics is too complex to be sampled by slits is this a definitive claim ? 2- Requires multi-IFUs to sample > 50 rotating disks (among > 150 distant galaxies); goal is to verify the absence of TF evolution ~ analysis of 40 new CDFS galaxies in progress ; ~ 50 more will be observed this semester 3- High rate of merging (major/minor) or could this be recovered by other scenarios (smooth gas accretion) ?


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