Modeling abundances! in star forming galaxies!
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1 Modeling abundances! in star forming galaxies!
2 Chemical Enrichment Q [Fe/H] and [X/Fe] evolve in a galaxy: fossils that retain the evolution history of the galaxy Galactic Archaeology!
3 3 types of galaxy models One-zone Semi-analytic! Chemo-dynamical simulations (monolithic) models (hierarchical) (Burkert Inhomogeneous & Hensler 87, chemical Katz 92, (Tinsley Instantaneous 80, Timmes+ mixing models Navarro enrichment & White 93, Steinmetz & 95, approximation! Pagel 97, (Kauffmann, Mass assembly Müller Internal 94, structures Mihos & Hernquist - 94, Matteucci SFR/inflow/outflow 01, Prantzos White+ history based 93, Cole+ on kinematics Kawata & of Gibson stars/gas, 03, CK 04, + with 93, analytic Chiappini+ formula! 97, 94, λcdm De scenario! Lucia+ 04,! spatial CK & distribution Nakasato 11, of CK+ Average 00 )! evolution of a Nagashima+ Global properties 05, Scannapieco+ elements 11, GASOLINE, galaxy (or a shell of Shankar+10 ) of galaxies in a RAMSES, AREPO )! galaxy)! large scale other types of models! Stochastic models (Argast et al 02; Ishimaru & Prantzos; Cescutti+)! Chemodynamical models without hydro (e.g., Minchev & Chiappini)!
4 Supernova Explosions 8.8 M 8 Few parameters. Central parts?! 12-25M 8 Kitaura, Janka,! Hillebrandt 06! Marek & Janka 09! Bruenn, Mezzacappa+ 09,13!
5 Stellar Yields Nomoto, Kobayashi, Tominaga 2013, ARAA (1D, no rotation) AGB core-collapse SN super AGB Also, Woosley & Heger; Limongi & Chieffi
6 Stellar Yields Nomoto, Kobayashi, Tominaga 2013, ARAA (1D, no rotation) PISN BH? core-collapse SN Also, Woosley & Heger
![01 for Z>Z 8, >20M 8 SN1998bw Kinetic energy [10 51 erg] 100 10 1 93J 94I 02ap 06aj 87A 08D](/docs-images/88/114886791/images/7-3.jpg "03bg 05bf 99br 03dh 97D 98bw 97ef 03lw R(SNIbc)>R(HN)>R(GRB)! rotation? binary?! 0.1 10 15 20 25 30 35 40 45 50 Main-sequence mass [M ] Nomoto et al.")
7 Hypernovae (>20M 8,>1foe) GRB SN light curves & spectra fitting M, E kin, M(Fe)! f HN (Z)=0.5 for Z<0.004, 0.01 for Z>Z 8, >20M 8 SN1998bw Kinetic energy [10 51 erg] J 94I 02ap 06aj 87A 08D 03bg 05bf 99br 03dh 97D 98bw 97ef 03lw R(SNIbc)>R(HN)>R(GRB)! rotation? binary?! Main-sequence mass [M ] Nomoto et al. 2002, 2013!
8 Type Ia Supernova Explosions Nucleosynthesis with tracer particles! Yields are similar to 1D model W7! Violent Merger,! Pakmor+ 12, Gadget! Röpke 04! GCD, Jordan+ 08, FLASH!
9 Our SNIa progenitor model Hachisu, Kato, Nomoto s! binary calculation WD+RG WD+MS DTD t -1 CK et al. 98;! CK & Nomoto 09! MS, ~3M 8! 0.1-1Gyr! in spirals or high-z! RG, ~1M 8! 1-20Gyr! in ellipticals
10 Milky Way-type galaxy Initial Condition: λcdm fluctuated sphere with λ~0.1, r~3mpc,! M tot ~10 12 M 8, N tot ~ , M gas ~10 6 M 8, M DM ~10 7 M 8 (CK & Nakasato 2011, ApJ, 729, 16)! Face on! Edge on! Movie:
11 [X/Fe]-[Fe/H] relations (CK & Nakasato 2011) Solar neighborhood
![[X/Fe]-[Fe/H]](/docs-images/88/114886791/images/12-0.jpg "relations (CK &")
12 [X/Fe]-[Fe/H] relations (CK & Nakasato 2011)
13 Carbon-Enhanced Metal Poor (CEMP) Stars Lee+13! CEMP-s: binary mass transfer; s-process enhancement! CEMP-no: not binaries (Starkenburg+14; Hansen); enriched by faint SNe (Ishigaki+14); also seen in DLAs (Cooke+10; CK+11)! No evidence of PISN enrichment (Aoki+15)! Placco+14! C-rich DLA [Fe/H]= -3.04, z=2.34! C-rich DLA [Fe/H]= -2.84, z=3.07! Peculiar DLA! 170M 8!
