constraints on secular evolution from star clusters in spirals and lenticulars jean p. brodie...
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Constraints on Secular Evolution from Star
Clusters in Spirals and Lenticulars
Jean P. BrodieUCO/Lick ObservatoryUniversity of California
Santa Cruz
Study of Astrophysics
of Globular clusters
in Extragalactic
SystemsP. Barmby (CfA), M. Beasley (UCSC), K. Bekki (UNSW), J. Cenarro (UCSC/U Madrid), L. Chomiuk (UCSC), D. Forbes (Swinburne), J. Huchra (CfA), S. Larsen (ESO), M. Pierce (Swinburne), R. Peterson (UCSC), R. Proctor (Swinburne), J. Howell (UCSC), L. Spitler (UCSC), J. Strader (UCSC)
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OverviewGalaxy Formation
Background: Globular clusters and their relevance to galaxy formation
Global properties of GC systems in early and late-type galaxies
Bimodal color distributions and implications for GC/galaxy formation
Constraints on secular evolution from GC ages, metallicities, specific frequencies and correlations with host galaxy properties
Lenticular Galaxies Faint Fuzzies: discovery and characteristics Ideas on formation Signposts for secular evolution?
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What are Globular Clusters?
SSPs – single ageand metallicity
105 – 106 Msun
All galaxies MV <–15 have at least one GC
~150 in MW~400 in M31> 10,000 in some ellipticals
SNNGC 100.4(Mv+15), 2 – 3 greater in E’s
M 13
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• Associated with galaxies of all morphological types • Constrain theories of galaxy formation and evolution When and how? Differences
Constraining galaxy
formation
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Good tracers of star formation histories of
galaxies
Massive star clusters form during all major star formation events (Schweizer 2001)
#of young clusters scales with amount of gas involved in interaction (Kissler-Patig et al 1998)
Cluster formation efficiency depends on SFR in spirals (Larsen & Richtler 2000)
NGC 6946 Larsen et al 2001
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Bimodal Color Distributions
V-I = 0.95 1.15 [Fe/H] = -1.5 -0.5
Bimodal color distributions globular cluster sub-populations
Color differences are due to age differences and /ormetallicity differences
Multiple epochs and/or mechanismsof formation
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GC/Galaxy Formation Models
1. Formation of ellipticals/GCs in mergers (Schweizer 1987, Ashman & Zepf 1992)
2. In situ/multi-phase collapse (Forbes, Brodie & Grillmair 1997)
3. Accretion/stripping (Cote’ et al. 1998)
4. Hierarchical merging (Beasley et al. 2002)
2 & 4 require (temporary) truncation of GC formation at high redshift
z
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GC Ages Increasing evidence that both red and blue globular clusters are
very old (>10 Gyr) Small percentage of red globular clusters may be young Ellipticals/Lenticulars:
NGC 1399 (Kissler-Patig, Brodie, Schroder et al. 1998; Forbes et al 2001) M87 (Cohen, Blakeslee & Ryzhov 1998) NGC 4472 (Puzia et al 1998; Beasley et al. 2000) NGC 1023 (Larsen & Brodie 2002) NGC 524 (Beasley et al 2003) NGC 3610 (Strader, Brodie et al 2003, 2004) NGC 4365 (Larsen, Brodie et al 2003) NGC 1052 (Pierce et al 2004) NGC 7457 (Chomiuk, Strader & Brodie 2004)
+ PhD theses of T. Puzia and M. Hempel Spirals: M 31 (Barmby et al. 2000; Beasley, Brodie et al 2004)
M 81 (Schroder, Brodie, Huchra et al. 2001) M 104 (Larsen, Brodie, Beasley et al 2002)
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Constraint # 1 Old ages of both sub-populations
Inconsistent with major merger picture
Relevance to Secular Evolution?
Read on!
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Color-Magnitude Diagrams
Average blue peak color (V–I)o=0.95 0.02
Average red peak color (V–I)o=1.18 0.04
[Fe/H]= – 1.4, –0.6 (Kissler-Patig, Brodie,
Schroder et al. 1998 AJ)
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Milky Way
Peaks at[Fe/H] ~ – 1.5 and – 0.6 (Zinn 1985)
MW GCs are all old
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Sombrero Peaks at (V–I)0=0.96 and 1.21
Larsen, Forbes & Brodie (MNRAS 2001)
Follow-up spectroscopy at Keck indicates vast majority
of GCs (both red and blue) are old (~13 Gyr) Larsen, Brodie, Forbes (2002)
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GCs and Galaxy Assembly Colors of both reds and
blues correlate with galaxy mass (MV and ) and color
Blue relation difficult to explain under accretion/major merger scenarios Constraints on Hierarchical Merging Paradigm from ages of GCs in dwarfs (~12 Gyr)
Brodie 2001; Larsen, Brodie et al 2001; Strader, Brodie & Forbes 2004
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.Metal-rich GCs in spirals and ellipticals have the same origin — they formed along with the bulge stars
Spirals fit the trend
Brodie & Huchra 1991; Forbes, Brodie & Grillmair 1997; Forbes, Larsen & Brodie 2001; Larsen, Brodie, Huchra et al 2001
Red GC relation has same slope as galaxy color relation Red GCs and galaxy stars formed in the same star formation event
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Constraints # 2 Similarities between peak colors
in spirals and ellipticals Hints at universal GC formation processes Slope of red GC color vs galaxy mass
relation is same as galaxy color vs galaxy mass relation (true for spirals and ellipticals)
Red GC formation is linked to formation of bulge
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Bulge GCs
Forbes, Brodie & Larsen ApJL Forbes, Brodie & Larsen ApJL (2001)(2001)
Number of metal-rich GCs scales with the bulge of metal-rich GCs scales with the bulge
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Numbers/Specific Frequency
The fraction of red GCs in ellipticals is about 0.5
The bulge SN for field ellipticals is ~1
Spirals and field ellipticals have a similar number of metal-rich GCs per unit (bulge) starlight
Metal-rich GCs in spirals are associated with bulge not disk # bulge (red/MR) GCs scales with bulge luminosity # red GCs/unit bulge light = bulge SN ~1 The total SN for field ellipticals is 13 (Harris 1991)
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Specific Frequency
SN
B/T
• ••
•
•
0.5
2.0
1.0
0.8 0.2
SN (total) constant at ~0.55 for spirals with B/T≤0.3 (Sb and later)
Constant number of GCs formed in late-type spirals
Universal old halo population
SN (total) ~ 2 for “field” Es
If higher SN for Es due to “extra” GCs formed with bulge, expect SN
to scale with B/T from ~0.55±0.25 at B/T=0 to ~1.9±0.5 at B/T=1
Goudfrooij et al 2003
Chandar et al 2004
3957
M51
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Exceptions Secular Evolution? NGC 3628: Interacting
HI tidal plume + bridge connection with NGC 3627 – extra GCs formed in interaction?
