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- WMAP Likelihood

WMAP Likelihood Reionization PPF for CAMB Halo Mass Conversion Cluster Abundance Cosmology 321 Current Topics 282 Galaxies and Universe 242 Radiative Processes 305 Research Preparation 307 GR Perturbation Theory 408 Advanced CMB 448 University of Chicago Astronomy Department KICP Thunch astro ph CO ADS InSpire Fast WMAP Likelihood Code and GSR PC Functions Cora Dvorkin amp Wayne Hu Optimized WMAP7 likelihood code for multicore systems OMPed loops and bottlenecks removed in the following codes WMAP 7yr likelihood F90 br mod dist f90 WMAP 7yr teeebb pixlike F90 updated 4 13 for missing optimizations Update for the WMAP9 likelihood code WMAP 9yr likelihood F90 br mod dist f90 WMAP 9yr teeebb pixlike F90 Speed improvements apply to the Gibbs low l TT likelihood Master TT TE EE likelihood Supplies an approximate replacement for the low l polarization pixel likelihood based on a 2 band EE approach Utilizes the use lowl pol false flag to replace l See Dvorkin Hu 2010 for speed and accuracy tests After first evaluation typical improvement in speed is 5xNcore 5 principal component PC functions of the GSR source function for determining the PC amplitudes of a model eta Mpc S1 S5 eigenfunctions dat 20 principal component

Original URL path: http://background.uchicago.edu/wmap_fast/ (2015-06-26)

Open archived version from archive - WMAP Likelihood

standard reionization parameters For other configurations the 3 main inputs for setting the reionization history x e z are a fiducial x e z model read in from xe fid where column 1 is z and column 2 is x e the principal component functions read in from xe pc with the first row containing the same redshift bins as in the fiducial model file and following rows containing the PCs starting with the lowest variance amplitudes of the n pc lowest variance PCs to specify the reionization model m amp where 1 2 n pc Any number of PCs may be used up to the number supplied in the xe pc file Unused PCs are set to zero amplitude The default configuration uses xez dat for the fiducial xe z and xepcs dat for the PCs This fiducial model has constant x e 0 15 over the range 6 lt z lt 30 and there are 95 redshift bins of width dz 0 25 The PCs are normalized using the conventions of Ref 1 Note that the code has not been tested for ionization variations at z lt 6 since there is strong evidence from quasar spectra that hydrogen is fully ionized after redshift 6 In addition to the usual output from CAMB the reionization history is written to a file if one is specified using xe out The format is the same as for the fiducial x e z file The redshift bins for the fiducial model and the PCs are expected to be identical and should only span the range over which the reionization history is to be varied Outside of this range the ionization fraction is set to nearly zero at high z i e whatever the residual post recombination ionization fraction is and is set to one at low z or slightly more than one for the standard helium reionization settings The order of the redshift bins in the fiducial model and PC files can be either increasing or decreasing but the principal component rows should be in order of increasing variance i e starting with the best measured component Other reionization basis functions may be used instead of principal components as long as the file listing these functions is in the correct format as described above CosmoMC The instructions for CosmoMC are similar to those for CAMB Files for the fiducial ionization history and PCs are the same The example params rpc ini and distparams rpc ini files provided are set up to vary 5 out of a total of 7 ionization PCs in an MCMC likelihood analysis of CMB data The total number of PCs allowed can be changed from 7 by changing num rpc in settings rpc f90 and adding or subtracting lines for the PC amplitudes in params rpc ini and distparams rpc ini The PC amplitudes come after all of the original CosmoMC parameters so they start with parameter 14 Note that if you change num rpc you will also

Original URL path: http://background.uchicago.edu/camb_rpc/ (2015-06-26)

Open archived version from archive - PPF CAMB Module

astro ph CO ADS InSpire PPF module for CAMB Wenjuan Fang The main CAMB code supports smooth dark energy models with constant equation of state and sound speed of one or a quintessence model based on a potential code This modified code generalizes it to support a time dependent equation of state w a that is allowed to cross the phantom divide i e w 1 multiple times by implementing a Parameterized Post Friedmann PPF prescription for the dark energy perturbations see references below Download here The modifications are based on the latest CAMB version of September 2008 Three files are modified i e equations f90 inidriver F90 and params ini and the modified code supports two options to specify w a By setting usew0wa in params cross ini to be true the code reads in w 0 w a and w a is given by w a w 0 w a 1 a By setting usew0wa to be false w a is specified by a user supplied file whose name is given by wafile in params cross ini The file should provide a series of a i w i in increasing order of a i and the size of the series should always i otherwise it just extrapolates the corresponding boundary value outwards The extrapolation is irrelevant if a max 1 and when a a min dark energy is negligible Then to use the code you only need to rename the modified files as the original ones or modify the Makefile to use the alternative f90 files and all remaining procedures are the same as you do with the original CAMB Note the outputted matter power spectra may have up to 10 difference from direct calculations of scalar field dark energy models when k is approaching 10 4 h

Original URL path: http://background.uchicago.edu/ppf/ (2015-06-26)

Open archived version from archive - Mass Conversion

Theory 408 Advanced CMB 448 University of Chicago Astronomy Department KICP Thunch astro ph CO ADS InSpire Halo Mass Conversion Wayne Hu amp Andrey Kravtsov Driver and fitting routines for converting halo mass definitions from one spherical overdensity to another assuming an NFW density profile massconvert f Inputs original mass M Delta and overdensity Delta and concentration c r Delta r s and the desired target overdensity Delta new Overdensity

Original URL path: http://background.uchicago.edu/mass_convert/ (2015-06-26)

