star formation in galaxies yuexing li (columbia univ. /amnh) mordecai mac low (amnh/columbia) ralf...
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Star Formation in GalaxiesStar Formation in Galaxies
Yuexing Li (Columbia Univ. /AMNH)
Mordecai Mac low (AMNH/Columbia)
Ralf Klessen (AIP, Germany)John Dubinski (CITA)
Zoltan Haiman (Columbia)
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NASA, Hubble Heritage Team, Nick Scoville and T. Rector
Star Forming GalaxiesStar Forming Galaxies
NASA/STScI/B.Whitmore
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1. Global Schmidt Law1. Global Schmidt Law
Kennicutt1998 Gao & Solomon 2004
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2. Star Formation Thresholds2. Star Formation Thresholds
Martin & Kennicutt (2001)
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Models of the SF lawsModels of the SF laws
Gravitational instability (Kennicutt89, Friedli et al. 94, Kennicutt98, Martin & Kennicutt 01)
Kinematical law (Wyse 86, Silk 87, Hunter, Elmegreen & Baker 98)
Density PDF from turbulence (Elmegreen 02, Kravtsov03, Krumholtz & McKee 05)
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P1: SF in Isolated Disks P1: SF in Isolated Disks
Code: GADGET v1.1 (Springel, Yoshida & White 01)
+ sink particles (gravitationally bound, convergent flow, n >103 cm-3, represent star clusters)
Galaxy model: DM halo + disk (stars & isothermal gas)
(Mo, Mao, White 98, Springel & White 99, Springel 00) Initial conditions:
– rotational vel.: 50 ≤ Vrot ≤ 220 km s-1
– gas fractions: 20 ≤ fg ≤ 90% of Md– effective sound speed cg = 6, 15 km s -1
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Numerical CriteriaNumerical Criteria
Jeans criterion for mass resolution (Bate & Burkert 97, Truelove et al. 97)
Gravity-hydro balance criterion for gravitational softening length (Bate & Burkert 97)
Equipartition criterion between gas, collisionless particle masses (Steinmetz & White 97)
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Resolution StudyResolution Study
105
6.4 x 106106
8 x105
Li, Mac Low & Klessen 2005a
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How Do Stars Form?How Do Stars Form?
LMK 2005b
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Star Formation MorphologyStar Formation Morphology
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Global Schmidt LawGlobal Schmidt Law
Kennicutt 1998
LMK 2005c
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Local Schmidt LawsLocal Schmidt Laws
LMK 2005c
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What Controls SF?What Controls SF?S
tar
form
atio
n ti
mes
cale
Gravitational instabilityLMK 2005d
Sta
r F
orm
atio
n E
ffic
ienc
y
Galaxy Model
LMK 2005c
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P2: SF in Interacting GalaxyP2: SF in Interacting Galaxy
Li, Mac Low & Dubinski, in prep
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Merger vs. SingleMerger vs. Single
LMK 2004
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Merger RemnantMerger Remnant
Mass distributionAge distribution
LMK 2004
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Connection btw SF and BH GrowthConnection btw SF and BH Growth Similarity btw cosmic SFH and quasar evolution
(Madau et al. 96, Shaver et al 96) Starburst – AGN connection (Norman & Scoville 88,
Smith, Lonsdale & Lonsdale 98) MBH – correlation (Magorrian et al. 98, Ferrarese &
Merritt 00, Tremaine et al. 02) Most starburst gals are mergers (Sanders & Mirable
96, Alexanders et al 2004) Larger amount of CO in nearby merging galaxies
(Scoville 2000) and high-z QSOs (Walter 2002) QSO lifetimes 106 – 108 yrs (Martini 2004) Recent simulations (De Mateo, Springel & Hernquist
05, Kazantzidis et al. 05)
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Simulated MSimulated MBHBH - - Relation Relation
Li, Haiman & Mac Low, in prep
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Quasar LifetimesQuasar Lifetimes
Li, Haiman & Mac Low, in prep
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SummarySummary Our simulations reproduce many obs. of SF in
gals -- the Schmidt Laws, SF thresholds… tot gravitational instability, CO SFE
Galaxy interaction trigger starburst. Higher SN of GCs, and bimodal metallicity dist. are natural products of gas-rich major mergers.
Merger also increase BH accretion, and the MBH – correlation is the fine-tuning of gas removal, in our case regulated by SF.
Quasar lifetime ranges 106 – 108 yrs, depending on the luminosity threshold