TheThe ProjectProject

Mapping the Stellar Kinematics of Nearby GalaxiesMapping the Stellar Kinematics of Nearby Galaxies

J. FalcJ. Falcóón-Barroson-Barroso

Collaborators:Collaborators: M. Balcells, A. Vazdekis, and the M. Balcells, A. Vazdekis, and the SAURONSAURON Team Team

PIs:PIs: R. Bacon R. Bacon ((LyonLyon)), R.L. Davies , R.L. Davies ((OxfordOxford)), P.T. de Zeeuw , P.T. de Zeeuw ((LeidenLeiden))

CoIs:CoIs:

M. BureauM. Bureau, M. Cappellari, E. Emsellem, , M. Cappellari, E. Emsellem, J. FalcJ. Falcóón-Barroson-Barroso, , D. Krajnovic, H. Kuntschner, R. McDermid, D. Krajnovic, H. Kuntschner, R. McDermid, R.F. PeletierR.F. Peletier

Associates:Associates:

R. van den Bosch, Y. Copin, K. Fathi, K. Ganda, B. Gerken, R. van den Bosch, Y. Copin, K. Fathi, K. Ganda, B. Gerken, J. de Jong, E. Jourdeuil, B. Miller, G. Monnet, M. Sarzi, J. de Jong, E. Jourdeuil, B. Miller, G. Monnet, M. Sarzi, T. Statler, G. van de Ven, A. Weijmans,...T. Statler, G. van de Ven, A. Weijmans,...

http://http://www.strw.leidenuniv.nl/sauronwww.strw.leidenuniv.nl/sauron

The TeamThe Team

OutlineOutline Integral field kinematic features in early-type galaxiesIntegral field kinematic features in early-type galaxies

Central disks, KDCs, Kin. Twists, CRCsCentral disks, KDCs, Kin. Twists, CRCs PseudobulgesPseudobulges High spatial resolution stellar kinematics with High spatial resolution stellar kinematics with OASISOASIS A detailed study: NGC7332 A detailed study: NGC7332

A SAURON look at galaxy bulges Projects on bulges Minor-axis stellar kinematics (Flat velocity disp. Profiles)

The The SAURONSAURON Bars Project Bars Project

ConclusionsConclusions

SAURON Stellar Velocity FieldsSAURON Stellar Velocity Fields

Emsellem et al. 2004, MNRAS, in press (astroph/0404034) Emsellem et al. 2004, MNRAS, in press (astroph/0404034)

Stellar Kin: Central Stellar DisksStellar Kin: Central Stellar Disks(Bureau et al. , Emsellem et al.)

Central Disks:• I: Disky isophotes • V: Pinched isovelocities Double-hump• : Max along minor axis Min along major-axis• h

3: Anti-correlated with

V

Kin. Twists: (Triaxiality)•V: Kin. twist/misalignment

KDCs:•V: Abrupt kin. twist Abrupt V change Peculiarities

Strong/weak: (NGC4526, 4459)

NGC4526

NGC4459

Stellar Kin.: Kin. Twists and KDCsStellar Kin.: Kin. Twists and KDCs

Kinematic Twist: (NGC4477)

KDC: (NGC4365)

Central Disks:• I: Disky isophotes • V: Pinched isovelocities Double-hump• : Max along minor axis Min along major-axis• h

3: Anti-correlated with

V

Kin. Twists: (Triaxiality)•V: Kin. twist/misalignment

KDCs:•V: Abrupt kin. twist Abrupt V change Peculiarities

Davies et al. 2001

NGC4477

NGC4365

Stellar Kin.: CRsStellar Kin.: CRs

Others: (Crs; NGC3414, 3608)

NGC3414

NGC3608

Stellar Kin.: OthersStellar Kin.: Others

Others: (CR; NGC4473, 4550)

