Workshop "Cosmology with Small Scale Structure" Jul 2226, 2013
Workshop "Cosmology with Small Scale Structure"
Informal workshop to discuss cosmological constraints from the full predictions of clustering of galaxies and matter including scales within dark matter halos. The workshop will be focused on tests that use e.g. galaxygalaxy correlation, clustergalaxy crosscorrelation, clustermass crosscorrelation, redshiftspace correlation function, marginalized over the galaxyhalo connection, to constrain cosmological parameters. We intend a working workshop, with discussions and active testing, and a few formal presentations.
major topics
 accuracy of theoretical models for galaxygalaxy and galaxymass correlations
 discuss and compare various statistics, e.g. xi_clg (clustergalaxy crosscorrelation (or M/N)), xi_clm (clustermass crosscorrelation), xi_gg(\sigma,\pi) (redshiftspace correlation function)
 theoretical uncertanties: which dominate and how can they be reduced?
 observational uncertanties: which dominate and how can they be reduced?
 is it really robust and competitive? how do we convince ourselves and others?
Dates
July 22 (Mon)  26 (Fri), 2013
Place
Conference room AB, Kavli IPMU, the University of Tokyo **The room was changed!**
Organizers
 Alexie Leauthaud (Kavli IPMU)
 Surhud More (Kavli IPMU)
 Masahiro Takada (Kavli IPMU)
Speakers
 Martin White
 Frank van den Bosch
 Kazuya Koyama
 Jeremy Tinker
 Andreas Berlind  and others …
Schedule
Monday 22
Smallscale statistics
 state of the art for various statistics: xi_gg, xi_gm, xi(rp, pi), M/N
 systematics for theoretical formulation
 systematics for practical implementation on e.g. des, lsst
 systematics in numerical simulations
 should we invent new statistics?
MODERATORS : Risa / Jeremy / Frank
Time  Discussion leaders  Topic & key questions 
9:30  Risa  Big Picture. 
10  Alexie  Quick summary of discussion from last meeting 
12  1  lunch  
1  2 


Open discussion and work time  
Tuesday 23
Simulations
 How accurately do we now know the ingredients that go into analytic halotype models: mass function, halo clustering, halo structure?
 What are the systematic errors due to ICs, Nbody codes, resolution, box size?
 What are the systematic errors due to halofinding algorithms? Does it matter what halo definition we use?
 What are the systematic errors due to not including baryons? Can we easily account for the effect of baryons without running gas simulations?
 How "universal" are these properties (mass function, etc), i.e., what is the error in using an analytic function for a given cosmological model, when it was derived using a different cosmology?
 Do we understand assembly bias well enough to account for it in our modeling?
 Is it better to bypass these halo properties and measure galaxy statistics directly by populating simulations? What are the systematic errors on statistics like the correlation function from all the items listed above?
 Can we get away with approximating different cosmological models by intelligently rescaling a small number of boxes? What are the errors caused by this? If we need to run many boxes to cover the cosmological parameter space, can we interpolate to make the problem tractable? How should we interpolate?
 The answers to all these questions will depend on the statistic and physical scale in question. That is a lot of information to compile. What of all this should we focus on?
MODERATORS: Salman / Katrin / Andreas
Time  Discussion leader  Topic & key questions 
9:30  12  Salman/Katrin/Andreas  
12  1  lunch  
1 1:30  
1:30  2  
2  2:30  
evening  WORKSHOP DINNER 
Wednesday 24
Redshift space distortions
MODERATORS: Martin / Masahiro / Jeremy
Time  Discussion leader  Topic & key questions 
9:30 12  Martin / Masahiro / Jeremy  
Jeremy  challenges for boss/ challenges for elg surveys (hetdex, eboss, bigboss)  
12  1  lunch 

1  2  
Thursday 25
Morning : Effects of baryons
Afternoon : modified gravity
MORNING MODERATORS : Joop / Andrew
AFTERNOON MODERATORS : Kazuya
Time  Discussion leader  Topic & key questions 
9:30 12  Joop Schaye / Andrew Zentner  
12  1  lunch 

1  3  Kazuya  Modified gravity 
Friday 26
optical cluster finding
 stateofthe art update (redmapper)
 where will be by the end of DES?
 which observational systematics can be informed by simulations?
 applications to smallscale modeling, including lensing and M/N
MODERATORS : Eduardo / Andrew /
Time  Discussion leader  Topic & key questions 
9:30  Eduardo  State of the art of cluster finding 
10  12  Eduardo / Andrew Wetzel  
12  1  lunch  
1 2  Summary by Frank  
Open discussion and work time  
EVENING  BBQ IN PARK 
Registration
Online registration form (Indico page) is available here.
Access to Kavli IPMU
http://www.ipmu.jp/visitors/accessipmu
Accommodation
http://www.ipmu.jp/visitors/accommodation
Visa Information
http://www.mofa.go.jp/j_info/visit/visa/short/novisa.html#list