NGC 7814: Best evidence? Least luminous sample galaxy (5 x less than NGC 4594). Satellite-to-main galaxy mass ratios of 10% more common for low mass galaxies (Goudfrooij et al 2003)
M 51: Does it have a bulge?Interacting with NGC 5195Too few “bulge” (MR) GCs? (uncertain estimate)16 vs 98 (bulge/disk deconvolution) or 16 vs 45 ( – BH mass) (Chandar et al 2004)
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Constraints #3
Number of metal-rich GCs scales with the bulge luminosity
Specific frequency as function of B/T broadly consistent with universal halo (blue) GC population + “extra” (red) GC population formed with bulge
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Conclusions1) Number of metal-rich GCs scales with the
bulge luminosity2) Chemical evidence also suggests that
metal-rich GC formation closely linked to bulge formation
3) Metal-rich GCs are old
1),2) & 3) argue against secular evolutionHowever, exceptions allow for bulge build-
up by secular evolution Galaxies of similar morphological type can
have different formation histories
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Lenticular GalaxiesFaint Fuzzies Collaborators:Andi Burkert, Soeren Larsen
Brodie & Larsen 2002 Larsen & Brodie 2000
HST program to study GCs in NGC 1023 (MB= –20) Nearby (10 Mpc) S0 galaxy Faint endof GCLF
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NGC 1023 GCLF Faint wing of NGC
1023 GCLF deviates significantly from Milky Way GCLF
3rd population of clusters in addition to normal compact red and blue GC sub-populations
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GC Selection
Typical GC Reff =2–3 pc
29 objects in NGC 1023 with Reff>7 pc
Almost all are red
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Spatial Distribution
Background cluster of galaxies ruled out
Extended objects have annular distribution corresponding to galaxy isophotes
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Search for other Faint Fuzzies
FFs detectable in 4 galaxies (3S0s, 1E) in HST WFPC2 archive
Found in 2: N 1023, N 3384 (both SB0s in groups) Ruled out in 2: N 3115 (S01,
isolated), N 3379 (E)ACS data……
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Keck Spectroscopy
NGC 1023 “master”spectrum <[Fe/H]>FF1023=–0.58±0.24 represents 133 hours of 10-m telescope time NGC 3384 - 30 hours <[Fe/H]>FF3384=–0.64±0.34
Brodie & Larsen AJ 2002
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Velocities
NGC 1023 <VFF>=559±64 km/s
Vgal=601 km/s NGC 3384
<VFF>=768±79 km/s
Vgal=704 km/s FFs are ~2 bulge Reff
from center disk not bulge objects
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Ages
FFs are mostly likely ~ 13 Gyr old and not younger than ~ 7–8 Gyr
Stable against disruption
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New Kind of Cluster?
Milky WayNGC 1023Globular Clusters
Open clusters are smaller, younger and less massiveNo MW objects correspond in metallicity, luminosity and size
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Origins
FFs have no analogs in MW or elsewhere in LG
Found exclusively in lenticulars (so far)
Is the mechanism responsible for the formation of FFs linked to the mechanism for forming lenticulars?
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Distribution and Kinematics
Distribution of VFF not same as galaxy rotation curve
FFs located in a ring with radius ~1.5’ (4-5 kpc) and Vrot 200 km/s
Tidal radius 48 pcQuickTime™ and a
TIFF (LZW) decompressorare needed to see this picture.
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Extended Cluster Formation
2. Resonance rings and secular evolution
Simulations of Geyer & Burkert (2003, 2004) form bound clusters with sizes and masses of FFs in GMCs if star formation occurs with a density threshold
Under what circumstances do these special star-forming conditions occur?
1. Galaxy-galaxy interations? e.g. Cartwheel
11
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Faint Fuzzies Signposts for secular evolution?
NGC 1023 and NGC 3384 are barred NGC 3115 is not B ~3.5 kpc
in NGC 1023 (Debattista et al 2002)
Bulge is red (old, MR) Kinematically and
chemically decoupled nuclear disk (stars ~ 7 Gyr)
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NGC 3081
MB=20 early-type (S0/a, Sa)
barred spiral (bulgeless) Inner ring encircles bar
at ~5 kpc ~58 blue (young) clusters in
ring with MV <9 (V<23.6) Typical cluster effective radius ~11 pc !
Will these clusters survive? Is bar formation important in
forming lenticular galaxies?
Buta et al (2004)
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Implications
If FF formation is linked to bar formation in disk galaxies
Disks and bars were present in
galaxies at high redshift (z >2)