IInntteerrnnaall DDyynnaammiiccss ooff GGaallaaxxiieess aanndd GGrroouuppss AAaarroonn JJ.. RRoommaannoowwsskkyy UUnniivveerrssiiddaadd ddee CCoonncceeppcciióónn CCoollllaabboorraattoorrss:: NN.. DDoouuggllaass,, LL.. CCooccccaattoo,, ((KKaapptteeyynn)),, KK.. KKuuiijjkkeenn ((LLeeiiddeenn)),, M. Merrifield (Nottingham), M. Arnaboldi (Torino), M. Merrifield (Nottingham), M. Arnaboldi (Torino), PPNNee OO.. GGeerrhhaarrdd ((MMPPEE)),, KK.. FFrreeeemmaann ((RRSSAAAA)) NN.. NNaappoolliittaannoo,, MM.. CCaappaacccciioollii ((CCaappooddiimmoonnttee)) EE.. OO’’SSuulllliivvaann ((CCffAA)),, DD.. FFoorrbbeess ((SSwwiinnbbuurrnnee)) TT.. PPoonnmmaann,, SS.. RRaayycchhaauuddhhuurryy ((BBiirrmmiinngghhaamm)) XX--rraayy TT.. RRiicchhttlleerr,, DD.. GGeeiisslleerr,, MM.. GGóómmeezz ((CCoonncceeppcciióónn)) SS.. ZZeeppff ((MMiicchhiiggaann SStt)),, GG.. BBeerrggoonndd ((IIAAAA)),, RR.. SShhaarrpplleess ((DDuurrhhaamm)),, YY.. SScchhuubbeerrtthh ((BBoonnnn)),, GGCCss LL.. BBaassssiinnoo,, FF.. FFaaiiffeerr,, JJ.. FFoorrttee ((LLaa PPllaattaa)),, LL.. IInnffaannttee ((PPUUCC)),, KK.. RRhhooddee ((WWeesslleeyyaann)),, PP.. SSáánncchheezz--BBlláázzqquueezz ((EEPPFFLL)) EElllliippttiiccaall ggaallaaxxyy eennvviirroonnmmeennttaall ddiiffffeerreenncceess Central properties of ellipticals show only minor dependence on environment NGC 821: (e.g. Reda et al. 2005) isolated

NGC 4697: group

Tidal fields in higher
env : Ω truncated DM halos? Ω truncated GC systems? NGC 4473: VViirrggoo cclluusstteerr:: MM8877,, MM8866,, MM8844 cluster Ω less radia((MMl iaihhnoossiseeott aatrll..o 22p000y055?)) GGCCSS ssuurrffaaccee ddeennssiittyy pprrooffiilleess Extended GCSs in BCGs (McLaughlin 1999)

NGC 4636: BGG in Virgo infalling group? (Dirsch et al. 2005)

N ∝ R -1.5 -5 N ∝ R Stripped halos?: GCs as proxy for DM (e.g. Bekki et al. 2005) GGaallaaxxyy//ggrroouupp MM//LL rreessuullttss//pprreeddiiccttiioonnss

Manenbaum plot, vdB plot, Tully plot

(Parker et al. 2005) CCoommbbiinneedd hhaalloo pprroobbeess • Planetary Nebulae, Globular Clusters, X-rays Ω Cross-checks for reliability Ω Much stronger combined constraints,

e.g., use MX(r) and find orbit anisotropy from kinematical data Ω Cross-correlate stellar+GC pops kinematics • Long-term PN.Spectrograph program on WHT (Douglas et al.) • Various GCs projects (VLT, Magellan, Gemini) • Chandra archive grant, new XMM-Newton data (O‘Sullivan et al.) PPrroobbiinngg EE hhaallooss wwiitthh XX--rraayy eemmiissssiioonn Chandra, XMM-Newton: large area, high angular resol´n Ω determine T(r), subtract pt. sources, check equilibrium Ω important to not select on LX (biased mass result!)

NGC 4365 NGC 4382

Chandra ACIS-S (Sivakoff, Sarazin & Irwin 2003) Globular Clusters in NGC 1399

D=19 Mpc, MB=-21.1 Fornax central E1 VLT+FORS2/MXU, Gemini-S+GMOS: Nov/Dec 2000, Nov/Dec 2002, Nov/Dec 2004 (Richtler et al.)

>700 velocities to 90 kpc, ∆v = 20-100 km/s NNGGCC 11339999:: GGCC ddiissppeerrssiioonn pprrooffiillee M87: Dispersion profiles PNe consistent with long-slit data

PN σp(R) constant or rising with R dark halo indicated

PNe have lower

σp(R) than GCs (Hanes et al. 2001)

PN, GC orbits differ M87: Modeled circular velocity profile

Stars + 234 GCs (Romanowsky & Kochanek 2001) XMM-Newton (Matsushita et al. 2002) Ω good agreement

Stars + 200 PNs (Douglas et al.) Ω strong stellar anisotropy NGC 4472: Dispersion profiles PNe consistent with long-slit data

PN σp(R) constant or rising with R dark halo indicated

PNe have similar

σp(R) to GCs (Zepf et al. 2000) NNGGCC 44663366:: GGCC ddiissppeerrssiioonn pprrooffiillee

174 GC velocities w/VLT+FORS2/MXU:

roughly constant velocity dispersion

lower halo mass than Chandra results (Schuberth et al.)

