RECORD
Changes in the halo formation rates due to features in the primordial spectrum
Cosmology and Nongalactic Astrophysics · Submitted 26 Oct 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim However, we find that the number density and the formation rates of halos change by about 13-22% for halo masses ranging over 10^4-10^14 solar mass, for potential parameters that lie within 2-sigma around the best fit values arrived at from the aforesaid joint constraints.
The compiled record
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
Open the compiled record
The abstract, sentence by sentence
Features in the primordial scalar power spectrum provide a possible roadway to describe the outliers at the low multipoles in the WMAP data. Apart from the CMB angular power spectrum, these features can also alter the matter power spectrum and, thereby, the formation of the large scale structure. Carrying out a complete numerical analysis, we investigate the effects of primordial features on the formation rates of the halos. We consider a few different inflationary models that lead to features in the scalar power spectrum and an improved fit to the CMB data, and analyze the corresponding imprints on the formation of halos. Performing a Markov Chain Monte Carlo analysis with the WMAP seven year data and the SDSS halo power spectrum from LRG DR7 for the models of our interest, we arrive at the parameter space of the models allowed by the data. We illustrate that, inflationary potentials, such as the quadratic potential with sinusoidal modulations and the axion monodromy model, which generate certain repeated, oscillatory features in the inflationary perturbation spectrum, do not induce a substantial difference in the number density of halos at their best fit values, when compared with, say, a nearly scale invariant spectrum as is generated by the standard quadratic potential. However, we find that the number density and the formation rates of halos change by about 13-22% for halo masses ranging over 10^4-10^14 solar mass, for potential parameters that lie within 2-sigma around the best fit values arrived at from the aforesaid joint constraints. We briefly discuss the implications of our results.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Features in the primordial scalar power spectrum provide a possible roadway to describe the outliers at the low multipoles in the WMAP data. | background 1.00 | 0.10 | 0.03 | hedged possibility 1.00 |
| s1 | Apart from the CMB angular power spectrum, these features can also alter the matter power spectrum and, thereby, the formation of the large scale structure. | background 0.98 | 0.09 | 0.03 | asserted 0.71 |
| s2 | Carrying out a complete numerical analysis, we investigate the effects of primordial features on the formation rates of the halos. | contribution 0.98 | 0.95 | 0.03 | asserted 0.78 |
| s3 | We consider a few different inflationary models that lead to features in the scalar power spectrum and an improved fit to the CMB data, and analyze the corresponding imprints on the formation of halos. | contribution 0.61 | 0.84 | 0.04 | asserted 0.75 |
| s4 | Performing a Markov Chain Monte Carlo analysis with the WMAP seven year data and the SDSS halo power spectrum from LRG DR7 for the models of our interest, we arrive at the parameter space of the models allowed by the data. | method 1.00 | 0.96 | 0.03 | asserted 1.00 |
| s5 | We illustrate that, inflationary potentials, such as the quadratic potential with sinusoidal modulations and the axion monodromy model, which generate certain repeated, oscillatory features in the inflationary perturbation spectrum, do not induce a substantial difference in the number density of halos at their best fit values, when compared with, say, a nearly scale invariant spectrum as is generated by the standard quadratic potential. | result 1.00 | 0.90 | 0.40 | asserted 1.00 |
| s6 | However, we find that the number density and the formation rates of halos change by about 13-22% for halo masses ranging over 10^4-10^14 solar mass, for potential parameters that lie within 2-sigma around the best fit values arrived at from the aforesaid joint constraints. | result 1.00 | 0.97 | 0.56 | asserted 1.00 |
| s7 | We briefly discuss the implications of our results. | interpretation 0.95 | 0.43 | 0.02 | unclear 0.99 |
What was examined, and what was not
- arXiv listing abstract v2
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
The paper
Original abstract
Features in the primordial scalar power spectrum provide a possible roadway to describe the outliers at the low multipoles in the WMAP data. Apart from the CMB angular power spectrum, these features can also alter the matter power spectrum and, thereby, the formation of the large scale structure. Carrying out a complete numerical analysis, we investigate the effects of primordial features on the formation rates of the halos. We consider a few different inflationary models that lead to features in the scalar power spectrum and an improved fit to the CMB data, and analyze the corresponding imprints on the formation of halos. Performing a Markov Chain Monte Carlo analysis with the WMAP seven year data and the SDSS halo power spectrum from LRG DR7 for the models of our interest, we arrive at the parameter space of the models allowed by the data. We illustrate that, inflationary potentials, such as the quadratic potential with sinusoidal modulations and the axion monodromy model, which generate certain repeated, oscillatory features in the inflationary perturbation spectrum, do not induce a substantial difference in the number density of halos at their best fit values, when compared with, say, a nearly scale invariant spectrum as is generated by the standard quadratic potential. However, we find that the number density and the formation rates of halos change by about 13-22% for halo masses ranging over 10^4-10^14 solar mass, for potential parameters that lie within 2-sigma around the best fit values arrived at from the aforesaid joint constraints. We briefly discuss the implications of our results.
