Galaxy CentersGalaxy Centers

Early- and late-type galaxiesEarly- and late-type galaxies Nuclei of E/S0 galaxies Nuclei of E/S0 galaxies

– Power of integral-field spectroscopyPower of integral-field spectroscopy– Black hole masses from stellar kinematics Black hole masses from stellar kinematics – Emission-line gas and activityEmission-line gas and activity

Nuclei of late-type galaxiesNuclei of late-type galaxies– Classical and exponential ‘bulges’Classical and exponential ‘bulges’– Central Compact SourcesCentral Compact Sources

Opportunities for HSTOpportunities for HST

Tim de ZeeuwTim de Zeeuw

Two families of galaxies Two families of galaxies `Early-type’ galaxies `Early-type’ galaxies

– RR1/41/4 bulges, high surface brightness, red, old stars bulges, high surface brightness, red, old stars– Global and nuclear properties correlateGlobal and nuclear properties correlate– Emission-line studies: >Emission-line studies: >75% have ‘activity’ 75% have ‘activity’ BH BH– More powerful AGN: more evidence for young stars More powerful AGN: more evidence for young stars

`Late-type’ galaxies `Late-type’ galaxies – Young stars, low SB Young stars, low SB – Strong line-strength gradientsStrong line-strength gradients– Many: bulgeless disks (M33)Many: bulgeless disks (M33)– Often: nuclear star clusterOften: nuclear star cluster– ~0% AGN ~0% AGN no BH no BH

(but cf NGC 4395) (but cf NGC 4395) SDSSSDSS

Integral-field SpectroscopyIntegral-field Spectroscopy

GalaxyGalaxy ImageImage

Velocity fieldVelocity field

Velocity curveVelocity curve

IntegralIntegral fieldfield

LongLong slitslit

Rich Physical Content Rich Physical Content Total fluxTotal flux

– Morphology, photometryMorphology, photometry

Absorption linesAbsorption lines– Stellar kinematicsStellar kinematics

LOSVD (V,LOSVD (V,,h3,h4),h3,h4)

– Line strength indexLine strength index HH, Mgb, Fe5015, Fe5270, Mgb, Fe5015, Fe5270

Emission linesEmission lines– Gas distributionGas distribution

HH, [OIII], [NI], [OIII], [NI] Line ratiosLine ratios

– Gas kinematicsGas kinematics V(HV(H, V([OIII]), FWHM(H, V([OIII]), FWHM(H, ,

FWHM([OIII])FWHM([OIII])

Reconstructed V imageStellar Velocity FieldMgb Line Index[OIII] Line intensityGas Velocity Field

48 representative E/S0 48 representative E/S0 Galaxies Galaxies

Emsellem, Cappellari et al. 2004, MNRAS, in pressEmsellem, Cappellari et al. 2004, MNRAS, in press

Stellar Velocity Stellar Velocity FieldsFields

HST and HST and

i=20° i=46° i=79°

Stellar Velocity FieldsStellar Velocity Fields

McDermid, Shapiro, et al. 2004, AN, 325, 100McDermid, Shapiro, et al. 2004, AN, 325, 100

2’’2’’

Kinematic structure on all Kinematic structure on all scales scales

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 Single slit STIS: incomplete view on smaller scales?Single slit STIS: incomplete view on smaller scales?

McDermid et al., 2004, AN, 325, 100 McDermid et al., 2004, AN, 325, 100 NGC 4382NGC 4382

The Black Hole in M32The Black Hole in M32

Use stellar absorption-line spectroscopy:Use stellar absorption-line spectroscopy:– Integral-field data to measure intrinsic shape and M/LIntegral-field data to measure intrinsic shape and M/L– HST/STIS to measure BH massHST/STIS to measure BH mass

Fit with numerical dynamical modelsFit with numerical dynamical models

Small companion of Small companion of Andromeda NebulaAndromeda Nebula

D ~ 0.8 MpcD ~ 0.8 Mpc

MMBHBH ~ ~ 3 x 103 x 1066 M Mּסּס

Influences kinematics Influences kinematics inside inside ~ ~ 0.10.1""

M32

M32: Best-fitting M32: Best-fitting ParametersParameters

Dynamical models for stellar Dynamical models for stellar motions have 3 parameters: motions have 3 parameters: M/L, MM/L, MBHBH, and inclination, and inclination

These are tightly constrained These are tightly constrained by STIS and SAURON databy STIS and SAURON data

Significant improvement over Significant improvement over STIS + 4 slits from groundSTIS + 4 slits from ground

