Distribution of Mass in the Milky Way Galaxy, Leiden, July Laura V. Sales. Kapteyn Astronomical Institute, Groningen, The Netherlands
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1 Distribution of Mass in the Milky Way Galaxy, Leiden, July 2009 Laura V. Sales Kapteyn Astronomical Institute, Groningen, The Netherlands
2 Outline - Brief review of thick disk formation scenarios: * Accretion * Heating * Radial Migration * Gas rich mergers - Description of the simulations - Orbital Eccentricities for each scenario: in-situ/ accreted populations - Application to the Milky Way
3 Models for thick disk formation: i)- Accretion Model Majority of stars in the thick disks are brought in by satellites that were disrupted by tidal interactions (Abadi et al. 2003a,b) Abadi et al Orbit circularity 40 kpc Old thick disk stars mostly of accreted origin In situ Fraction Age
4 Models for thick disk formation: ii)- Heating E Satellite delivers energy and momentum that increases the internal energy of the pre-existing thin disk z Satellite relatively massive Msat~ Mdisk Weak dependence on orbit inclination, 30 o- 60 O preferred Quinn & Goodman 1986; Toth & Ostriker 1992, Benson et al. 2004, Font et al. 2001, Kazantzidis et al. 2008, Villalobos & Helmi 2008 Kazantzidis et al. (2008)
5 Models for thick disk formation: iii)- Radial migration Stars in the thin disk may be trapped onto resonant corotation with transient spiral arms, and may migrate inwards and outwards along the spiral waves. (Sellwood & Binney 2002) Roskar et al. 2008a,b + surface brightness vertical velocity dispersion (Kregel et al. 2005) Formation of a Modest thick disk component
6 Models for thick disk formation: iv)- Gas rich mergers thick-disk stars are formed from gas that is accreted to the galaxy during a chaotic period of hierarchical clustering at high redshift. Brook et al. 2004,2005 Brook et al. 2005
7 Models for thick disk formation: iv)- Gas rich mergers thick-disk stars are formed from gas that is accreted to the galaxy during a chaotic period of hierarchical clustering at high redshift. Brook et al. 2004,2005 Brook et al SINS: Observations of H disks at z~2-3 Disks geometrically thick and highly turbulent ( /Vc ~ ) Forster-Schreiber 2006, 2009
8 Models Comparison i) Accretion (Abadi et al. 2003) ii) Heating (Villalobos & Helmi 2008) iii) Radial Migration (Roskar et al. 2008a,b) iv) Gas rich mergers (Governato et al. 2007) Kinematical properties of the thick disks: eccentricities
9 Vertical Mass Density Profiles (No thin disk) Each scenario able to produce a thick disk...
10 Modeling of the orbits Integration in fixed potential NFW halo x Hernquist bulge 2 Miyamoto-Nagai disks
11 Eccentricities as a function of z z eccentricity (accreted scenario)
12 Eccentricity distribution for each Thick Disk formation model
13 Eccentricity distribution for each Thick Disk formation model
14 Eccentricity distribution for each Thick Disk formation model Solar neighborhood cylinder (2<R/Rd<3) Distributions do differ In-situ low, < >~ Accreted high, < >~0.5
15 Conclusions
16 Conclusions We have compared the eccentricity distribution of thick disks formed by four different scenarios: i) accretion, ii) heating, III) radial migration, iv) gas rich mergers
17 Conclusions We have compared the eccentricity distribution of thick disks formed by four different scenarios: i) accretion, ii) heating, III) radial migration, iv) gas rich mergers Regardless the mechanism, we find: In-situ population is characterized by a low eccentricity, with mean < >~ Accreted stars dominate the high-eccentricity tail. Differences in -distribution for scenarios i)-iv): Driven by the fraction of in-situ/accreted stars.
18 Conclusions We have compared the eccentricity distribution of thick disks formed by four different scenarios: i) accretion, ii) heating, III) radial migration, iv) gas rich mergers Regardless the mechanism, we find: In-situ population is characterized by a low eccentricity, with mean < >~ Accreted stars dominate the high-eccentricity tail. Differences in -distribution for scenarios i)-iv): Driven by the fraction of in-situ/accreted stars. Encouraging, in view of current and future surveys of the Milky Way (SEGUE, RAVE, GAIA)
19 Simulated galaxies:
University of Groningen
University of Groningen Orbital eccentricity as a probe of thick disc formation scenarios Sales, Laura V.; Helmi, Amina; Abadi, Mario G.; Brook, Chris B.; Gomez, Facundo A.; Roskar, Rok; Debattista, Victor
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