NGC4473

NGC4550

PseudobulgesPseudobulges

NGC3384

NGC7457

NGC7457

Flat velocity dispersion field

NGC3384

Flat velocity dispersion along the major axis due to a

central disk

Best candidates for pseudobulges in Pinkney et al. 2003

SAURON and OASISSAURON and OASIS

SAURON: global kinematics and line-strengthsSAURON: global kinematics and line-strengths OASIS spatial resolution: zoom-in on nucleusOASIS spatial resolution: zoom-in on nucleus Allows study of orbital structure near central BHAllows study of orbital structure near central BH

McDermid et al. (2004)McDermid et al. (2004)NGC 4382NGC 4382

CDCDCentral DisksCentral Disks

KTKTKin. TwistsKin. Twists

KDCKDCKin. Decoupled Kin. Decoupled

corescores

CRCRCounter-rotating Counter-rotating

corescores

AxiAxiAxisymmetric Axisymmetric

galaxiesgalaxies

EC(/12)EC(/12)Ellipticals ClustersEllipticals Clusters

5 (9) 6 (9) 2 (3) 1 (1) 3 (6)

EF(/12)EF(/12)Ellipticals FieldEllipticals Field

9 (11) 6 (9) 4 (6) 1 (1) 2 (4)

LC(/12)LC(/12)Lenticulars ClustersLenticulars Clusters

10 (10) 4 (5) 2 (2) 3 (3) 2 (5)

LF(/12)LF(/12)Lenticulars FieldLenticulars Field

8 (9) 5 (7) 2 (4) 2 (4) 3 (6)

Total(/48)Total(/48) 32 (39) 21 (30) 10 (15) 7 (9) 10 (21)

Total(%)Total(%) 67 (81) 44 (63) 21 (31) 15 (19) 21 (44)

Central stellar disks pervasive (70-80%) KDCs and counterrotation numerous (>20-30%;

>15-20%) Non- axisymmetries very common (45-60%) Regular axisymmetric objects not as frequent (20-

40%)

Stellar Kin.: Comp. IncidenceStellar Kin.: Comp. Incidence

Ordinary looking Boxy-S0 galaxyRegular stellar kinematics

(Fisher et al. 1994) Plateau in the light profile

(Lutticke et al. 2000) Photometrically detected central disk

(Seifert & Scorza 1996) Complex gas distribution, showing a strong counter-rotating H component and a weak co-rotating one.

(Plana & Boulesteix 1996) Flat H line-strength along major axis

(Bender & Paquet 1999)

AA Case Study: NGC7332 Case Study: NGC7332(Falcón-Barroso et al. 2004)

NGC7332

NGC7339

AA Case Study: NGC7332 Case Study: NGC7332

SAURON FoV

I-band major axis light profile (Peletier & Balcells 1997)

Stellar KinematicsStellar Kinematics

A Kinematically Decoupled Core

Double-peak velocity dispersion

Kinematic Evidence of the Central Disk

Cylindrical Rotation

AA Case Study: NGC7332 Case Study: NGC7332

Double-hump rotation curve

Major-Axis

Complex gas distribution in general with some signs of ordered motion. Off-plane gas clumps

Ionized Gas KinematicsGas Kinematics

AA Case Study: NGC7332 Case Study: NGC7332

Absorption Line StrengthLine Strength

Raw

Clean

AA Case Study: NGC7332 Case Study: NGC7332

Age+MetallicityAge+Metallicity

Interpretation of the Results:

• The presence of a bar • Boxy bulge • Plateau in the light profile• Cylindrical Rotation • Double-hump rotation curve• Velocity dispersion profile with a central minimum and a plateau at moderate radii• Strong h3 – V anti-correlation (revealing the central disk)• Homogeneous stellar populations (being 4-6 Gyr everywhere in the galaxy)

• The origin of the gas

• A tidal interaction with the neighbour galaxy NGC7339

• Evolutionary Scenarios• The bar has certainly affected the evolution of NGC7332• It is also quite possible that interactions played a role in the shaping of NGC7332

AA Case Study: NGC7332 Case Study: NGC7332

A look at galaxy bulgesA look at galaxy bulges

Ongoing projects on bulgesOngoing projects on bulges

24 24 SaSa bulges (as part of the main survey) bulges (as part of the main survey) 11 11 S0-SbcS0-Sbc bulges from the Balcells & Peletier bulges from the Balcells & Peletier

samplesample 22 22 Sb-SmSb-Sm bulges (M. Carollo & R.F. Peletier) bulges (M. Carollo & R.F. Peletier)

The Balcells & Peletier SampleThe Balcells & Peletier Sample

• A sample of highly inclined (i>50º) nearby galaxies to look at pure bulges with no disk contamination.