MMBHBH = (2.5 = (2.5 ± ± 0.4) x 100.4) x 1066 M Mּסּס (cf. (cf.

van der Marel et al. 1998, ApJ, 493, 613)van der Marel et al. 1998, ApJ, 493, 613)3 level

Verolme et al. 2002, MNRAS, 335, 517Verolme et al. 2002, MNRAS, 335, 517

External check: NGC 821 (E6)External check: NGC 821 (E6) Same data setSame data set

– STIS major axisSTIS major axis– SAURON large scaleSAURON large scale

Independent codesIndependent codes– Nukers/Leiden groupNukers/Leiden group– Different orbit samplingDifferent orbit sampling– Different smoothingDifferent smoothing

Good agreementGood agreement– MMBHBH error decreases error decreases

when two-dimensional when two-dimensional kinematics is includedkinematics is included

– MMBHBH error ~30% error ~30% Gebhardt 2004, Carnegie symposiumGebhardt 2004, Carnegie symposium

Importance of 2D kinematicsImportance of 2D kinematics

Model fits major-axis kinematics perfectlyModel fits major-axis kinematics perfectly Little can be recovered of the true orbital Little can be recovered of the true orbital

structure from incomplete kinematic coveragestructure from incomplete kinematic coverage

Symmetrized Symmetrized data for NGC data for NGC 44734473

Axisymmetric Axisymmetric modelmodel

VV hh33 hh44

MMBHBH from Stellar Kinematics from Stellar Kinematics BH masses for ~20 E/S0 galaxies and bulgesBH masses for ~20 E/S0 galaxies and bulges

– Based on one STIS slit, and ~2 ground-based slits Based on one STIS slit, and ~2 ground-based slits

– MMBHBH accuracy can be improved by using accuracy can be improved by using integral-fieldintegral-field data; data;

this also provides accurate M/L’s and inclinationsthis also provides accurate M/L’s and inclinations– Possible for all nearby E/S0s in HST/STIS archivePossible for all nearby E/S0s in HST/STIS archive

LimitationsLimitations– Only for bright nearby nucleiOnly for bright nearby nuclei– Modest spatial resolution at Virgo (0.2'' slit)Modest spatial resolution at Virgo (0.2'' slit)– Not enough S/N for core galaxies in Virgo: these are Not enough S/N for core galaxies in Virgo: these are

targets for AO-assisted IFU’s on 8m groundbased targets for AO-assisted IFU’s on 8m groundbased telescopes (e.g. SINFONI on VLT) telescopes (e.g. SINFONI on VLT)

The S0 galaxy NGC 3245The S0 galaxy NGC 3245

Barth, Sarzi, et al 2001, ApJ, 555, 685Barth, Sarzi, et al 2001, ApJ, 555, 685 MMBH BH ~ 2.1 x 10~ 2.1 x 1088 M M

Nuclear emission-line gas Nuclear emission-line gas Prominent in active nuclei and spiral bulgesProminent in active nuclei and spiral bulges

– ~20% have regular dust disks~20% have regular dust disks– HH, [NII] kinematics from STIS resolves region where , [NII] kinematics from STIS resolves region where

black hole dominates motion, but is often irregular black hole dominates motion, but is often irregular

About 100 objects observed with HSTAbout 100 objects observed with HST– Up to ~100 Mpc distance; often multiple parallel slitsUp to ~100 Mpc distance; often multiple parallel slits– ~20% can be ~fitted with circular rotation ~20% can be ~fitted with circular rotation – Modest number of published black hole masses Modest number of published black hole masses

Few cases with MFew cases with MBHBH from gas from gas andand from stars from stars– Mixed results: good agreement in one case Mixed results: good agreement in one case – Important to test this in carefully selected galaxiesImportant to test this in carefully selected galaxies– Improved kinematic (hydrodynamic) model needed Improved kinematic (hydrodynamic) model needed

Verdoes Kleijn et al., 1999, AJ, 118, 2592Verdoes Kleijn et al., 1999, AJ, 118, 2592WFPC2 V-bandWFPC2 V-band

Nearby Radio GalaxiesNearby Radio Galaxies

All have emission-line gas; many dust disks/lanesAll have emission-line gas; many dust disks/lanes Dust distribution in radio- and in quiescent galaxies Dust distribution in radio- and in quiescent galaxies

very similarvery similar Jets nearly perpendicular to dust except when dust Jets nearly perpendicular to dust except when dust

is aligned with major axis is aligned with major axis (e.g., Schmitt et al. 2002; Verdoes & de Zeeuw astro-ph/0405034)(e.g., Schmitt et al. 2002; Verdoes & de Zeeuw astro-ph/0405034)

