Myung Gyoon Lee - cfht.hawaii.edu€¦ · Overview of current issues and limits of spectroscopic...
Transcript of Myung Gyoon Lee - cfht.hawaii.edu€¦ · Overview of current issues and limits of spectroscopic...
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Myung Gyoon Lee Department of Physics & Astronomy
Seoul National University, Korea
Next Generation CFHT workshop, Mar27-29, 2013, Hilo, Hawaii
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FOREVER ( FORmation & EVolution of clustERs
(of stars and galaxies) )!
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Overview of current issues and limits of spectroscopic studies of extragalactic star clusters ◦ In Early Type Galaxies (ETGs)
◦ For Age, Metallicity, and Kinematics
What to do with ngCFHT
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One of the most shocking and intriguing findings: Color distribution of globular clusters in ETGs: Bimodal! (numerous references in Brodie & Strader 2006 ARAA)
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Globular Clusters in M49 (Geisler, Lee, & Kim 1996, AJ, Lee, Kim & Geisler 1998, AJ)
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100 ETGs in Virgo (Cote+2004, Peng+2006,Jordan+2009)
Color distribution of globular clusters in bright ETGs: Bimodal!
5 Peng+2006 ACSVCS (Cote et al 2004)
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What does color bimodality tell or what can we tell with it?
Two aspects for today 1) Halo Structure of ETGs & Dark Matter
2) How ETGs & GCs formed
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Massive ETGs have dual halos! A blue halo and a red halo.
Yin & Yang model?
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Lee+ (2012)
The blue halo (Metal-poor) ◦ Blue pops (GCs and faint stars)
◦ Metal-poor
◦ Rounder, Extended
◦ Non-rotating?
The red halo (Metal-rich) ◦ Red pops (GCs and bright stars)
◦ Main body of ETGs
◦ Metal-rich
◦ Flatter, Centrally concentrated
◦ Rotating?
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Globular Clusters in M49
(Lee, Kim & Geisler 1998 AJ)
Blue halo : Red halo
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Metallicity and Age!
Kinematics!
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Last two decades: ◦ 4-10m telescopes with various spectrographs
◦ a history of agony and tantalizing clues!
Current status: ◦ Still difficult and challenging task for EGCs today
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Park, Lee, Arimoto et al. (2012, ApJ)
Re-analyzed line index data for GCs in 7 gEs in the literature ◦ M87, M49, M60, NGC 4636, NGC 5128, NC 1399, and NGC 1407
Derived [Fe/H] and age from a comparison of line indices with SSP model (Thomas+ 2003) for a combined sample of GCs in gEs (167 blue and 148 red GCs).
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(M87, M49:Cohen et al 1998, 2003, M60:Pierce 2006, NGC 4636: Park et al 2012,
NGC 5128: Woodley et al 2010, NGC 1399: Forbes et al 2001,
NGC 1407: Cenarro et al 2007, MW: Harris 2010)
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Globular Clusters in
MWG (Puzia et al2002 )
NGC 5128 (Woodley et al 2010)
NGC 4636 (Park et al 2012 ),
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Metallicity distribution is bimodal: ◦ Peaks at [Fe/H]=-1.25 and -0.42 : the MP halo & the MR halo
◦ (MW: [Fe/H] -1.52 and -0.52)
A larger fraction of high [Fe/H] than MW GCs
13 (Park, Lee et al. 2012, ApJ)
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Young GCs:
◦ A broad range
◦ A larger fraction of high [Fe/H]
Old GCs:
◦ Both metal-poor & metal-rich!
◦ Low [Fe/H] GCs are major.
14 (Park, Lee et al. 2012, ApJ)
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A broad distribution: 1-15 Gyrs
Old GCs formed mostly early (>10 Gyr ago) !
Existence of young GCs with 1-10 Gyrs!!!
15 (Park, Lee et al. 2012, ApJ)
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Metal-poor GCs: The bulk formed at >10 Gyr ago.
◦ Some GCs with intermediate-age
Metal-rich GCs: ◦ Old GCs and young GCs
◦ A larger fraction of younger GCs.
Cosmic star formation history
(10 Gyr=z~2)
16 (Park, Lee et al. 2012, ApJ)
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(current) A small N in a small region in a galaxy.
With ngCFHT, we can cover the entire GCS in each galaxy!
To study cluster formation history in a galaxy.
17 (Park, Lee et al. 2012, ApJ)
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Lee et al (2010) Park et al (2012): Subaru + literature
Analysis of all velocity data in 7 gEs
Srader et al (2011): M87 MMT/Hectospec: 2hour(g<22, 1field), R=~5A (3700-9100A)
KEC/LRIS : 3hour(<g>=22.5, 4 mask), R=~4.0A (3300-5600A)
KEC/DEIMOS :3hour(I<23, 4mask)+0.6h(1mask), R=~1.5A (6500-8700A)
Pota et al (2013): (SLUGGS, 12 ETGs) KEC/DEIMOS: 1(M87)~2(N1407)hour : err(vel)~15km/s,
R=~1.5A
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Park et al (2012, ApJ)
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Obs(Park et al (2012) <-> Model(Bekki et al 2008)
Rotation/Velocity dispersion
Model(Bekki et al 2008)
Model(Bekki et al 2008)
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Obs(Park et al (2012) <-> Model(Bekki et al 2005)
Rotation/velocity dispersion: Diversity!
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A mixture (bibimbap) scenario for ETGs
(updated from Lee et al 2010b, ApJ).
** Every galaxy has a different formation history,
but massive galaxies have dual halos.
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Large aperture -> V<~23
Wide field of view: 1.6 square deg
R = 2000-6000, err(v)<~10
Kinematics, age, metallicity of star clusters
Targets: Virgo and (M31+M33, M81 Group, M106 Group, Leo I Group)
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Strader+(2011)
”M87 is not dynamically coupled to the Virgo cluster”
“W find no strong signatures of rotation, which was seen in the outer region previously (expected for a major merger).”
Why different from old results?
Strader et al (2011)
Cote et al (2001)
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The most extensive case: M87 (Strader et al 2011)
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What can ngCFHT do?
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Substructures around massive galaxies
Connecting structures
Diffuse large scale structure-IGCs (wandering GCs) !!!
Tips of icebergs!
See NGVS.
ngCFHT is an ideal tool for this!
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The blue halos are much larger than the red halos!
IGCs are mostly blue GCs! (old & metal-poor?)
28 Lee, Park & Hwang (2010, Science): SDSS
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FOREVER ( FORmation & EVolution of clustERs
(of stars and galaxies) )!
With the power of ngCFHT,
a new era for extragalactic star clusters will be open.