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DES GALAXIES PROCHES AUX GALAXIES LOINTAINES ETUDES CINEMATIQUE ET DYNAMIQUE Benoît Epinat Supervisor: Philippe Amram (LAM) Co-supervisor: Chantal Balkowski.

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Presentation on theme: "DES GALAXIES PROCHES AUX GALAXIES LOINTAINES ETUDES CINEMATIQUE ET DYNAMIQUE Benoît Epinat Supervisor: Philippe Amram (LAM) Co-supervisor: Chantal Balkowski."— Presentation transcript:

1 DES GALAXIES PROCHES AUX GALAXIES LOINTAINES ETUDES CINEMATIQUE ET DYNAMIQUE Benoît Epinat Supervisor: Philippe Amram (LAM) Co-supervisor: Chantal Balkowski (GEPI) FROM NEARBY TO HIGH REDSHIFT GALAXIES KINEMATICAL AND DYNAMICAL STUDIES

2 06/11/2008 - LAM2 First Part - Galaxy formation and evolution A. Galaxy formation & Mass assembly B. The need for kinematical observations Second Part - The GHASP sample A. A 3D kinematical sample of local galaxies B. Galaxies with rotating disks C. Some local results Third Part - High redshift kinematics A. Overview of kinematical high-z observations B. Projection of GHASP sample at high redshift C. Observational biases D. Evolution of galaxy kinematics

3 06/11/2008 - LAM 3 Cosmological scenario Time

4 06/11/2008 - LAM 4 Formation of galactic disks Haloes form from initial density fluctuations Gas collapses into haloes Stars form Abraham & van den Berg 2000

5 06/11/2008 - LAM 5 Cosmological scenario Time

6 06/11/2008 - LAM 6 Mass assembly - Formation and evolution of galaxies Abraham & van den Berg 2000 Haloes form from initial density fluctuations Gas collapses into haloes Stars form Continuous gas accretion? Minor mergers? Major mergers? Angular momentum

7 06/11/2008 - LAM 7 Mass assembly Intermediate redshift mergers (HST, Hubble Deep Field) How to follow mass assembly? Stellar masses: Broad band imagery Spectrophotometry Halo masses dynamical mass Coalescence (Mergers) morphology kinematics HST

8 06/11/2008 - LAM 8 Galaxy evolution Time z=2.5

9 06/11/2008 - LAM 9 Galaxy evolution BzK 15504 z=2.4 M star =8.10 10 M sol M gas =4.10 10 M sol V=230 km/s V/  ~5 SFR~140 M sol /yr Gas consumption timescale: 285 Myr Genzel et al. 2006, 2008 VF HH

10 06/11/2008 - LAM 10 Galaxy evolution Time z=2.5 z=0.6 z=0 ?

11 06/11/2008 - LAM 11 Galaxy evolution Genzel et al. 2006, 2008 BzK 15504, z=2.4 Yang et al. 2008 J033249.53-274630.0, z=0.5 Epinat et al. 2008 M63, Local galaxy Lemoine Busserole et al. in prep VVDS22001425, z=1.3 HH Velocity field HST VF HH WE NEED TO DISENTANGLE EVOLUTION EFFECTS FROM RESOLUTION EFFECTS ON KINEMATICAL DATA USE OF A LOCAL KINEMATICAL REFERENCE SAMPLE

12 06/11/2008 - LAM12 First Part - Galaxy formation and evolution A. Galaxy formation & Mass assembly B. The need for kinematical observations Second Part - The GHASP sample A. A 3D kinematical sample of local galaxies B. Galaxies with rotating disks C. Some local results Third Part - High redshift kinematics A. Overview of kinematical high-z observations B. Projection of GHASP sample at high redshift C. Observational biases D. Evolution of galaxy kinematics

13 06/11/2008 - LAM 13 Dwarfs, Irregulars Blue compact Local reference sample: GHASP (Gassendi H  survey of SPirals) Morphological Type Environment/ Galaxy density Early-type Gaseous Disk Intermediate Barred & non-Barred Galaxies HSB & LSB Mass Luminosity Field Pairs Compact Groups Groups Late-type GHASP: ~ 203 nearby galaxies -15<Mb<-22 Sa to irregular

14 06/11/2008 - LAM 14 Scanning Fabry-Perot datacubes He-Ne source Observed at OHP

15 06/11/2008 - LAM 15 Fabry-Perot Data Reduction Wavelength calibration Sky subtraction Smoothing/adaptive binning Cappellari et Copin 2003

