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Comparative Analysis of Milky Way and M31: Insights from the 8th Sino-German Workshop

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36 diapositives · 507 Views · Sep 11, 2014

The 8th Sino-German Workshop held in Kunming from February 23-28, 2009, focused on comparing the properties of the Milky Way (MW) and Andromeda (M31) galaxies. This study highlighted the observed similarities and differences in their halos and disks, exploring aspects such as chemical evolution, star formation rates, and structural differences. The findings suggest that while the Milky Way is often deemed typical among spiral galaxies, M31 presents intriguing deviations that contribute to our understanding of galaxy formation and evolution.

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Comparative Analysis of Milky Way and M31: Insights from the 8th Sino-German Workshop
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  1. 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

  2. Content • MW vs. M31: observed properties • Halo • Disk • Two disks: chemical evolution model • Summary

  3. Observed properties: MW vs. M31 Milky Way M31 785kpc from the Sun

  4. M31 and MWG have similar mass and morphology

  5. 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.

  6. 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.

  7. 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

  8. Halo properties Metal - Velocity Tully-Fish Relation SDSS: 1047 edge-on spirals Hammer et al. 2007

  9. Halo properties X X -- M33 Since M31 has a metal rich halo Metallicity – luminosity relation Mouhcine et al. 2005

  10. 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

  11. Halo Globular Clusters Number distribution  Double peak Number:  M31: 700, metal rich  MW : 200

  12. 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)

  13. Disk Profiles Total gas fraction M31: 1/2 of MW Total disk SFR MW M31 Yin et al. 2009

  14. 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

  15. Scaled profiles MW MW SFR Gas M31 M31 Gas fraction Gradient

  16. Observed disk properties:summary

  17. Two disks: chemical evolution comparison

  18. 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 ?

  19. 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)

  20. 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)

  21. 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.

  22. 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 

  23. 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

  24. This modified KS law is very successful in predicting the current properties of disk • Not much TESTED for the disk history – less constrains available • Recently, observed abundance gradient from Open Clusters and Planetary Nebulae have made this possible

  25. How about the history of MWD ?The evolution of abundance gradient along MWD Infall SF Law Model A, B Model C

  26. Fu et al. 2009

  27. 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

  28. 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 ?

  29. SFR Yin et al. 2009

  30. 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

  31. Simulation Observed M32 Two rings structure Evidence of M31 disk interaction Block et al. (Nature 2006)

  32. MDFs MWD age = 13Gyr M31 disk age = 5-7Gyr Yin et al. 2009

  33. 3. Summary (I): Comparing two disks

  34. 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

  35. 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)

  36. Thanks