kiaa/pku -- ioa workshop “near field cosmology” beijing, dec 1-5, 2008 star formation and...
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KIAA/PKU -- IoA workshop
“Near Field Cosmology”Beijing, Dec 1-5, 2008
Star Formation and Chemical Evolution of the Milky Way and M31 Disks
Jinliang HOU
In collaboration with :
Ruixiang CHANG, Jun YIN, Jian FU, Li CHEN, Shiyin SHEN et al.
Center for Galaxy and CosmologyShanghai Astronomical Observatory, CAS
A short introduction of our group
Star Clusters and the Structure of Galaxies
Astronomical Mansion
Shanghai Astronomical Observatory, CAS
Research interests of the group
Structure and evolution of galaxies---- from the Milky Way to high z galaxies
Star clusters and the structure of the Milky Way Galaxy Chemical evolution of the galaxies, high-z galaxies (ma
inly Damped Lyman Alpha systems) Structure and dynamics of the nearby galaxies Large sample analysis of the nearby galaxies (SDSS,
Galex, 2MASS, LAMOST et al. ) Galaxy formation and evolution
PhD students:
1. YIN Jun
2. LIU Chenzhe
3. SHI Xihen
4. GAO Xinhua
5. Wang Caihong
6. GAN Jinalin (now in Heideberg, MPIA),
7. HAN Xuhui (now in Paris Observatoire)
8. FU Jian (now in Munich, MPA)
MS Students:
1. YU Jinchen
2. WANG Youfen
Staff
1. HOU Jinliang
2. CHEN Li
3. SHAO Zhenyi (now
in UMASS, USA)
4. CHANG Ruixiang
5. SHEN Shiyin
Senior Professors :
1. ZHAO Junliang
2. FU Chenqqi
3. WANG Jiaji
Some international collaborators: White S.D.M, Kauffmann G. (MPA)
Prantzos N. (IAP)
Boissier S. (Observatoire de Marseille)
Tytler D. (UCSD)
Mo Houjun (UMASS)
Levshakov S. (Ioffe Institute of Physical Technique)
de Grijs R. (U. Sheffield)
Some group members
Local SFR Law in the Milky Way disk based
on abundance gradient evolution
Observed differences between M31 and MW
disks
Model comparisons between M31 and Milky
Way disks
Summary
Content
Local SFR Law in the Milky Way disk based on abundance gradient evolution
Kennicutt Law --- average properties
Strong correlation between the average gas mass surface density and SFR density for nearby disk and starburst galaxies (Kennicutt 1998)
Two types of correlations
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 Kennicutt SFR 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
The evolution of abundance gradient along the Milky Way disk
Infall
SF Law Model A, B
Model C
Fu, Hou, Chang et al. 2009
Adoption of SFR Law for the chemical evolution model of spiral galaxies
1. For the average properties of a galaxies, KS law is OK
2. For local properties, SFR could be local dependent, a simple description is the introducing of angular velocity (Silk 1997, Kennicutt 1998 )
Observed differences between M31 and MWG
M31 and MWG have similar mass and morphology
Components in the Milky Way Galaxy
dark halo
stellar halo
thin disk
thick disk
bulge
We would like to understand how our Galaxy came to look like this.
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.
Is this true?
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.
Disk Profiles
Yin, Hou, Chang et al. 2009
Total disk SFR
MW
M31
[O/H] gradient from young objects
- 0.017 dex / kpc
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) Scaled gradient
MWD: - 0.161 - 0.093
M31 : - 0.094
Scaled profiles
MW
M31
MW
M31
Gas SFR
Gasfraction
Model comparisons between M31 and Milky Way 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 ?
Model classification
Disk only : One component : Disk (Hou et al.) Two components : Thick Disk + Thin Disk (Chang et al.)
Disk+Halo:Two components : Disk +Halo Three components : Thick Disk + Thin Disk + Halo
Disk+Halo+Bulge:Three components : Bulge+Disk+Halo
Semi-Analytical Model Phenomenological Model /
Unified One Component Model
1. Disk forms by gas infall from outer dark halo
2. Infall is inside-out
3. SFR: modified KS Law (SFR prop to v/r)
M31 disk MW disk
Mtot (Ms) 7 1010 3.5 1010
rd (kpc) ( R band) 5.5 2.3
Vflat(km/s) 220 226
Radial Profiles as constrains
• Gas profile • SFR profile• Abundance gradient
Do the similar chemical evolution models
reproduce the global properties for the Milky
Way and M31 disks ?
