stellar migration in disks and disk outskirts victor p. debattista r. ro š kar, s. loebman, p....
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Stellar Migration in Stellar Migration in Disks and Disk Disks and Disk
OutskirtsOutskirtsVictor P. Debattista
R. Roškar, S. Loebman, P. Yoachim, A. Brooks, G. Stinson, T. Kaufmann, T. Quinn, J. Wadsley, C. Brook, F. Governato, J. Dalcanton
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Sellwood & Binney (2002) demonstrate that spirals
can migrate stars over large distances at the CR
without heating
Migration can be inward or outward directed
Galactic archaeology in which strata are jumbled
Migration can be quantified by considering low
density regions
Stellar Migration
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Simple Picture of Galaxy Formation
gasdark matterNFW, MW c
e.g. Fall & Efstathiou (1980), Dalcanton et al. (1997)Also viscous evolution - Lin & Pringle (1987), Ferguson & Clarke (2001)
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Approximate disk formation via dissipational collapse after last major merger using SPH code GASOLINE
• 1M particles in each component, Mvir = 1012 M
• 10% baryons by mass • ~ 106 M per DM particle• initially 1.4x105 M per gas 4.6x104 M per star
• 50 pc force resolution for baryons, 100 pc for DM• star formation and feedback (Stinson et al. 2007) including feedback from SN Ia, II and stellar winds
Advantages:• fully self-consistent evolution• no ad-hoc assumptions about the disk• full modeling of dynamical processes• star formation and feedback allow for direct comparisons with observations (age, metallicity, SFR etc.)
Simulations
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Model Galaxy Properties
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Steady heating~ t0.53
Velo
cit
y D
isp
ers
ion
[km
/s]
Age [Gyr]
Data: Geneva-Copenhagen survey (Holmberg 2009)
Age [Gyr]Age [Gyr]
Simulation
Steady heating~ t0.35
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60% truncated10% pure expo.
Pohlen & Trujillo 2006
van der Kruit 1979
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Consistent with observations of de Jong (1996), Bell & de Jong (2000), MacArthur (2004)
But why is there an upturn?
• stellar disk is clearly extended beyond end of SF• if populated by stars formed in-situ, there shouldn’t be an age minimum
Outer disk is populated by material from the inner disk
Roškar et al. 2008
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Very few particles beyond the break actually formed there
(plots show particles on mostly circular orbits)
Radial Migration Populates Outer DiskR
fin
al
Rform
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(Roškar et al. 2008a)
Very few of the stars beyond the ``break’’ actually born there
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Most particles in the outer disk still retain nearly circular orbits
RbRb
All
Circular
Outer Disk Kinematics
J/Jc(E)
Outer disk only
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a) Fourier expansion -> b) power spectrum -> c) identify patterns/resonances
a)
b)
c)
Confirming Role of Spirals
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HST star count profiles
Rbr the same for all pops
Age
Comparison to NGC 4244
Possible interpretations
Break just formed
Break has never changed
Radial migration forces stars to adopt a common break radius
de Jong et al. 2007
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simulation HST star count profiles
Rbr the same for all pops
Age
Comparison to NGC 4244
de Jong et al. 2007
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Stacking Galaxies
Azzollini et al. 2008
No breaks
Breaks Anti-breaks
All rest frame ~ u-g
> 1010Msun < 1010Msun
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NGC 6155
Break at 34” (Pohlen & Trujillo 2006)
Data using VIRUS-P on 2.7-m HJS telescope 1.7’ x 1.7’ fov. Rebin data to S/N ~45 beyond break
Fit the spectra using GANDALF (Sarzi et al. 2006) assuming exponential SFH and varying metallicity
Yoachim et al. 2010
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Reconstructing the SF History
Except for small radii, assuming that a star was born where it currently is leads to gross errors in the local SFR
MeasuredActual
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How much are SFH determinations in NGC 300 influenced by radial mixing?• simulation with lower total mass -> spirals of smaller amplitude -> less migration• could be influenced by interactions (might be the case with M33)
MW ~1012 Msun
NGC 300 ~ 1011 Msun
(Gogarten et al. 2010)
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Outer Disk Contamination
Roskar et al. 2010
The outer disk is contaminated also by stars forming in situ, in the warped region.
Sanchez-Blazquez et al. 2009
Martinez-Serrano et al. 2009
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Roskar et al. 2010
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Could significantly affect:• outer disk surface density• age distribution• metallicityBut - migration still dominates
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Predicting What Anti-Centre Survey Might Find
Expect the mean age of disk stars to increase beyond the break.
The variation of outer disk scale-length for different age stellar bins constrain migration rates
Mean
ag
e
IntermediateYoun
g
Old
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Predicting What Anti-Centre Survey Might Find
[Fe/H] continues to decline with radius: some of the oldest disk stars present here. The solar neighborhood, instead, is contaminated by younger, more metal rich, stars, increasing the mean.
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“Solar” Neighborhood
Most of the stars in the solar neighborhood (7 < R < 9 kpc) formed elsewhere. The metal poor ones come from a wide range of radii, including from outside the solar neighborhood, while the metal rich ones come from inside the solar radius.
Rform
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“Solar” Neighborhood
Assuming stars remain in situ, we find a significant gradient and low dispersion in AMR. But AMR is flattened & broadened by migration, which is true also for stars on circular orbits. Note: increase in metallicity of old stars and increasing scatter with age
Age
[Fe/
H]
Edvardsson et al. 1993, Nordstrm et al. 2004, Haywood 2008
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• A “thick” disk detected in star counts as a function of height in the solar neighborhood
• Also considered distinct in metallicity, velocity dispersion and age
• Various formation hypotheses… accretion of satellites, heating by minor mergers, rapid formation after the last major merger…
Two components
(Gilmore & Reid 1983)
Thin disk
Thick disk Sun
Thick Disk Formation
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Effect on Vertical Direction
If vertical action is conserved by migration then stars moving outwards puff up and vice-versa
Is there such a thing as a dynamically distinct thick disk?
Schoenrich & Binney 2009
Sales+ 2009
Caruana 2009
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Thin disk
Thick disk
Testing Thick Disk Formation
See also Amina’s talk
z
Metal poor + slow rotation
Metal rich + fast rotation
In transition region, V should correlate with [Fe/H]
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Decreasing metallicity and vrot with height
Thick Disk: An SDSS Puzzle
Ivezic+ 2008
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Stars form with a single expo profile but quickly develop a second component
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More stars formed in situ at high ; smaller variation in radial density across migration scale
EXPECT less of a “bimodality” in vertical density
= 0.039 = 0.1
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Stars are born on circular orbits and hence have no correlation between V and [Fe/H]. Heating brings stars into the local volume creating a correlation. Migration shuffles [Fe/H] and erases the correlation
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Profiles of mean metallicity changes for a chemical selection. <[/Fe]> separates for kine. selection
Bensby+2003, 2005; Feltzing 2006
0.1 dexSee Venn’s talk
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Predicting What LAMOST Might Find
Separating stars by [O/Fe], the -enhanced (older) population should have no correlation of V versus [Fe/H] while the lower [O/Fe] (younger) stars will show a correlation
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Migration complicates Galactic archaeology
and needs to be quantified to decipher the
clues to galaxy formation inherent in
observational data
Migration can account for a wide range of
observational data, in both the Milky Way and
external galaxies.
Faint regions of disk galaxies contain
important clues to past migration and are
prime targets for quantifying migration rates
Conclusions