Trigger of activity: likely related to stellar/gaseous Trigger of activity: likely related to stellar/gaseous kinematics on small scales kinematics on small scales

This can be probed with STIS multiple parallel slitsThis can be probed with STIS multiple parallel slits

Late-type galaxiesLate-type galaxiesF606W, F160W & F110WF606W, F160W & F110W

Sb and Sc galaxiesSb and Sc galaxies HST allows study of HST allows study of

bulges with effective bulges with effective radii Rradii Ree smaller than 1’’ smaller than 1’’

Surveys reveal large Surveys reveal large nuclear complexity in nuclear complexity in late-type spiralslate-type spirals

Here: results from Here: results from survey of ~100 nearby survey of ~100 nearby Sb & Sc galaxies with Sb & Sc galaxies with WFC2 & NICMOSWFC2 & NICMOS

9”9”

Carollo, Stiavelli, de Zeeuw, et al. 1997-2002Carollo, Stiavelli, de Zeeuw, et al. 1997-2002

Structure of smallest bulgesStructure of smallest bulges

HST allows extension HST allows extension of earlier ground-based of earlier ground-based studies to smallest studies to smallest scales scales

Many ~exponential Many ~exponential stellar density profilesstellar density profiles

These ‘bulges’ may be These ‘bulges’ may be disks disks (e.g. Kormendy 1993) (e.g. Kormendy 1993)

Formation mechanism Formation mechanism is currently unclearis currently unclear

~400 pc~400 pc

Central Compact SourcesCentral Compact Sources

Late-type bulges Late-type bulges often host central often host central compact sourcescompact sources– Most are resolved Most are resolved

on pc scaleson pc scales– Radii up to 20 pcRadii up to 20 pc

70% of spirals 70% of spirals hosts CCShosts CCS

Structural ParametersStructural Parameters Narrow RNarrow R1/41/4 sequence sequence

down to ~ 300 pcdown to ~ 300 pc Exponential bulges Exponential bulges

bridge dwarf and Rbridge dwarf and R1/41/4 sequencessequences

Central Compact Central Compact Sources intermediate Sources intermediate between MW GC’s & between MW GC’s & young star clustersyoung star clusters

Central Compact SourcesCentral Compact Sources● Many CCS: like star clusters of 10Many CCS: like star clusters of 106 6 - 10- 108 8 MM

● Others: colors influenced by activity/dustOthers: colors influenced by activity/dust● Very difficult to detect black holes inside a CCS Very difficult to detect black holes inside a CCS

Bruzual & Charlot tracksfor a 3x106 M cluster

13 Gyrs

13 Gyrs

100 Myrs

Stellar Populations of Bulges Stellar Populations of Bulges

Massive RMassive R1/41/4 bulges bulges – Mean age 8-10 GyrMean age 8-10 Gyr– Age spread Age spread ~2 Gyr~2 Gyr

Small bulges Small bulges – Mean age 2-5 GyrMean age 2-5 Gyr– Age spread 10 GyrAge spread 10 Gyr

Small bulges younger Small bulges younger than massive spheroids, than massive spheroids, similar age as host disksimilar age as host disk

V-HV-H~0.9~0.9(V-H)~0.4(V-H)~0.4

V-HV-H~1.4~1.4(V-H)~0.1(V-H)~0.1

Carollo, Stiavelli, et al.

+ F330W (HRC)

NGC3259

Next stepsNext steps ACS follow-up ACS follow-up

– Cycle 11; 25 orbits; Cycle 11; 25 orbits; – B, I and U (HRC)B, I and U (HRC)– Improved age and Improved age and

metallicity estimatesmetallicity estimates

STIS follow-upSTIS follow-up– Cycle 13; 35 orbitsCycle 13; 35 orbits– V and V and of 2 CCS of 2 CCS– Provides mass, and Provides mass, and

rotational support rotational support

HST resolution HST resolution cannot be matched cannot be matched from groundfrom ground

Opportunities for HSTOpportunities for HST Stellar absorption-line studies of E/S0 galaxies Stellar absorption-line studies of E/S0 galaxies

– No need for additional single STIS slitsNo need for additional single STIS slits– Useful to study some nuclei at multiple position anglesUseful to study some nuclei at multiple position angles