16 06/11/2008 - LAM 16 Adaptive binning vs gaussian smoothing Epinat et al. 2008 Garrido et al. 2005 Spatial coverage is increased More diffuse emission is detected Independent bins

17 06/11/2008 - LAM 17 Fabry-Perot Data Reduction Wavelength calibration Sky subtraction Smoothing/adaptive binning High quality 3D datacubes: High resolution (~10 km/s and seeing limited) Independent bins Cappellari et Copin 2003

18 06/11/2008 - LAM 18 UGC 7901 Epinat et al. 2008 Kinematics from H  line observations Adaptive binning Doppler-Fizeau 0 =6562.8 A HH VF  map

19 06/11/2008 - LAM 19 UGC 8334 (Sbc) Epinat et al. 2008 DSS-B  map Velocity Field HH The GHASP sample

20 06/11/2008 - LAM 20 DSS-B  map Velocity Field HH UGC 5786 (SAB(r)b) Epinat et al. 2008 The GHASP sample

21 06/11/2008 - LAM 21 UGC 4820 (S(r)ab) Epinat et al. 2008 DSS-B  map Velocity Field HH The GHASP sample

22 06/11/2008 - LAM 22 The GHASP sample fully reduced with a unique method

23 06/11/2008 - LAM 23 The GHASP sample: velocity field modelling -= Residuals Observed Velocity FieldAxi-symmetric model Parameters : X,Y, PA, i, V sys, V  (r) 22 For rotating disks, V  is preponderant Motions are observed in the plane of the disk   Each point of the RC contains 25 bins A bin may contain up to 100 pixels !

24 06/11/2008 - LAM 24 Error bars: Monte Carlo method Model residual VF Model perturbed VF Residual velocity field Set of parameters Statistics give the error bars: DX, DY, DI, DPA, DVsys X 2,Y 2 I 2, PA 2 Vsys 2 X 1,Y 1 I 1, PA 1 Vsys 1... X 3,Y 3 I 3, PA 3 Vsys 3 X n,Y n I n, PA n Vsys n TF power spectrum with Random phase

25 06/11/2008 - LAM 25 ● Galaxies Low inclination galaxies (<25°) ● Ambiguous morphological PA Epinat et al. 2008 Comparison with morphological data

26 06/11/2008 - LAM 26 ● Galaxies ΔPA > 20° ● Ambiguous morphological PA Epinat et al. 2008 Comparison with morphological data

27 06/11/2008 - LAM 27 Morphological type ● 0->2 ✔ 2->4 4->6 6->8 8->10 Tully & Pierce 2001 HI data Best fit Epinat et al. 2008 Local Tully-Fisher relation

28 06/11/2008 - LAM 28 Local data Conclusions & Perspectives ● Kinematical parameters in agreement with morphological parameters ● Maximum velocity is reached within optical disk ● Complete kinematical study of GHASP sample – RC shape – Halo shape from mass modelling – Bar signature – Gaseous velocity dispersion – Kinematical classification

29 06/11/2008 - LAM29 First Part - Galaxy formation and evolution A. Galaxy formation & Mass assembly B. The need for kinematical observations Second Part - The GHASP sample A. A 3D kinematical sample of local galaxies B. Galaxies with rotating disks C. Some local results Third Part - High redshift kinematics A. Overview of kinematical high-z observations B. Projection of GHASP sample at high redshift C. Observational biases D. Evolution of galaxy kinematics

30 06/11/2008 - LAM 30 On the VLT FLAMES/GIRAFFE : No AO but 15 IFU - seeing : from 0.4'' to 0.8'' - pixel : 0.52'' high spectral resolution : ~ 25km/s SINFONI : No AO - seeing up to 0.5'' - pixel : 0.125'' AO - seeing up to 0.2'' - pixel : 0.05'' low spectral resolution : ~100 km/s On the Keck OSIRIS : AO - seeing up to better than 0.1'' - pixel : 0.1'' low spectral resolution : ~100 km/s Integral Field capabilities BzK-15504 (z = 2.38) Genzel et al. 2006, 2008  map Flores et al. 2006  map VF Lemoine-Busseroles et al. in prep  map VF

31 06/11/2008 - LAM 31 Simulation of high-z galaxies Simulation at z=1.7 ➔ lowest angular size with standard cosmological constants Seeing of 0.5" ➔ no AO Pixel size of 0.125" ➔ SINFONI configuration Cosmological parameters: H 0 =71km/s/Mpc  m =0.27   =0.27

