{"arxiv_id":"2312.03810","incoming":{"papers":1,"sentences":1,"groups":[],"unlabelled_sentences":1},"outgoing":{"papers":63,"sentences":112,"groups":[{"kind":"method_or_tool","label":"Uses the method or tool of","papers":2,"sentences":2,"quotes":[{"arxiv_id":"astro-ph/0205436","title":"Cosmological parameters from CMB and other data: a Monte-Carlo approach","url":"/paper/astro-ph/0205436","section":"Observational Constraints","sentence":"Afterwards, the modifications were incorporated to the cosmomc [ref] (which was adapted to include the new parameter of interest) an then analyzed with getdist codes Original code can be obtained at https://github.com/cmbant/CosmoMChttps://github.com/cmbant/CosmoMC..","intent_p":1.0,"contests_p":null},{"arxiv_id":"astro-ph/9911177","title":"Efficient Computation of CMB anisotropies in closed FRW models","url":"/paper/astro-ph/9911177","section":"Observational Constraints","sentence":"We proceeded to modify the camb [ref] source code Original code is available at https://github.com/cmbant/CAMBhttps://github.com/cmbant/CAMB. to include our calculations in the primordial power spectrum.","intent_p":1.0,"contests_p":null}]},{"kind":"data_used","label":"Uses data or values from","papers":5,"sentences":10,"quotes":[{"arxiv_id":"1907.1287","title":null,"url":"/paper/1907.1287","section":"Observational Constraints","sentence":"Observational data used corresponds to the latest [ref] data consisting in Planck temperature and polarization correlations likelihood plikTT,TE,EE+lowE+lensing Code available at https://pla.esac.esa.inthttps://pla.esac.esa.int..","intent_p":1.0,"contests_p":null},{"arxiv_id":"1807.0621","title":null,"url":"/paper/1807.0621","section":"Introduction","sentence":"Recent data have narrowed the value of the scalar spectral index $|n_s - 1 | ≃10^-2$ [ref] .","intent_p":0.97,"contests_p":null},{"arxiv_id":"1502.0211","title":null,"url":"/paper/1502.0211","section":"Introduction","sentence":"As observed in [ref] , the parameter $n_run$ is consistent with a value of zero, but it is not centered precisely at zero.","intent_p":0.89,"contests_p":null},{"arxiv_id":"2212.0411","title":null,"url":"/paper/2212.0411","section":"Introduction","sentence":"There exists a range of values that are equally probable such that $|n_run| ≲10^-3$ [ref] , and the possibility of a non-zero value must be taken into account in future experiments [ref] .","intent_p":0.85,"contests_p":null},{"arxiv_id":"1807.0620","title":null,"url":"/paper/1807.0620","section":"Primordial Power Spectrum","sentence":"Substituting these numerical values of $ρ_$ and $N_$ in Eq. [ref], and taking into account that the most recent data [ref] suggest $T_0 ≃2.4 ×10^-13$ GeV, we ultimately obtain the value $|τ| = 8 ×10^6$ Mpc by making the appropriate units conversions; also we can check that $λ_0 |τ| >1$.","intent_p":1.0,"contests_p":null}]},{"kind":"supports_this_paper","label":"Cites as support","papers":1,"sentences":1,"quotes":[{"arxiv_id":"1211.3463","title":"CSL Wave Function Collapse Model as a Mechanism for the Emergence of Cosmological Asymmetries in Inflation","url":"/paper/1211.3463","section":"Parameterization of $λ_k$","sentence":"In Ref. [ref] , it was demonstrated that the simplest functional dependence $λ_k =λ_0 k$ can indeed be interpreted as a specific form of the collapse operator.","intent_p":0.97,"contests_p":null}]},{"kind":"background","label":"Cites as background","papers":30,"sentences":33,"quotes":[{"arxiv_id":"2006.0309","title":null,"url":"/paper/2006.0309","section":"The CSL inflationary model","sentence":"The purpose of this section is to provide a brief overview of the calculations developed in [ref] .","intent_p":0.89,"contests_p":null},{"arxiv_id":"hep-ph/0403129","title":"Primordial fluctuations and cosmological inflation after WMAP 1.0","url":"/paper/hep-ph/0403129","section":"Slow roll model","sentence":"These parameters can be defined in terms of the Hubble parameter $H ≡ȧ/a$ (where the dot denotes the derivative with respect to cosmic time $t$) to yield what we refer to as the Hubble flow functions (HFF) [ref] : [equation] where $N ≡ln(a/a_ini)$ is the number of e-folds from the beginning of inflation.","intent_p":0.83,"contests_p":null},{"arxiv_id":"astro-ph/0106020","title":"Higher order corrections to primordial spectra from cosmological inflation","url":"/paper/astro-ph/0106020","section":"Slow roll model","sentence":"These parameters can be defined in terms of the Hubble parameter $H ≡ȧ/a$ (where the dot denotes the derivative with respect to cosmic time $t$) to yield what we refer to as the Hubble flow functions (HFF) [ref] : [equation] where $N ≡ln(a/a_ini)$ is the number of e-folds from the beginning of inflation.","intent_p":0.83,"contests_p":null},{"arxiv_id":"1207.2086","title":"Cosmological Inflation and the Quantum Measurement Problem","url":"/paper/1207.2086","section":"Introduction","sentence":"This debate is not new, and a large amount of literature has been dedicated to these concerns [ref] .","intent_p":0.98,"contests_p":null},{"arxiv_id":"gr-qc/9504030","title":"Semiclassicality and Decoherence of Cosmological Perturbations","url":"/paper/gr-qc/9504030","section":"Introduction","sentence":"This debate is not new, and a large amount of literature has been dedicated to these concerns [ref] .","intent_p":0.98,"contests_p":null}]}],"unlabelled_sentences":66},"claims":[],"thresholds":{"intent_p":0.8,"supports_p":0.95,"contests_p":0.7},"method":"Citing sentences come from each paper's LaTeX source; every \\cite marks the sentence and the works it cites. Pith's classifier typed each sentence. A label is shown at intent probability 0.8 or more (0.95 for support), a contest at 0.7 or more. Measured accuracy against two blind model families is at https://pith.science/accuracy. The quoted sentences are the citing authors' own.","held_up":null,"_links":{"html":"https://pith.science/paper/2312.03810"}}