Emission-line gasEmission-line gas– Map small number of carefully chosen nearby nucleiMap small number of carefully chosen nearby nuclei

– Will provide MWill provide MBHBH, and may establish trigger of activity , and may establish trigger of activity

Late-type galaxiesLate-type galaxies– HST can make key contribution by imaging and HST can make key contribution by imaging and

spectroscopy of compact nuclei and exponential ‘bulges’spectroscopy of compact nuclei and exponential ‘bulges’– Will help establish formation mechanismWill help establish formation mechanism

Next step: fly an integral-field spectrograph on RM2Next step: fly an integral-field spectrograph on RM2

Slow RotatorsSlow Rotators

EE

E

E

S0 E

EE

EE

E

E

General agreement with RC3General agreement with RC3

Fast RotatorsFast Rotators

S0

S0 S0

S0

S0 E

E

EE

E

E E

S0 S0

S0

S0

S0 S0 S0

S0

E

S0S0

S0

S0

S0

E S0

E

E S0

E E

S0

S0

S0

40% classified as ellipticals in RC340% classified as ellipticals in RC3

Galaxies without black holesGalaxies without black holes

M33 and NGC 205M33 and NGC 205– Central star clusterCentral star cluster– No AGNNo AGN– Strong upper limit on Strong upper limit on

black hole massblack hole mass

If they have a BH, If they have a BH, then its mass is well then its mass is well below the (Mbelow the (MBHBH,,σσ) )

relationrelation

Black Hole DemographicsBlack Hole Demographics EllipticalsEllipticals

– Be careful with masses Be careful with masses from gas kinematicsfrom gas kinematics

– Need stellar kinematics Need stellar kinematics for core galaxies (8m) for core galaxies (8m)

SpiralsSpirals– Not many masses, Not many masses,

especially especially < < 4x104x1077 M M

– Late type disks: no BH? Late type disks: no BH?

ScatterScatter– Observational errorsObservational errors– Systematics (triaxiality, asymmetries)Systematics (triaxiality, asymmetries)– Related to merger history?Related to merger history?

NGC 821 continuedNGC 821 continued ModificationsModifications

– Nukers corrected STIS/PSF Nukers corrected STIS/PSF convolution in code, reran convolution in code, reran models with own long-slit models with own long-slit kinematicskinematics

– SAURON maps finalized SAURON maps finalized (Emsellem et al. 2004)(Emsellem et al. 2004)

Agreement remains good Agreement remains good – MBH’s agree within 1MBH’s agree within 1– Addition of SAURON data Addition of SAURON data

improves accuracyimproves accuracy– Data is published, so Data is published, so

anyone can test their code anyone can test their code

Importance of 2D KinematicsImportance of 2D Kinematics

Four slits + STISFour slits + STIS SAURON + STISSAURON + STIS

3 level

Nuclear Stellar CuspsNuclear Stellar Cusps Classical bulgesClassical bulges

– Massive, RMassive, R1/41/4

– Cusp slopes like Cusp slopes like E/S0 galaxiesE/S0 galaxies

Sb/Sc bulgesSb/Sc bulges– Shallower Shallower

nuclear cusps nuclear cusps – Follow their own Follow their own

global/nuclear global/nuclear relationrelation

– Different Different structures on structures on 10pc scales10pc scales

RR1/41/4 bulges bulges Sb/Sc bulgesSb/Sc bulges

Nearby Radio GalaxiesNearby Radio Galaxies All have emission-line gas; many dust disks/lanesAll have emission-line gas; many dust disks/lanes Trigger of activity: seems related to gas/stellar Trigger of activity: seems related to gas/stellar

kinematics on small scales kinematics on small scales

Verdoes Kleijn et al., 1999, AJ, 118, 2592Verdoes Kleijn et al., 1999, AJ, 118, 2592WFPC2 V-band; 5''x 5'' framesWFPC2 V-band; 5''x 5'' frames

The E5 galaxy NGC 3377The E5 galaxy NGC 3377

SAURON: low spatial resolution: upper limit on MSAURON: low spatial resolution: upper limit on MBHBH

OASIS: lower limit on MOASIS: lower limit on MBHBH, insufficient field of view, insufficient field of view Combination: FOV and resolution: good MCombination: FOV and resolution: good MBH BH

Accuracy can be improved further with STIS dataAccuracy can be improved further with STIS data

SAURONSAURON OASISOASIS CombinationCombination

Copin, Cretton, Emsellem, 2004, AACopin, Cretton, Emsellem, 2004, AA