32 06/11/2008 - LAM 32 Projection of GHASP at high-z Wavelength calibrated, sky subtracted and non-smoothed cube For each slice of the cube (wavelength): mask to lower sky contribution and foregroung stars smoothing taking into account actual distance and the scale for z=1.7 to simulate the seeing without AO (0.5") UGC 7901 HH

33 06/11/2008 - LAM 33 Simulations of high-z galaxies Wavelength calibrated, sky subtracted and non-smoothed cube For each slice of the cube (wavelength): mask to lower sky contribution and foregroung stars smoothing taking into account actual distance and the scale for z=1.7 to simulate the seeing without AO (0.5") binning to simulate the pixel size (0.125") no noise additon UGC 7901 HH

34 06/11/2008 - LAM 34 Resulting maps UGC 7901 153/203 GHASP galaxies have been projected at z=1.7 HH Velocity field  map 'Redshifted' Local

35 06/11/2008 - LAM 35 z=1.7 z=0 Px = 0.68” Seeing = 2 ” Px = 0.125” Seeing = 0.5 ” the size of the galaxy is enlarged (seeing)‏ but, in the same time, the size of the galaxy is diminished (flux)‏ the inclination is lowered when the Beam Smearing Parameter decreases the velocity gradient is lowered in the inner RC but, in the same time, the velocity gradient is enlarged in the outer RC What are the biases?

36 06/11/2008 - LAM 36 Dispersion at High redshift Central peak elongated toward minor axis ➢ Unresolved velocity gradient  map, z=1.7  map, local Velocity field, high resolution

37 06/11/2008 - LAM 37 Rotating disk (RD) ‏ Perturbed rotations (PR)‏ Complex kinematics (CK)‏ What are the biases ? e.g. Flores et al. 2006, Yang et al. 2008 Classification of the kinematics of distant galaxies  map VF  map VF  map VF

38 06/11/2008 - LAM 38 Classification of the kinematics of distant galaxies Rotating disk (RD)‏ YES: General case YES: Inner ring  map HH VF HH  map VF

39 06/11/2008 - LAM 39 Rotating disk (RD)‏ misclassified NO: Solid body rotation curve NO: Low velocity gradient Classification of the kinematics of distant galaxies  map HH VF  map HH VF

40 06/11/2008 - LAM 40 Rotating disk (RD) misclassified‏ NO: Asymmetry in the H  distribution Close pairs seen as RD? Classification of the kinematics of distant galaxies  map HH VF  map HH VF ~70% of regular GHASP rotating disks are classified correctly

41 06/11/2008 - LAM 41 UGC 5556 – DSS B UGC 5556 –  UGC 5556 – VF UGC 5556 @ z=1.7 Seeing=0.5”, px=0.125”  VF Strong bars

42 06/11/2008 - LAM 42  Fit on 2D maps : velocity field  Seeing is taken into account  2 parameter RC models  Outputs: Center Inclination PA Vsys Vmax Rc Model fitting   minimisation cube modelling map modelling Exponential disk Forster Schreiber et al. 2006 Isothermal sphere Arctangent Puech et al. 2006 'Flat' model Wright et al. 2007

43 06/11/2008 - LAM 43 Cube modelling Low resolution datacube: Smoothing and binning each slice Low resolution map extraction Time consuming

44 06/11/2008 - LAM 44 Map modelling = High resolution flux map is not known! Oversampling of the high-z flux map Faster and Similar result

45 06/11/2008 - LAM 45 Model fitting Signature of the velocity shear Local velocity dispersion = _ 2 2

46 06/11/2008 - LAM 46 Model fitting 'Observed' maps Model Residuals Dispersion maps Velocity fields Rotation curve

47 06/11/2008 - LAM 47 Kinematical major axis at high-z Position angle of major kinematical axis is constrained correctly Better constrained for larger galaxies

48 06/11/2008 - LAM 48 Kinematical inclination at high-z Non accurate for the smallest galaxies Error does not depend on the inclination Effect on the maximum velocity determination Better constrained using high resolution broad band images Inclination is fixed in the fitting procedure

49 06/11/2008 - LAM 49 Along major axis -> under estimated Model -> statistically good Maximum circular velocity at high-z

50 06/11/2008 - LAM 50 Local -> rather constant No correction -> under estimated Model corrected -> statistically good - - z=0.6 (corrected) -> slightly higher - - z>1 (corrected) -> higher Local velocity dispersion at high-z Instrumental and methodological biases? Evolution of the velocity dispersion?