(Jones et al. 2002) GCs in NGC 1407 (Eri A group)

E1 , MB = -21.6 D = 27 Mpc

VLT+FLAMES/ GIRAFFE, Keck+LRIS: Nov 2004

35 GC velocities ∆v = 15-30 km/s NNGGCC 11440077:: GGCC ddiissppeerrssiioonn pprrooffiillee

stars PNe in NGC 3379

E1 , MB = -20.0 D = 11 Mpc. Leo I central

WHT+PN.S: March 2002 3 hrs : 197 PN velocities to 7 Reff , ∆v = 20 km/s NNGGCC 33337799:: sstteellllaarr//PPNN ddiissppeerrssiioonn pprrooffiillee

stars

=0 NFW halo MOND
γ p(R) ∝ R , γ = -0.36 ± 0.07 PNs no DM NGC 3379 : circular velocity profile Orbit models include variable anisotropy! (find
~ -0.3  +0.5)

• cumulative M/L
CDM+AC

at 5 Reff : = 7.1 ± 0.6 PN.S • DM fraction const M/L

inside Reff ~ 3% best-fit halo GCs in NGC 3379

E1 , MB = -19.9 D = 10 Mpc

UT2+FLAMES/ GIRAFFE: May-Jul 2003 5 hours :

34 GC velocities ∆v = 5-15 km/s NGC 3379 : GCS dispersion profile

Weakly declining dispersion: γ p(R) ∝ R , γ = -0.13 ± 0.12

cf. PNs Due largely to different N(R) ,
(r) NGC 3379 : GCS dynamics Model predictions vs. data (isotropy)

GCs data CDM Best PNs + CDM Best HI ring + CDM MOND const M/L NGC 3379: HI gas ring Mass measurement N3379 + N3384: M/LB (100 kpc) = 27 ± 5 (Schneider 1985)

Not consistent with group-mass halo NGC 3379 : Constraints on halo

Problem for consensus solution: HI and GCs not consistent “Ordinary” (~L*) elliptical galaxy sample Family 1 (disky/faint) Family 2 (boxy/bright) N4564 N4339 N4473 N4552 N4374 N4365 PNe PNe (PNe) PNe PNe (PNe) Cluster (GCs) (GCs) Xray Xray Xray Xray

N4494 N3377 N4742 N3379 N5846 N3608 PNe PNe (PNe) PNe PNe PNe Group (GCs) GCs Xray Xray Xray Xray

N821 N5582 N6673 N2663 N7196 N7507 PNe Field (GCs) Xray (GCs) Xray (GCs) Extended stellar/PN dispersion profiles 5 “normal” (L*) ellipticals:

σp(R) declining with R (Ciardullo et al. 1993; Méndez et al. 2001; Romanowsky et al. 2003; Teodorescu et al. 2005) Population of ordinary ellipticals with low DM content? MM//LL ggrraaddiieenntt ppaarraammeetteerr

∇
l : logarithmic radial gradient of M/L R »≈ M ’ ≈ M ’ ÿ R ∆ ∇ ≡ e …∆ d ÷ − ∆ d ÷ Ÿ = e l ∆ ÷ ∆ ÷  ∆r …« M * ◊out « M * ◊in ⁄Ÿ in∆r

theoretical quantity empirical quantity

∇
l : independent of bandpass, distance;

insensitive to measurement radii (rin , rout)  (f =0.17,

=0.9) SF CCDDMM pprreeddiiccttiioonnss (fbb=0.17, 88=0.9)

∇
l : increases with M*, decreases with SF

Sensitive to

M*-Re relation Valid statistically, not individually EEmmppiirriiccaall ggrraaddiieennttss Sample of 21 Es, S0s M/L from stars, PNe, GCs

Significant correlations between ∇
l

& MB ,M* , a4 , γ

Not with env Low concentration halos? (after Napolitano et al. 2005) Fits to ∇
data assuming CDM HOD (van den Bosch et al. 2003)

ΛCDM (Bullock et al. 2001)

0.5 cvir (e.g.
WDM) Low concentration halos?

Chandra/XMM galaxy sample: c ~ 2-4 (~ cluster concentrations) (Fukazawa et al. 2006) RReessuullttss ffoorr ssttaarr ffoorrmmaattiioonn eeffffiicciieennccyy Assuming LCDM concentrations:

Brighter galaxies: reasonable SF

Fainter galaxies: weak lensing some SF > 1

(fb > 0.17) Next conference: ‚GROUPS OF GUANACOS IN THE NEARBY UNIVERSE„ ?!

Natural outcome of merger?

Dekel et al. (2005) Natural outcome of merger? Radial anisotropy, triaxiality can naturally lower projected dispersions

Data may be reproduced if:

Sbc-Sbc 1:1 merger or recent starburst contaminating PNe Simulations realistic? Blue bump from excess baryon cooling : extra concentration of stars, DM steepens dispersion

~30% central DM fraction contradicts best observational estimate (~10% fast rotators) Radial anisotropy? Dekel et al. (2005) radial

isotropic

tangential N3379 orbit model

N821,N3379,N4494 PNe

Athanassoula (2005)