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new NcHIprimAtan object (primordial spectrum power law x atan). New m…
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…set_gen tool to generate .mset files. Added flag controling the tensor mode usage in NcHIPertBotlzmannCBE. New references (to the atan models).
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Sandro Dias Pinto Vitenti committed Oct 29, 2015
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1 change: 1 addition & 0 deletions docs/numcosmo-docs.sgml
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Expand Up @@ -166,6 +166,7 @@
<section>
<title>Inflationary</title>
<xi:include href="xml/nc_hiprim_power_law.xml"/>
<xi:include href="xml/nc_hiprim_atan.xml"/>
</section>
</chapter>

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104 changes: 82 additions & 22 deletions docs/references.bib
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Expand Up @@ -4037,6 +4037,24 @@ @Article{Coleman1991
Timestamp = {2011.06.12}
}

@Article{Colin2015,
Title = {{Robust predictions for the large-scale cosmological power deficit from primordial quantum nonequilibrium}},
Author = {{Colin}, S. and {Valentini}, A.},
Journal = {ArXiv e-prints},
Year = {2015},

Month = oct,
Abstract = {The de Broglie-Bohm pilot-wave formulation of quantum theory allows the existence of physical states that violate the Born probability rule. Recent work has shown that in pilot-wave field theory on expanding space relaxation to the Born rule is suppressed for long-wavelength field modes, resulting in a large-scale power deficit {\xi}(k) which for a radiation-dominated expansion is found to have a characteristic (approximate) inverse-tangent dependence on k. In this paper we show that the functional form of {\xi}(k) is robust under changes in the initial nonequilibrium distribution as well as under the addition of an inflationary era at the end of the radiation-dominated phase. In both cases the predicted deficit {\xi}(k) remains an inverse-tangent function of k. Furthermore, with the inflationary phase the dependence of the fitting parameters on the number of superposed pre-inflationary energy states is comparable to that found previously. Our results indicate that an inverse-tangent power deficit is likely to be a fairly general and robust signature of quantum relaxation in the early universe.},
Adsnote = {Provided by the SAO/NASA Astrophysics Data System},
Adsurl = {http://adsabs.harvard.edu/abs/2015arXiv151003508C},
Archiveprefix = {arXiv},
Eprint = {1510.03508},
Keywords = {General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Theory, Quantum Physics},
Owner = {sandro},
Primaryclass = {gr-qc},
Timestamp = {2015.10.29}
}

@Article{Collaboration2012,
Title = {Large Synoptic Survey Telescope: Dark Energy Science Collaboration},
Author = {LSST Dark Energy Science Collaboration},
Expand Down Expand Up @@ -7252,7 +7270,7 @@ @Article{Girardi1998
Timestamp = {2010.09.21}
}

@Misc{git,
@Misc{Git,
Title = {Version Control System},

Author = {Git},
Expand All @@ -7262,7 +7280,7 @@ @Misc{git
Url = {http://git-scm.com/}
}

@Misc{Git,
@Misc{git,
Title = {Version Control System},

Author = {Git},
Expand Down Expand Up @@ -11553,6 +11571,7 @@ @Article{Lesgourgues2011
Year = {2011},

Month = apr,

Abstract = {The Cosmic Linear Anisotropy Solving System (CLASS) is a new accurate Boltzmann code, designed to offer a more user-friendly and flexible coding environment to cosmologists. CLASS is very structured, easy to modify, and offers a rigorous way to control the accuracy of output quantities. It is also incidentally a bit faster than other codes. In this overview, we present the general principles of CLASS and its basic structure. We insist on the friendliness and flexibility aspects, while accuracy, physical approximations and performances are discussed in a series of companion papers.},
Adsnote = {Provided by the SAO/NASA Astrophysics Data System},
Adsurl = {http://adsabs.harvard.edu/abs/2011arXiv1104.2932L},
Expand All @@ -11571,8 +11590,6 @@ @Article{Lesgourgues2011a
Year = {2011},