51 06/11/2008 - LAM 51 Lemoine Busserole et al in prep – no AO, MASSIV pilot run z=1.31 z=1.46 z=1.40 z=1.31 projected data using model ➢ projected data without model high redshift data z>1 Dynamical support evolution? High-z galaxies display rotation High-z galaxies display large dispersion -> change in the dynamical support -> signs of dynamical evolution

52 06/11/2008 - LAM 52 Conclusion & Perspectives A) "Recipes" to analyse high-z galaxies – Among the four models: "flat" model – Inclination needs high resolution broad band imagery – Position angle of major axis correctly is constrained by kinematical data – Maximum velocity is statistically recovered – Velocity dispersion can be corrected from unresolved velocity gradient – Modelling can be improved by the use of high resolution line flux maps

53 06/11/2008 - LAM 53 Conclusion & Perspectives B) High-z data vs projected local data – Same observational biases allow comparison and disentangle distance effect from evolutionary effects – B>3 needed to retrieve kinematical parameters – B>10 needed to constrain halo shapes – High-z disks show higher velocity dispersion than local galaxies. These disks, probably thick may be transient and progenitor of bulge or thick star disks

54 06/11/2008 - LAM 54 Conclusion & Perspectives C) What are the mechanisms of disk formation? – Continuous gaz accretion of clumps? (e.g. Immeli, 2004 ; Bournaud et al. 2007,2008 ; Genzel et al 2008) – Major or minor merging events? (Robertson & Bullock, 2008; Puech et al 2008) – Present high-z samples are biased: bright and massive ➔ More kinematical signatures of high-z disks are necessary ➔ Implication in MASSIV large program: Representative sample of ~100 galaxies at redshift z~1.5 observed with SINFONI facility

55 06/11/2008 - LAM 55 Conclusion & Perspectives D) High-z simulation perspectives – Probe the angular momentum and Tully-Fisher relation evolution from IMAGES sample (GIRAFFE) at z=0.6, MASSIV sample at z=1.5 and local data – Probe the spectral resolution effects on the data (R=15000-> R=3000) – Use various nearby samples (Barred, Compact Groups, Mergers, Blue Compact Galaxies, LSB,...)  FP database (www.fabryperot.oamp.fr)www.fabryperot.oamp.fr

56 06/11/2008 - LAM 56 Dwarfs, Irregulars Blue compact Local reference sample: GHASP (Gassendi H  survey of SPirals) Morphological Type Environment/ Galaxy density Early-type Gaseous Disk Intermediate Barred & non-Barred Galaxies HSB & LSB Mass Luminosity Field Pairs Compact Groups Groups Late-type GHASP: ~ 203 nearby galaxies -15<Mb<-22 Sa to irregular

57 06/11/2008 - LAM 57 ~ 570 galaxies TOTAL Samples of nearby galaxies - Fabry-Perot data http://FabryPerot.oamp.fr

58 06/11/2008 - LAM 58 HCG 31 Color H  velocity Field (Amram et al. 2004) White HI isovelocities (Verdes Montenegro et al 2005)  map VF R band

59 06/11/2008 - LAM 59 Conclusion & Perspectives D) High-z simulation perspectives – Probe the angular momentum and Tully-Fisher relation evolution from IMAGES sample (GIRAFFE) at z=0.6, MASSIV sample at z=1.5 and local data – Probe the spectral resolution effects on the data (R=15000-> R=3000) – Use various nearby samples (Barred, Compact Groups, Mergers, Blue Compact Galaxies, LSB,...)  FP database (www.fabryperot.oamp.fr)www.fabryperot.oamp.fr – Simulations in the frame of: ● GIRAFFE, SINFONI, OSIRIS ● KMOS, MUSE, 3DNTT ● E-ELT (EAGLE)

60 06/11/2008 - LAM 60 That's all Folks!

61 06/11/2008 - LAM 61 High redshift samples GHASP IMAGES (GIRAFFE) SINS (SINFONI) Cosmological evolution? Selection bias on high-z data?

62 06/11/2008 - LAM 62 Kinematical data are needed disentangle mergers and non mergers disentangle major mergers and minor mergers compare transient disk and evolved disks compute angular momentum compute halo mass compute halo shapes WE NEED TO DISENTANGLE EVOLUTION EFFECTS FROM RESOLUTION EFFECTS ON KINEMATICAL DATA USE OF A LOCAL KINEMATICAL REFERENCE SAMPLE

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