14 Subclasses of SNIa in dsphs? normal SNIa! CK, Nomoto, Hachisu 2015, ApJL, 804, 24! sub-ch SNIa! ~1M 8 RG or ~1-2M 8 MS H He CO SN Iax! ~1M 8 RG or ~2-6M 8 MS ONe CO In deflagrations, Mn is mostly synthesized in NSE, while in sub-ch SNeIa, mostly in incomplete-si burning, which depends on Z.! A mix of sub-ch SNIa & SNIax can reproduce [Mn/Fe]~ -0.5.!
15 Cosmological Simulation Movie: Stellar Luminosity Gas Metallicity 10Mpc; N~ ; m gas ~10 7 M 8 ; H 0 =70, Ω m =0.3, Ω λ =0.7, Ω b =0.04, n=1, σ 8 =0.9
16 Baryon Physics UV background radiation! (Haardt & Madau 1996)! BH,NS,WD! E Fe O Fe E O SNIa! SD(CK+98,09)! E Cooling(Z)! O(Sutherland & Dopita 93)! Fe O Fe E O Fe E SNII/HN (CK+06)! O Fe E E Star Formation! v<0, t cool <t dyn, t dyn <t sound! t sf =t dyn /c, c=0.1, Kroupa IMF! E Stellar Wind! E Feedback! 100% thermal! to N FB ~400! E BH Formation! Z=0, ρ>ρ crit,1000m 8! E BH Growth! accretion Bondi-Hoyle! merger! BH BH M acc! E
17 Constraining parameters from cosmic SFRs, Magorrian relation, and galaxy size-mass relation α =1, ε f =0.25, ρ=0.1, M seed =1000M 8! cosmic SFR! Blackhole Mass! redshift! ~ Galaxy Mass Taylor & CK 2014, MNRAS, 442, 2751!
18 Cosmological Simulations with AGN Feedback M BH seed ~ M 8! Taylor & CK 2014, MNRAS, 442, 2751! Cosmic SFR! Magorrian relation! 10,25/hMpc 3 run! obs: Bouwens+11, Karim+11, Cucciati+12, Oesch +12, Burgarella+13, Gunawardhana+13, Sobral+13 obs: Kormendy & Ho 2013
19 Other Big Simulations EAGLE w Gadget-3 (100Mpc)! Cosmic SFR?! Illustris w AREPO (106.5Mpc)! Size-Mass relation?! obs: Omand et al. 2014! Schaye et al. 14! Snyder et al. 15!
20 25Mpc box! εg~1kpc! Mg~107M8 21! Colour: Temperature; Taylor & CK !
21 AGN-driven outflows Taylor & CK 2015b, MNRAS, Letter, in press! AGN winds! AGN-driven winds remove the remaining gas (3% of baryon) and ~2% of total produced metals.!
22 Down-sizing Stellar Mass Function! Taylor & CK 2015, MNRAS, 448, 1835! α-enhancement of ellipticals! ~ Mass of galaxies!
23 Mass Metallicity Relations (MZR) Taylor & CK 2015, MNRAS, 448, 1835! Gas-phase Oxygen Abundance,! SFR weighted! Stellar Metallicity, luminosity weighted!
24 Environmental dependence Kacprzak et al. 2015, ApJL, 802, 26! ZFIRE survey with MOSFIRE/Keck: No discernible difference between the MZR of field and cluster galaxies to within 0.02dex at z~2.!
25 Time evolution Taylor & CK 2015c, in prep.! Mass-Metallicity Relation! BH Mass-σ Relation! Steeper slop at higher-z! No evolution!
26 Metallicity Gradients vs Mass Steep Kobayashi & Arimoto 1999! Spolaor, CK et al. 2010! GMOS-slit observations! GRAPE SPH simulations (CK 2004) Flat Kobayashi & Arimoto (1999) SAURON (Kuntschner et al. 2010)! Hopkins et al. 09
27 Metallicity Gradients vs Mass ATLAS 3D, CALIFA, SAMI, MaNGA! Taylor & CK 2015d, in prep.! Flat Spolaor (2010) s transition MW Steep Measured in MAX(2re,10kpc), V-luminosity/SFR weighted!
28 Cosmic SN rates in cosmological simulation with AGN feedback (P. Taylor 15),! assuming massive (>40M 8 ) & metal-poor ([Fe/H]<-1) HNe as GRBs.!
29 Summary Nucleosynthesis yields & SN progenitors are tested with! Z>0: Elemental Abundance Ratios in the solar neighborhood! Z=0: Abundance patterns of EMP stars not PISN but faint SN! SF & FB (from SNe and AGN) parameters are determined from! ü Cosmic SFR! ü M BH -σ Relation! ü Size-Mass Relation BH seeds are stellar origin, M 8! Simulation outputs are tested for! ü Luminosity/Mass Number Function! Color-Magnitude Diagram / Specific SFRs! ü Mass-Metallicity Relation insensitive to AGN! α-enhancement of Es! Predictions that will be tested with future observations! Metallicity Radial Gradients depend on the merging history! SN rates, host galaxies, galactocentric distance (talks at FM10)!
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