Human review
References
How the literature uses it
14 arXiv papers cite this in 15 sentences
Papers citing it · 11 sentences without a confident label
Cites it as background 4 papers
-
The data have also been used widely to put constraints on different parametric forms of primordial spectrum, mostly motivated by inflation [ref] .
Primordial power spectrum: a complete analysis with the WMAP nine-year data · Introduction · 0.84
-
Additionally, different authors have carried out numerical analysis with the past CMB and LSS data sets [ref] and laid out forecasts for constraints with future observations [ref] .
Searching for Oscillations in the Primordial Power Spectrum with CMB and LSS Data · Introduction · 0.92
-
Prospects of observing these signals have been extensively studied using cosmic microwave background (CMB) [ref] , large-scale structure (LSS) [ref] and 21-cm hydrogen line experiments [ref] .
Probing Primordial Features with the Stochastic Gravitational Wave Background · Introduction · 0.81
What it cites · 6 sentences without a confident label
Uses the method or tool of 1 paper
-
Moreover, in the case of potentials with oscillations, which lead to fine features in the inflationary scalar power spectrum, we actually need to modify CAMB in order to ensure that the CMB angular power spectrum is evaluated at every multipole and compare them with the data [ref] .
Oscillations in the inflaton potential: Complete numerical treatment and comparison with the recent and forthcoming CMB datasets · Comparison with the WMAP and the SDSS data · 0.91
Compares with 1 paper
-
Moreover, it is obvious from Table [ref] that the axion monodromy model does not lead to the same extent of improvement in the fit as has been obtained before (in this context, see Refs. [ref] ).
Oscillations in the inflaton potential: Complete numerical treatment and comparison with the recent and forthcoming CMB datasets · Joint constraints from the WMAP and the SDSS data · 0.82
Cites as support 1 paper
-
Although the reconstruction efforts suggest that the features in the scalar power spectrum are typically localized over certain scales, it has been found that, oscillatory potentials which generate features on all scales also provide a much better fit to the CMB data than the nearly scale invariant power spectrum [ref] .
Oscillations in the inflaton potential: Complete numerical treatment and comparison with the recent and forthcoming CMB datasets · Introduction · 0.98
Cites as background 3 papers
-
Over the last few years, two types of oscillatory inflationary potentials have drawn a considerable amount attention [ref] .
Oscillations in the inflaton potential: Complete numerical treatment and comparison with the recent and forthcoming CMB datasets · Models of interest · 0.90
-
Over the last few years, two types of oscillatory inflationary potentials have drawn a considerable amount attention [ref] .
BINGO: A code for the efficient computation of the scalar bi-spectrum · Models of interest · 0.90
-
The perturbations originating from such a scalar field produces an almost scale independent power spectrum [ref] .
Inflation and the Theory of Cosmological Perturbations · Introduction · 0.83
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.