Month = apr,

__markedentry = {[sandro:]},
Abstract = {By confronting the two independent Boltzmann codes CLASS and CAMB, we establish that for concordance cosmology and for a given recombination history, lensed CMB and matter power spectra can be computed by current codes with an accuracy of 0.01%. We list a few tiny changes in CAMB which are necessary in order to reach such a level. Using the common limit of the two codes as a set of reference spectra, we derive precision settings corresponding to fixed levels of error in the computation of a CMB likelihood. We find that for a given precision level, CLASS is about 2.5 times faster than CAMB for computing the lensed CMB spectra of a LambdaCDM model. The nature of the main improvements in CLASS (which may each contribute to these performances) is discussed in companion papers.},
Adsnote = {Provided by the SAO/NASA Astrophysics Data System},
Adsurl = {http://adsabs.harvard.edu/abs/2011arXiv1104.2934L},
Expand All @@ -11592,8 +11609,6 @@ @Article{Lesgourgues2011b
Month = sep,
Pages = {32},
Volume = {9},

__markedentry = {[sandro:]},
Abstract = {We present a new flexible, fast and accurate way to implement massive neutrinos, warm dark matter and any other non-cold dark matter relics in Boltzmann codes. For whatever analytical or numerical form of the phase-space distribution function, the optimal sampling in momentum space compatible with a given level of accuracy is automatically found by comparing quadrature methods. The perturbation integration is made even faster by switching to an approximate viscous fluid description inside the Hubble radius, which differs from previous approximations discussed in the literature. When adding one massive neutrino to the minimal cosmological model, CLASS becomes just 1.5 times slower, instead of about 5 times in other codes (for fixed accuracy requirements). We illustrate the flexibility of our approach by considering a few examples of standard or non-standard neutrinos, as well as warm dark matter models.},
Adsnote = {Provided by the SAO/NASA Astrophysics Data System},
Adsurl = {http://adsabs.harvard.edu/abs/2011JCAP...09..032L},
Expand Down Expand Up @@ -14670,6 +14685,7 @@ @Article{PlanckCollaboration2015a
Year = {2015},

Month = jul,

Abstract = {This paper presents the Planck 2015 likelihoods, statistical descriptions of the 2-point correlation functions of CMB temperature and polarization. They use the hybrid approach employed previously: pixel-based at low multipoles, $\ell$, and a Gaussian approximation to the distribution of cross-power spectra at higher $\ell$. The main improvements are the use of more and better processed data and of Planck polarization data, and more detailed foreground and instrumental models. More than doubling the data allows further checks and enhanced immunity to systematics. Progress in foreground modelling enables a larger sky fraction, contributing to enhanced precision. Improvements in processing and instrumental models further reduce uncertainties. Extensive tests establish robustness and accuracy, from temperature, from polarization, and from their combination, and show that the {\Lambda}CDM model continues to offer a very good fit. We further validate the likelihood against specific extensions to this baseline, such as the effective number of neutrino species. For this first detailed analysis of Planck polarization, we concentrate at high $\ell$ on E modes. At low $\ell$ we use temperature at all Planck frequencies along with a subset of polarization. These data take advantage of Planck's wide frequency range to improve the separation of CMB and foregrounds. Within the baseline cosmology this requires a reionization optical depth $\tau=0.078\pm0.019$, significantly lower than without high-frequency data for explicit dust monitoring. At high $\ell$ we detect residual errors in E, typically at the {\mu}K$^2$ level; we thus recommend temperature alone as the high-$\ell$ baseline. Nevertheless, Planck high-$\ell$ polarization spectra are already good enough to allow a separate high-accuracy determination of the {\Lambda}CDM parameters, consistent with those established from temperature alone.},
Adsnote = {Provided by the SAO/NASA Astrophysics Data System},
Adsurl = {http://adsabs.harvard.edu/abs/2015arXiv150702704P},
Expand Down Expand Up @@ -18035,6 +18051,31 @@ @Article{Twamley2006
Timestamp = {2011.07.18}
}

@Article{Underwood2015,
Title = {{Quantum field theory of relic nonequilibrium systems}},
Author = {{Underwood}, N.~G. and {Valentini}, A.},
Journal = {Phys. Rev. D},
Year = {2015},