SFR
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
Block et al. (Nature 2006)
Observed
Simulation
M32 Two rings structure
Summary : M31 disk properties
1. Current star formation properties are atypical in the M31 disk.
Disk formation be affected by interactions
2. Has low SFR in disk shorter time scale for the infall. contradicts the longer infall time scale for halo.
Problems
Chemical evolution model cannot reproduce the outer profiles of gas surface density and SFR profiles at the same time
The observed abundance gradient along the Milky Way disk still not consistent
The evolution of gradients is very important. Two tracers :
1. PN (Maciel et al. 2003, 2005, 2006, 2007) and
2. Open Clusters (LAMOST Survey, CHEN Li’s talk, this workshop)
Comparison among MW, M31 and M33
MWD M31 disk M33 disk(Yin Jun’s talk )
Infall
Timescale
Quiet
7Gyr
Interaction
7Gyr
SlowAccretion
15Gyr
SFR Local dependent
Modulated by events
Local dependent
Outflow No No Yes
Abundance Gradient
Steep/flat ? Flat Steep
Thanks
Observed difference between M31 and Milky Way galaxies
Hammer et al. 2007
Halo properties
Metal - Velocity
Tully-Fish Relation
SDSS: 1047 edge-on spirals
Mouhcine et al. 2005
Halo properties
Metallicity – luminosity relation
X
X -- M33
Disk scale lengthDisk scale length
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 = 4.75kpc (Pizagno et al. 2006)
M31 distance: 785kpc
AM prop to rdVrot
(Mo et al. 1998)
Disk specific angular momentum Disk specific angular momentum (AM)(AM)
Hammer et al. 2007
MW is about a factorof 2 less than nearby spirals
Observation: which galaxy is a “typical” spiral?
Statistical
Zibetti et al. (2004) from SDSS survey: 1000 edge-on disc galaxies, metal-rich halo is more common.
Harris & Harris (2001) NGC5128 similar to M31 halo
Metal-rich seems more common
How halo forms ? Why metal-rich ?Does observed halo really halo?
• M31 : metal-rich halo• MWG: metal-poor halo
Observational constrains in the solar neighborhood
• Find a set of parameters that can best reproduce some observational constrains in the solar neighborhood.
• Observables of the Milky Way Galaxy
1. MDF (Metallicity Distribution Function)
disk and halo
2. [O/Fe] versus [Fe/H] from metal poor to metal rich
3. SFR at present time
Physics of the model : Gas infall and star formation proceeds in each ring
Physical process
Disk profile • Gas • SFR • Abundance gradients• other global quantities
Rings independent
Solar neighborhood• Gas fraction• Abundance ratio [O/Fe] ~ [Fe/H]• G-dwarf metallicity etc.
Infall Model
• Two time scales: – h depends on the halo formation mechanism
– d as a function of radius, disk formation
Halo Disk delayed by tdelay
Phenomenological Model
Star formation: Kennicutt law
Halo
Disk
Chemical evolution Gas of an element i
Gas depletion
Low mass
SNIa
IMS star
SNII
Halo and disk
K dwarf
Halo
Halo :
Disk :
Disk and halo surface density profile
Disk : exponential Halo: modified Hubble law
Metallicity Distribution in the MW Disk and Halo
Infall Model
• Two time scales: – h depends on the halo formation mechanism
– d as a function of radius, disk formation
Halo Disk delayed by tdelay
Phenomenological Model
[O/H] gradient from young objects in the Milky Way Disk
- 0.07 dex / kpc
Rudolph et al. 2006
Halo Globular Clusters
Number distribution
Double peak
Number:
M31: 700
MW: 162
[Fe/H] gradient from Open Clusters in the Milky Way disk
All Open Clusters : age mixed - 0.063dex/kpc
Chen, Hou, Wang (2003)
Summary – 2 :
possible correlation between halo Z and Mstar
• Model predicts more massive stellar halo in M31, about 6 to 9 times than that of MW halo.
• Massive halo has higher metallicity.
Bekki, Harris & Harris (2003) simulation :
Stellar halo comes from the outer part of the progenitor discs when the bulge is formed by a major merger of two spirals.
Correlation between halo metallicity and bulge mass
What we can do next for M31 ?
• Similar model, at present, we only concentrate on disk
• Need to include halo also, a lot of observations are available for the halo, especially in the field of globular clusters.
• To add the color evolution, this is important to constrain the model, is it possible to consistent between chemical and color ?
• To solve the problem of low gas density in the outer disk, introduce new assumption ? – Higher outer disk SFE ?
– Wind in the outer disk ?
– Interaction ?