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Cosmic expansion in homogeneous and inhomogeneous universes [Elektronische Ressource] : supernovae type Ia as cosmic probes / Marina Seikel

106 pages
Publié par :
Ajouté le : 01 janvier 2010
Lecture(s) : 26
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Doctoral thesis in theoretical physics
Cosmic expansion in homogeneous and inhomogeneous
Supernovae type Ia as cosmic probes
Marina Seikel
Theoretical High Energy Physics Group
Fakult at fur Physik
Universit at BielefeldCover Picture:
SN 1994D in the galaxy NGC 4526
Source: Hubble Space Telescope (NASA/ESA)Cosmic expansion in homogeneous and inhomogeneous
Supernovae type Ia as cosmic probes
Marina Seikel
September 13, 2010
Supervisor: Prof. Dr. Dominik J. Schwarz
Referees: Prof. Dr. Nicolas Borghini
Prof. Dr. Dietrich B odeker
Prof. Dr. B arbel Frommev
Abstract. Since it has been discovered in the late 1990s that the universe is
likely to be expanding accelerated, a large variety of cosmological models have
been developed that allow for cosmic acceleration. Some of the models include a
dark energy term that causes the acceleration, while others modify gravity or drop
the assumption of homogeneity and isotropy.
As an example of such a model, we analyze a braneworld model with one
timelike extra-dimension. There are strong constraints to the parameter values of
such a model resulting from the claim that there must be a physical solution to the
Friedmann equation at least between now and the time of recombination. We t
the model to supernova type Ia data and check the consistency of the result with
other observations. For parameter values that are consistent with observations,
the braneworld model is indistinguishable from a CDM universe as far as the
considered cosmological tests are concerned.
Although all cosmological models that assume homogeneity and isotropy of the
universe and have been tested so far conclude that the universe expands acceler-
ated, this does not prove acceleration beyond doubt. Therefore, we constructed a
test of acceleration, which is model-independent in the sense that no assumptions
about the content of the universe or about the parameterization of the deceler-
ation parameter are made and that it does not assume any dynamical equations
of motion. Yet, the test assumes the universe and the distribution of supernovae
to be statistically homogeneous and isotropic. Since the rst version of the test
is troubled by systematic e ects, we modify the analysis to be independent of the
calibration of the supernova absolute magnitude. As a result, all systematics are
reduced. While most supernova data sets provide evidence for acceleration, when
the test is applied, the SDSS data set lacks this evidence.
Due to structure in the universe, the assumption of homogeneity and isotropy
might not be justi ed | especially on small scales. As the Einstein equations
are non-linear, spatial averaging and temporal evolution do not commute. Conse-
quently, a universe with structure evolves di erently than a perfectly homogeneous
universe. The size of this backreaction e ect is, however, discussed very controver-
sially. In this work, we test the in uence of backreaction on the measurement of
the present Hubble rate using supernova data. We nd, however, no evidence for
backreaction in the presently available supernova data sets.Contents
List of Figures ix
List of Tables xi
Preface xiii
Chapter 1. Cosmic expansion and supernovae type Ia 1
1. Cosmic expansion 1
1.1. Dynamics of the expanding universe 1
1.2. Distance measures 3
1.3. Models of dark energy 4
2. Supernovae type Ia 8
2.1. Types of supernovae 8
2.2. SNe Ia as standard candles 8
2.3. Observation of supernovae 10
Chapter 2. Braneworlds with a timelike extra-dimension 15
1. The idea of extra-dimensions 15
1.1. Compact 15
1.2. Randall-Sundrum model 16
2. A braneworld model 16
3. Timelike extra-dimension 19
3.1. General equations 19
3.2. Flat universe without dark radiation 20
4. Test of the BRANE1 model 23
4.1. Fit to supernova type Ia data 23
4.2. Angular separation 24
4.3. Other observations 25
4.4. Conclusion 27
Chapter 3. Model-independent tests of accelerated expansion 29
1. Kinematical approach 29
2. Model-independent test 30
2.1. Assumptions 30
2.2. Previous model-independent tests 30
2.3. Method 31
2.4. Data sets 32
2.5. Results for a at universe 35
2.6. for open and closed universes 40
2.7. Systematics 42
viiviii CONTENTS
3. Model- and calibration-independent test 43
3.1. Modifying the method 43
3.2. Results for the Gold, ESSENCE and Union data sets 43
3.3. for the Constitution and SDSS data sets 48
3.4. Conclusion 51
Chapter 4. Probing backreaction e ects with supernova data 53
1. Backreaction 53
1.1. Local structure 53
1.2. Averaging problem 54
2. Av formalism 56
2.1. Basic considerations 56
2.2. General averaging equations 57
2.3. E ective Friedmann equations 58
2.4. Cosmological perturbation theory 59
2.5. Fluctuation of the Hubble rate 59
3. Probing backreaction e ects 61
3.1. Supernova data 61
3.2. Calibration 63
3.3. Results for the tophat window function 63
3.4. for the Gaussian window 65
3.5. Conclusion 67
Chapter 5. Concluding remarks 69
Appendix A. Notation 71
Appendix B. Physical quantities 75
Appendix C. Abbreviations 77
Appendix D. Supernova data sets 79
Appendix E. Theoretical constraints of the braneworld model 81
1. BRANE1 81
1.1. Negative brane tension 81
1.2. Positive brane 83
2. BRANE2 83
2.1. Positive brane tension 83
2.2. Negative brane 85
Bibliography 87List of Figures
1.1 Di erent distance measures in a at CDM universe. 4
1.2 68:3%, 95:4% and 99:7% con dence regions in the ( ;
) plane assuming a CDMm
+model. Figure taken from [A 10]. 5
1.3 68:3%, 95:4% and 99:7% con dence regions in the ( ;w) plane. Figure taken fromm
+[A 10]. 6
+1.4 Spectra of SNe Ia at di erent redshifts. Figure taken from [ R 98]. 9
1.5 Hubble diagram for the SNe published by Riess et al. (1998). Also shown are three
cosmological models. In the bottom panel, the distance modulus from the model with
= 0:20 and
= 0:00 is subtracted from the data. Figure taken from [R 98]. 11m
1.6 Top panel: Light-curves of low redshift SNe from the Calan-Tololo survey, showing
an intrinsic dispersion of 0:3 mag in peak absolute magnitude. Bottom panel:
Light-curves after correction according to the Phillips relation. 12
2.1 Constraints on the density parameters
of a BRANE1 model with matter‘ 5
= 0:3. 21m
2.2 Distance modulus minus the distance modulus of an empty universe for the three
braneworld model ts and CDM. 25
2.3 Angular separation for the three braneworld model ts and CDM. 26
2.4 Ages of stars from Th abundances. Figure taken from [JB01]. 27
3.1 for di erent cosmological models. (a) shows the following models assuming a
at universe: CDM ( = 0:28), de Sitter (i.e.
= 1) and models with constantm
deceleration parameter q = 0:5 and q = 0:5. (b) shows a universe with
= 0:3m
and di erent values of
is determined by
= 1

. 33k m k
3.2 Di erences in the apparent magnitudes in the ESSENCE set obtained by the SALT
and the MLCS2k2 light-curve