Month = sep,
Number = {6},
Pages = {063531},
Volume = {92},

__markedentry = {[sandro:]},
Abstract = {In terms of the de Broglie-Bohm pilot-wave formulation of quantum theory, we develop field-theoretical models of quantum nonequilibrium systems which could exist today as relics from the very early Universe. We consider relic excited states generated by inflaton decay, as well as relic vacuum modes, for particle species that decoupled close to the Planck temperature. Simple estimates suggest that, at least in principle, quantum nonequilibrium could survive to the present day for some relic systems. The main focus of this paper is to describe the behavior of such systems in terms of field theory, with the aim of understanding how relic quantum nonequilibrium might manifest experimentally. We show by explicit calculation that simple perturbative couplings will transfer quantum nonequilibrium from one field to another (for example from the inflaton field to its decay products). We also show that fields in a state of quantum nonequilibrium will generate anomalous spectra for standard energy measurements. Possible connections to current astrophysical observations are briefly addressed.},
Adsnote = {Provided by the SAO/NASA Astrophysics Data System},
Adsurl = {http://adsabs.harvard.edu/abs/2015PhRvD..92f3531U},
Archiveprefix = {arXiv},
Doi = {10.1103/PhysRevD.92.063531},
Eid = {063531},
Eprint = {1409.6817},
Keywords = {Particle-theory and field-theory models of the early Universe},
Owner = {sandro},
Primaryclass = {hep-th},
Timestamp = {2015.10.29}
}

@Article{Uzan2007,
Title = {The acceleration of the universe and the physics behind it},
Author = {Uzan, J. P.},
Expand Down Expand Up @@ -18064,6 +18105,25 @@ @Article{Uzan1999
Timestamp = {2008.05.06}
}

@Article{Valentini2015,
Title = {{Statistical anisotropy and cosmological quantum relaxation}},
Author = {{Valentini}, A.},
Journal = {ArXiv e-prints},
Year = {2015},

Month = oct,

__markedentry = {[sandro:]},
Abstract = {We show that cosmological quantum relaxation predicts an anisotropic primordial power spectrum with a specific dependence on wavenumber k. We explore some of the consequences for precision measurements of the cosmic microwave background (CMB). Quantum relaxation is a feature of the de Broglie-Bohm pilot-wave formulation of quantum theory, which allows the existence of more general physical states that violate the Born probability rule. Recent work has shown that relaxation to the Born rule is suppressed for long-wavelength field modes on expanding space, resulting in a large-scale power deficit with a characteristic inverse-tangent dependence on k. Because the quantum relaxation dynamics is independent of the direction of the wave vector for the relaxing field mode, in the limit of weak anisotropy we are able to derive an expression for the anisotropic power spectrum that is determined by the power deficit function. As a result, the off-diagonal terms in the CMB covariance matrix are also determined by the power deficit. We show that the lowest-order l-(l+1) inter-multipole correlations have a characteristic scaling with multipole moment l. Our derived spectrum also predicts a residual statistical anisotropy at small scales, with an approximate consistency relation between the scaling of the l-(l+1) correlations and the scaling of the angular power spectrum at high l. We also predict a relationship between the l-(l+1) correlations at large and small scales. Cosmological quantum relaxation appears to provide a single physical mechanism that predicts both a large-scale power deficit and a range of statistical anisotropies, together with potentially testable relationships between them.},
Adsnote = {Provided by the SAO/NASA Astrophysics Data System},
Adsurl = {http://adsabs.harvard.edu/abs/2015arXiv151002523V},
Archiveprefix = {arXiv},
Eprint = {1510.02523},
Keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Theory, Quantum Physics},
Owner = {sandro},
Timestamp = {2015.10.29}
}

@Article{Valentini2010,
Title = {Inflationary cosmology as a probe of primordial quantum mechanics},
Author = {Valentini, Antony},
Expand Down Expand Up @@ -19305,15 +19365,15 @@ @Misc{GPL3
Url = {http://www.gnu.org/licenses/gpl-3.0.html}
}