• Photometry of 45 nearby bulges (Balcells & Peletier 1994)(Andredakis et al. 1995)(Peletier & Balcells 1997)(Balcells et al. 2003, 2004a, 2004b)

• Stellar Populations of 19 bulges(Peletier et al. 1999)(Falcón-Barroso et al. 2002)(Falcón-Barroso et al. 2003a)

• Kinematics of 19 nearby bulges (Falcón-Barroso et al. 2003b)

Long Slit spectroscopy (minor axis) of 19 bulges Long Slit spectroscopy (minor axis) of 19 bulges from the Balcells & Peletier samplefrom the Balcells & Peletier sample

ISIS at WHT (La Palma)ISIS at WHT (La Palma)

Ca II triplet regionCa II triplet region

SSP models from Vazdekis et al. 2003 used as SSP models from Vazdekis et al. 2003 used as templates for kinematicstemplates for kinematics

Minor-Axis Stellar Kinematics in bulgesMinor-Axis Stellar Kinematics in bulges(Falcón-Barroso et al 2003b)

Minor Axis RotationMinor Axis Rotation

Minor-Axis Stellar Kinematics in bulgesMinor-Axis Stellar Kinematics in bulges

Rotation in the inner partsRotation in the inner parts

Velocity Dispersion ProfilesVelocity Dispersion Profiles

• Centrally Peaked Profs.

Classical bulges

Large Vel. Disp. Gradient (<<0)

• Flat Profiles

Bulges dominated by rotation

(Pseudobulges?, Kormendy 1993)

Small Vel. Disp. Gradient (~0)

Minor-Axis Stellar Kinematics in bulgesMinor-Axis Stellar Kinematics in bulges

Velocity dispersion gradientsVelocity dispersion gradients

No correlations were found with bulge luminosity, central velocity dispersion or Sérsic index n

Barred or box-peanut bulges

Non-Barred bulges

Minor-Axis Stellar Kinematics in bulgesMinor-Axis Stellar Kinematics in bulges

2 strong barred galaxies observed (Aug 2003)2 strong barred galaxies observed (Aug 2003) NGC936NGC936 NGC6951NGC6951

The Bar ProjectThe Bar Project(JourdeuilJourdeuil et al.)

Scientific GoalsScientific Goals 2D application of the 2D application of the

Tremaine-Weinberg method Tremaine-Weinberg method to measure pattern speeds to measure pattern speeds and quantify uncertainties in and quantify uncertainties in 1D data1D data

Detailed study of the orbital Detailed study of the orbital structure using N-body structure using N-body simulationssimulations

Link between the orbital Link between the orbital structure and the stellar structure and the stellar populationspopulations

ConclusionsConclusions Stellar kinematics exhibits rich variety:

(central disks pervasive; KDCs/CRs numerous; non-axisymmetry common) Number of KDCs/CRs likely to increase with higher spatial resolution (i.e. OASIS)

NGC7332 shows evidence for hosting a bar + signatures for recent interactions (with neighbour galaxy NGC7339?)

Big SAURON effort on spiral bulges (3 complementary samples are being studied) Long slit minor axis stellar kinematics, on the Balcells & Peletier sample, show a wide

range of velocity dispersion profiles Both, flattened bulges and galaxies with brighter face-on disk central surface brightness

showing shallower velocity dispersion profiles

A specific SAURON project on barred galaxies has started with the main goal of studying in detail the orbital distribution its link with stellar populations