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London Hack Days on the CMB, CLASS and Monte Python PDF

87 Pages·2014·1.1 MB·English
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Preview London Hack Days on the CMB, CLASS and Monte Python

London Hack Days on the CMB, CLASS and Monte Python (a) (a,b,c) (d) Benjamin Audren , Julien Lesgourgues , Jesus Torrado , (a) T h o m a s T r a m (a)EPFL, (b)CERN, (c)LAPTh, (d)Leiden London, 12-16.05.2014 J. Lesgourgues Lecture I: Introduction Almost any type of research activity in cosmology will use a Boltzmann code at some point Computing CMB anisotropy spectra: scalar and tensor spectra for TT, EE, BB -9 10 -10 10 -11 10 -12 10 -13 10 -14 10 -15 10 -16 10 10 100 1000 l J. Lesgourgues Lecture I: Introduction l(l+1)Cl/2π Almost any type of research activity in cosmology will use a Boltzmann code at some point Computing matter power spectrum: matter power spectrum (linear, Halofit) 5 10 z=0 4 z=2 10 3 10 2 10 1 10 0 10 -1 10 -4 -3 -2 -1 0 10 10 10 10 10 k [h/Mpc] J. Lesgourgues Lecture I: Introduction 3 P(k,z) [Mpc/h] Almost any type of research activity in cosmology will use a Boltzmann code at some point C o m p u t i n g t r a n s f e r f u n c t i o n s ( e . g . i n i t i a l c o n d i t i o n s f o r N - b o d y ) : d e n s i t y t r a n s f e r f u n c t i o n s a t z = 1 0 0 4 1 0 3 p h o t o n s 1 0 b a r y o n s 2 C D M 1 0 n e u t r i n o s 1 1 0 0 1 0 - 1 1 0 - 2 1 0 - 3 1 0 - 4 1 0 - 5 1 0 - 4 - 3 - 2 - 1 0 1 1 0 1 0 1 0 1 0 1 0 1 0 k [ h / M p c ] J. Lesgourgues Lecture I: Introduction -δ( kτ,) R/ ( kτ,i n)i Targets Computing matter density (number count) spectra, or lensing angular spectra: linear and nonlinear lensing potential spectrum -7 10 z=0.1 -8 z=0.3 10 z=0.5 -9 10 -10 10 -11 10 -12 10 sources in gaussian windows of width ∆z = 0.1 -13 10 10 100 l J. Lesgourgues Lecture I: Introduction 2 [l(l+1)] Cl/2π Almost any type of research activity in cosmology will use a Boltzmann code at some point Computing background evolution in a given cosmological model: 15 10 radiation matter 1010 Lambda 5 10 0 10 -5 10 -10 10 -15 10 1 10 100 1000 10000 conformal time (Mpc) J. Lesgourgues Lecture I: Introduction 2 densities (Mpc ) Almost any type of research activity in cosmology will use a Boltzmann code at some point Computing thermal history in a given cosmological model: 0 10 -1 10 -2 10 -3 10 -4 10 1 10 100 1000 10000 z J. Lesgourgues Lecture I: Introduction xe As a theorist... ... you may want to develop the code for incorporating new physics and compute/understand the e↵ects of your favourite model on observables As both... ... you want to infer constraints on cosmological parameters from a new dataset ... you want to test your own favorite model, given existing data ... you want to predict the sensitivity of a future experiment to a given parameter Almost any type of research activity in cosmology will use a Boltzmann code at some point As an observer... ... you want to compute these quantities easily and eciently ... you may want to develop the code for outputting new observables J. Lesgourgues Lecture I: Introduction As both... ... you want to infer constraints on cosmological parameters from a new dataset ... you want to test your own favorite model, given existing data ... you want to predict the sensitivity of a future experiment to a given parameter Almost any type of research activity in cosmology will use a Boltzmann code at some point As an observer... ... you want to compute these quantities easily and eciently ... you may want to develop the code for outputting new observables As a theorist... ... you may want to develop the code for incorporating new physics and compute/understand the e↵ects of your favourite model on observables J. Lesgourgues Lecture I: Introduction Almost any type of research activity in cosmology will use a Boltzmann code at some point As an observer... ... you want to compute these quantities easily and eciently ... you may want to develop the code for outputting new observables As a theorist... ... you may want to develop the code for incorporating new physics and compute/understand the e↵ects of your favourite model on observables As both... ... you want to infer constraints on cosmological parameters from a new dataset ... you want to test your own favorite model, given existing data ... you want to predict the sensitivity of a future experiment to a given parameter J. Lesgourgues Lecture I: Introduction

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