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challenges in scientific computing and data analysis
Matthias Steinmetz
Modelling the Milky Way:Modelling the Milky Way:
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Can
we
form disk
galaxies?
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Not really
Formation of disks has been notoriously difficultFeedback?Resolution?Numerical Methods?
AMR vs
SPH
Remember: on galacticscales, hydrodynamicsis an approximation (probably) !What is the mass of MW-typeDM halo
Abundance M~2.51012 MStellar dynamics M~1012 M
Agertz
et al, 2010
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Vcirc
and Vesc
from SDSS
Xue
et al 2008
RAVE
12
21.018.0
10
82.0
= +ACnoM
M12
40.030.0
10
21.1
= +ACMM
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Compare SDSS stellar mass function with DM halo mass function
M12105.2 =MWM
Forero
et al 2009Guo
et al 2009
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We still do not really understand how to form disk galaxies
Guo
et al 2009
Agertz
et al, 2010
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Most of the angular momentum comes in late and thus at low density
Navarro & MS 1997
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The local universe is not a representative part of the universe. The MW is situated in a region of relatively low density and with large nearby mass concentrations like Virgo, the local supercluster, Perseus
Pisces and Coma
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Local Group alikes
are pretty rare!
analysis of 90 Mpc box, constrained simulationWMAP5 normalizationone excellent candidate
Virgo:
Mass: 1.21014 M
(more massive)
distance: 14.9 Mpc
(19.0 Mpc
NED)
Fornax:
mass: 4.2 1013 M
(7.01013 M
ApJ
548, L139)
distance: 19.2 Mpc
(17.6 Mpc
NED)
Local group
mass: 3.01013M
(lower mass end)
MW/Andromeda distance: 690kpc (700kpc)
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CLUES
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Metz, Kroupa
& Jerjen
2009
complete!
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Libeskind
et al 2005
6 DM only simulations, populated with galaxies semi-
analytically.
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MWM31
Preferential
infall
of satellites
Libeskind
et al, 2011
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MWM31
Preferential
infall
of satellites
Quadrupole: infall
along
a filamentPointing
towards
Virgo
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The
MW is
not
a typical
galaxy
Forero
et al, 2011
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Doumler
et al, 2011
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Doumler
et al, 2011
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How about observations?
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The Milky Way is all around us!
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How about observations?
The substructure crisisSystematic searches using large imaging surveys (SDSS) reveal a considerable (sufficient?) number of new satellites
Substructure in phase space tracing the formation history of the Milky Way
Lot of activities following the discovery of Sagittarius dwarf
ImagingSDSS, PanStarrs, Euclid, LSST
SpectroscopySDSS, RAVE, GAIA, HERMES, 4MOST
AstrometryHipparcos & GAIA
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Velocity Substructure in RAVE
Williams et al, 2010
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Velocity Substructure in RAVE
Williams et al, 2010
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Illustrative simulations
Williams et al, 2010
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Recent disruption event
Williams et al,2010
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Mary Williams http://www.rave-survey.aip.de/rave/
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Outlook: The GAIA epoch
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The Future: GAIA
Cornerstone mission of ESAScheduled for launch in late 2012Main objective: To create the largest and most precise three dimensional chart of our Galaxy by providing unprecedented positional and radial velocity measurements for about one billion stars in our Galaxy and throughout the Local Group.
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Schedule
ProposalConcept
& Technology StudyMission Selection
Re-Assessment
StudyPhase
B1
Scientific
operation
Launch late 2012
Final
Studies
Mission Data Processing
Implementation
Data Processing
Definition
Operation
Mission Products Intermediate
Selection of Prime Contractor (EADS Astrium)
Phase
B2Phase
C/D
Software Development
1995
2000
2005
2010
2015
2020
19941993
1997
1998
1999
2019
20182017
2016
2014
2013
2012
2011
2009
2008
2007
2006
2004
2003
20022001
1996
2021
NowFigure courtesy Michael Perryman and Franois Mignard
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Light Bending in Solar System
Light bending in microarcsec, after subtraction of the much larger effect by the Sun
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The Future: GAIA
RAVERAVE
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GAIA
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One Billion Stars in 3-D will Provide
in our Galaxy the distance and velocity distributions of all stellar populationsthe spatial and dynamic structure of the disk and haloits formation historya detailed mapping of the galactic dark-matter distributiona rigorous framework for stellar structure and evolution theoriesa large-scale survey of extra-solar planets (~15,000)a large-scale survey of Solar System bodies (~250,000)
and beyonddefinitive distance standards out to the LMC/SMCrapid reaction alerts for supernovae and burst sources (~20,000)QSO detection, redshifts, microlensing structure (~500,000)fundamental quantities to unprecedented accuracy: to 210-6 (210-5 present)
Fundamental physics - reference frame - solar system - extrasolarplanets -stellar systems - stellar physics - Galactic astronomy - quasars and galaxies.
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challenges in scientific computing and data analysis Slide Number 2Can we form disk galaxies?Not really Vcirc and Vesc from SDSSCompare SDSS stellar mass function with DM halo mass functionWe still do not really understand how to form disk galaxiesMost of the angular momentum comes in late and thus at low densitySlide Number 9Slide Number 10Local Group alikes are pretty rare!Slide Number 12CLUESSlide Number 14Slide Number 15Preferential infall of satellitesPreferential infall of satellitesThe MW is not a typical galaxy Slide Number 19Slide Number 20How about observations?The Milky Way is all around us!How about observations?Velocity Substructurein RAVEVelocity Substructurein RAVEIllustrative simulationsRecent disruption eventSlide Number 28Slide Number 29The Future: GAIAScheduleLight Bending in Solar SystemThe Future: GAIAGAIAOne Billion Stars in 3-D will ProvideSlide Number 36
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