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8th Sino-German Workshop Kunming, Feb 23-28, 2009. Milky Way vs. M31: a Tale of Two Disks. Jinliang HOU In collaboration with : Ruixiang CHANG, Shiyin SHEN, Jun YIN, Jian FU et al. Center for Galaxy and Cosmology Shanghai Astronomical Observatory, CAS. Content.

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8th sino german workshop kunming feb 23 28 2009
8th Sino-German WorkshopKunming, Feb 23-28, 2009

Milky Way vs. M31: a Tale of Two Disks

Jinliang HOU

In collaboration with :

Ruixiang CHANG, Shiyin SHEN, Jun YIN, Jian FU et al.

Center for Galaxy and Cosmology

Shanghai Astronomical Observatory, CAS


Content

  • MW vs. M31: observed properties

    • Halo

    • Disk

  • Two disks: chemical evolution model

  • Summary


  • Milky Way M31

    785kpc from the Sun


    M31 and MWG have similar mass and morphology


    Components in the Milky Way Galaxy

    dark halo

    stellar halo

    thick disk

    thin disk

    bulge

    We would like to understand how our Galaxy came to looklike this.


    The milky way typical or not
    The Milky Way, typical or not?

    • It is always regarded that the MWG is the typical spiral in the universe, especially at its mass range.

    • How about M31 galaxy, it is a spiral that is comparable with MWG in the Local Group, and now it is possible to have detailed observations.


    Differences in general
    Differences : in general

    Halo:

    • M31: metal-rich for field populations

    • M31: more globular clusters ( ~ 3 times )

    • M31: more substructures

      Disk:

    • M31: 2 times larger than MW

    • M31: present day SFR ~ 1/10 of MW

    • M31: gas fraction ~ 1/2 of MW


    Halo properties

    Metal - Velocity

    Tully-Fish Relation

    SDSS: 1047 edge-on spirals

    Hammer et al. 2007


    Halo properties

    X

    X -- M33

    Since M31 has a metal rich halo

    Metallicity – luminosity relation

    Mouhcine et al. 2005


    Halo properties

    Chapman et al. 2006

    X

    Stellar Halo Definition

    Chapman et al (2006 ) kinematically defined stellar halo : metal-poor

    X -- M33

    Metallicity – luminosity relation ???

    Black dot: simulation from Renda et al. 2005


    Halo globular clusters
    Halo Globular Clusters

    Number distribution

     Double peak

    Number:

     M31: 700, metal rich

     MW : 200


    Disk scale length

    M31 distance: 785kpc

    Band Observed scale length ( kpc )

    M31 the Milky Way

    U 7.7

    B 6.6 4.0-5.0

    V 6.0

    R 5.5 2.3-2.8

    I 5.7

    K 4.8

    L 6.1

    Note: SDSS average rd = 4.8kpc (Pizagno et al. 2006)


    Disk profiles
    Disk Profiles

    Total gas fraction

    M31: 1/2 of MW

    Total disk SFR

    MW

    M31

    Yin et al. 2009


    O h gradient from young objects

    Two gradients reported:

    Steep: -0.07 dex / kpc

    (Rudolph et al. 2006 )

    Flat: -0.04 dex/kpc

    (Deharveng et al. 2000

    Dalfon and Cunha 2004)

    [O/H]gradient from young objects

    Scaled gradient

    MWD:-0.161

    -0.093

    M31 :-0.094

    -0.017 dex / kpc


    Scaled profiles
    Scaled profiles

    MW

    MW

    SFR

    Gas

    M31

    M31

    Gas

    fraction

    Gradient




    Purpose of the chemical evolution study for the milky way and m31 disks
    Purpose of the chemical evolution studyfor The Milky Way and M31 disks

    Using the same model

    • Find common features

    • Find which properties are galaxy dependent

    • M31 and MWG, which one is typical ?


    Unified one component model
    Unified One Component Model

    • Disk forms by gas infall from outer dark halo

    • Infall is inside-out

    • SFR:

      • modified KS Law (SFR prop to v/r)


    Why use modified ks law m ks law
    Why use modified KS law (M-KS law)?

    Strong correlation between the average gas mass surface density and SFR density for nearby disk and starburst galaxies (Kennicutt 1998)


    Two types of correlations ks law
    Two types of correlations: KS law

    The later form implies SFR depends on the angular frequency of the gas in the disk. This suggestion is based on the idea that stars are formed in the galactic disk when the ISM with angular frequency Omega is periodically compressed by the passage of the spiral pattern.


    Applications of ks law
    Applications of KS law

    When the Kennicutt law is applied in the detailed studies of galaxy formation and evolution, there are several formulism that often adopted by the modelers :

    SFR 


    Previous work using m ks law milky way disk
    Previous work using M-KS law (Milky Way disk)

    Boissier & Prantzos 1999; 2000

    Boissier et al. 2001

    Hou et al. 2000;2001;2005

    Francois et al. 2004

    Etc……

    Current properties of disk



    How about the history of mwd the evolution of abundance gradient along mwd
    How about the history of MWD ?The evolution of abundance gradient along MWD

    Infall

    SF Law

    Model A, B

    Model C



    Adoption of sfr law for the chemical evolution model of spiral galaxies
    Adoption of SFR Law for the chemical evolution model of spiral galaxies

    M-KS law

    • For the average properties of a galaxies, KS law is OK and (r) = 0.25

    • For local properties, SFR could be local dependent, that is, (r) radial dependent, M-KS law is preferred


    Radial profiles as constrains
    Radial Profiles as constrains

    • Gas profile

    • SFR profile

    • Abundance gradient

    • Metallicity distribution Functions in different positions

    • Do the similar chemical evolution models reproduce the global properties for the Milky Way and M31 disks ?


    SFR

    Yin et al. 2009


    M31 gas and sfr in disk
    M31 gas and SFR in disk

    • Observed of gas and SFR profiles are abnormal when compared with Kennicutt law.

    • Gas and SFR must be modified by some interaction


    Simulation

    Observed

    M32

    Two rings

    structure

    Evidence of M31 disk interaction

    Block et al. (Nature 2006)


    MDFs

    MWD

    age = 13Gyr

    M31 disk

    age = 5-7Gyr

    Yin et al. 2009


    3 summary i comparing two disks
    3. Summary (I): Comparing two disks


    3 summary ii m31 disk properties
    3. Summary (II):M31 disk properties

    • Current star formation properties are atypical in the M31 disk.

      • Disk evolution could be affected by events

    • Has low current SFR in disk

      • Shorter time scale for the infall in disk


    3 summary iii problems in two disks
    3. Summary (III): Problems in two disks

    • Chemical evolution model cannot reproduce the outer profiles of gas surface density and SFR profiles at the same time for M31 disk

    • The observed abundance gradient along the Milky Way disk still not consistent

    • The evolution of gradients is very important.

      Two tracers :

      • PN (Maciel et al. 2003, 2006, 2007)

      • Open Clusters (Chen et al. 2003; 2007; LAMOST Survey)



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