@Misc{GtkDoc,
@Misc{GTKDOC,
Title = {GTK-Doc},

Owner = {sandro},
Timestamp = {2011.09.29},
Url = {http://www.gtk.org/gtk-doc/}
}

@Misc{GTKDOC,
@Misc{GtkDoc,
Title = {GTK-Doc},

Owner = {sandro},
Expand Down Expand Up @@ -19346,19 +19406,17 @@ @Misc{
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@Misc{,
Title = {GNU General Public License, Version 2},

Owner = {sandro},
Timestamp = {2011.09.16},
Url = {http://www.gnu.org/licenses/gpl-2.0.html}
Owner = {mariana},
Timestamp = {2013.12.16},
Url = {http://www.r-project.org/}
}

@Misc{,
Title = {GNU General Public License, Version 3},
Title = {Lambda -- NASA},

Owner = {sandro},
Timestamp = {2011.09.16},
Url = {http://www.gnu.org/licenses/gpl-3.0.html}
Timestamp = {2013.06.05},
Url = {http://lambda.gsfc.nasa.gov/toolbox/tb_camb_form.cfm}
}

@Misc{,
Expand All @@ -19370,17 +19428,19 @@ @Misc{
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@Misc{,
Title = {Lambda -- NASA},
Title = {GNU General Public License, Version 3},

Owner = {sandro},
Timestamp = {2013.06.05},
Url = {http://lambda.gsfc.nasa.gov/toolbox/tb_camb_form.cfm}
Timestamp = {2011.09.16},
Url = {http://www.gnu.org/licenses/gpl-3.0.html}
}

@Misc{,
Owner = {mariana},
Timestamp = {2013.12.16},
Url = {http://www.r-project.org/}
Title = {GNU General Public License, Version 2},

Owner = {sandro},
Timestamp = {2011.09.16},
Url = {http://www.gnu.org/licenses/gpl-2.0.html}
}

@Misc{,
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5 changes: 5 additions & 0 deletions docs/references.tex
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Expand Up @@ -48,6 +48,11 @@
\nocite{Delubac2015}
\nocite{PlanckCollaboration2015a}

%Antony's papers
\nocite{Valentini2010}
\nocite{Colin2015}
\nocite{Underwood2015}
\nocite{Valentini2015}

\bibliography{references}
\bibliographystyle{apsrev}
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4 changes: 3 additions & 1 deletion numcosmo/Makefile.am
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Expand Up @@ -240,6 +240,7 @@ nc_headers = \
model/nc_hicosmo_qspline.h \
model/nc_hicosmo_qgrw.h \
model/nc_hiprim_power_law.h \
model/nc_hiprim_atan.h \
lss/nc_window.h \
lss/nc_window_tophat.h \
lss/nc_window_gaussian.h \
Expand Down Expand Up @@ -346,7 +347,8 @@ nc_sources = \
model/nc_hicosmo_qlinear.c \
model/nc_hicosmo_qspline.c \
model/nc_hicosmo_qgrw.c \
model/nc_hiprim_power_law.c \
model/nc_hiprim_power_law.c \
model/nc_hiprim_atan.c \
lss/nc_window.c \
lss/nc_window_tophat.c \
lss/nc_window_gaussian.c \
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2 changes: 2 additions & 0 deletions numcosmo/math/ncm_cfg.c
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Expand Up @@ -62,6 +62,7 @@
#include "model/nc_hicosmo_qgrw.h"
#include "model/nc_hicosmo_de_reparam_ok.h"
#include "model/nc_hiprim_power_law.h"
#include "model/nc_hiprim_atan.h"
#include "lss/nc_window_tophat.h"
#include "lss/nc_window_gaussian.h"
#include "lss/nc_growth_func.h"
Expand Down Expand Up @@ -288,6 +289,7 @@ ncm_cfg_init (void)
ncm_cfg_register_obj (NC_TYPE_HICOSMO_DE_REPARAM_OK);

ncm_cfg_register_obj (NC_TYPE_HIPRIM_POWER_LAW);
ncm_cfg_register_obj (NC_TYPE_HIPRIM_ATAN);

ncm_cfg_register_obj (NC_TYPE_CBE_PRECISION);

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