Open archived version from archive - Cluster Abundance

Clusters Transfer Function WMAP Likelihood Reionization PPF for CAMB Halo Mass Conversion Cluster Abundance Cosmology 321 Current Topics 282 Galaxies and Universe 242 Radiative Processes 305 Research Preparation 307 GR Perturbation Theory 408 Advanced CMB 448 University of Chicago Astronomy Department KICP Thunch astro ph CO ADS InSpire High Redshift Cluster Abundance Michael Mortonson Wayne Hu amp Dragan Huterer Driver and fitting routines for computing the predicted number of clusters in a ΛCDM cosmology that agrees with CMB SN BAO H 0 measurements up to 2010 at some specified parameter confidence and the mass which would rule out that cosmology at some specified sample confidence Code abundance f Inputs cluster mass defined at an overdensity Delta 200 with respect to the mean density in units of h 1 M s cluster redshift survey area in which it was found sq degrees desired confidence level for ΛCDM parameters e g 0 5 for the typical prediction 0 95 for 95 allowed parameters that maximize the abundance Outputs mean predicted number above the input mass and redshift sample variance exclusion level for finding one such cluster mass required for a 95 sample variance exclusion local slope of the mass function for Eddington

Original URL path: http://background.uchicago.edu/abundance/ (2015-06-26)

Open archived version from archive - Ast 321

Large Scale Structure inflationary perturbation theory Padmanabhan Structure Formation in the Universe non linear collapse In the syllabus below I give a cross reference to Peacock s book for further reading Requirements There will be weekly problem sets 50 and a final project 50 For a final project you may work in groups of 5 or fewer people on any of the following Particle Mesh N Body Code Inflationary Perturbation Solver Einstein Boltzmann Code Halo Model Code Monte Carlo Markov Chain You may also come up with your own comparable numerical project or be creative and develop a webApp or iApp If you are truly computation averse see me for permission to do a reading project You will present your project to the class at the end of the quarter and submit the PDF of the presentation for linkage here Extra credit if you make your code publically available Problem Sets Problem Set 1 Due Jan 14 Problem Set 2 Due Jan 21 Problem Set 3 Due Jan 28 Problem Set 4 Due Feb 4 Problem Set 5 Due Feb 11 Problem Set 6 Due Feb 25 Problem Set 7 Due Mar 4 Final Project Preparation Each project has a core set of things that I expect you to accomplish I encourage you to develop your codes further in ways of your choosing to develop a more extensive toolbox N body Group Follow Andrey Kravtsov s Notes Halo Model Group Read Cooray Sheth Phys Rept 372 2002 1 129 e Print astro ph 0206508 and construct the halo model nonlinear matter power spectrum out the 1 halo 2 halo terms halo bias and the NFW profile You may find these excersises helpful Problem Set 1 Problem Set 2 Problem Set 3 Problem Set 4 but you do not need to

Original URL path: http://background.uchicago.edu/~whu/Courses/ast321_11.html (2015-06-26)

Open archived version from archive - Ast 282

Material 96 nbsp PhD Thesis 95 Baryon Acoustic Oscillations Cosmic Shear Clusters Transfer Function WMAP Likelihood Reionization PPF for CAMB Halo Mass Conversion Cluster Abundance Cosmology 321 Current Topics 282 Galaxies and Universe 242 Radiative Processes 305 Research Preparation 307 GR Perturbation Theory 408 Advanced CMB 448 University of Chicago Astronomy Department KICP Thunch astro ph CO ADS InSpire Current Topics Astro 282 WF 4 30 5 50 AAC 107 Office Hours TBA First Meeting 3 29 Description This course will introduce topics of current interest in Cosmic Microwave Background research acoustic peaks in the primary anisotropy power spectrum CMB polarization and secondary anisotropy due to the large scale structure in the universe Reading Material Lecture Notes updated 4 10 for with a stat mech supplement Cosmic Microwave Background Review On line CMB tutorials Helper reference on FRW cosmology Slides Overview 1 Overview 2 Overview 3 Requirements Problem sets This is 60 of your grade Final projects Oral Component in class 1 2 lecture hour presentations and Written component a write up of the presentation OR a web page with graphics This is 40 of your grade Problem Sets PS 1 Due April 7 PS 2 Due April 14 PS

Original URL path: http://background.uchicago.edu/~whu/Courses/ast282_06.html (2015-06-26)

Open archived version from archive - Ast 242

Likelihood Reionization PPF for CAMB Halo Mass Conversion Cluster Abundance Cosmology 321 Current Topics 282 Galaxies and Universe 242 Radiative Processes 305 Research Preparation 307 GR Perturbation Theory 408 Advanced CMB 448 University of Chicago Astronomy Department KICP Thunch astro ph CO ADS InSpire Galaxies and the Universe Astro 242 MW 1 30 2 50 TAAC 41 The textbook for this course is Carroll and Ostlie An Intro to Modern Astrophysics Addison Wesley 2006 We will cover Chapters 24 30 at a rate of a chapter per 1 2 weeks Ch 24 Milky way Ch 25 Nature of galaxies Ch 26 Galactic evolution Ch 28 Active galaxies Midterm Ch 27 Structure of the Universe Ch 29 Cosmology Ch 30 Early universe Final Grades will be based on problem sets 50 in class midterm 20 and final 30 Problem Sets PS 1 due 1 14 24 4 24 15 24 18 24 20 24 23 PS 2 due 1 26 25 2 25 4 25 14 25 15 25 16 PS 3 due 2 2 26 1 26 4 26 11 26 12 PS 4 due 2 9 28 6 28 9 28 13 28 14 28 15 28 18 Prepare

Original URL path: http://background.uchicago.edu/~whu/Courses/ast242_15.html (2015-06-26)

Open archived version from archive