{"arxiv_id":"1607.04218","incoming":{"papers":20,"sentences":44,"groups":[{"kind":"method_or_tool","label":"Uses its method or tool","papers":9,"sentences":14,"quotes":[{"arxiv_id":"1703.08633","title":"Constraining Reionization with the $z \\sim 5-6$ Lyman-$\\alpha$ Forest Power Spectrum: the Outlook after Planck","url":"/paper/1703.08633","section":"Simulating Reionization Histories in Light of New Planck Constraints","sentence":"In order to simulate each reionization model discussed here we have used the methodology presented in [ref] , which allows us to vary the timing and duration of reionization, and its associated heat injection, enabling us to simulate a diverse range of reionization histories.","intent_p":1.0,"contests_p":null},{"arxiv_id":"1912.09397","title":"How to constrain warm dark matter with the Lyman $\\alpha$ forest","url":"/paper/1912.09397","section":"Introduction","sentence":"Therefore, in this work we suggest the following procedure for obtaining robust Lyman-$α$ forest bounds: [(1)] * In order to minimise the pressure effects, we run hydrodynamical simulations with model of ultraviolet background (UVB) LateCold from [ref] .[The details about the numerical simulations can be found in [ref] .] In this model the reionization starts at redshift $z=6.7$, later than other thermal histories, considered in [ref] or by other groups.","intent_p":0.81,"contests_p":null},{"arxiv_id":"2007.13751","title":"General framework for cosmological dark matter bounds using $N$-body simulations","url":"/paper/2007.13751","section":"Simulation input and output","sentence":"In order to vary the redshift dependence, we employ the reionization model of Ref. [ref] .","intent_p":0.98,"contests_p":null},{"arxiv_id":"2007.12705","title":"Strong bound on canonical ultra-light axion dark matter from the Lyman-alpha forest","url":"/paper/2007.12705","section":"Introduction","sentence":"We also vary the mid-point redshift of hydrogen reionization \\(z_rei ∈[6, 15]\\) and the total heat injection during reionization \\(T_rei ∈[1.5 ×10^4, 4 ×10^4] K\\) according to the model of Ref. [ref] .","intent_p":0.96,"contests_p":null},{"arxiv_id":"2111.10386","title":"New limits on light dark matter - proton cross section from the cosmic large-scale structure","url":"/paper/2111.10386","section":"Introduction","sentence":"In order to vary the thermal IGM parameters \\([T_0 (z), γ (z), u_0 (z)]\\) (see above), we vary the input ionization and heating rates by the model of Ref. [ref] .","intent_p":0.92,"contests_p":null}]},{"kind":"data_used","label":"Uses its data or values","papers":1,"sentences":1,"quotes":[{"arxiv_id":"1912.09397","title":"How to constrain warm dark matter with the Lyman $\\alpha$ forest","url":"/paper/1912.09397","section":"Introduction","sentence":"By construction it gives the minimal filaments size.[We thank J. Onorbe for sharing with us the data of the LateCold thermal history that were not published together with the other thermal histories in [ref] . hi photo-heating and photo-ionization rates are shown in Fig. [ref].] We have assumed that the intergalactic medium is optically thin, and that reionization happens uniformly in all the space. * We explicitly marginalise over the IGM temperature (Doppler broadening) adding their effects to the FPS in post-processing.","intent_p":0.87,"contests_p":null}]},{"kind":"supports_this_paper","label":"Cites it as support","papers":2,"sentences":2,"quotes":[{"arxiv_id":"1703.08633","title":"Constraining Reionization with the $z \\sim 5-6$ Lyman-$\\alpha$ Forest Power Spectrum: the Outlook after Planck","url":"/paper/1703.08633","section":"Conclusions","sentence":"This is because both the cooling and dynamical times in the rarefied IGM are long, comparable to the Hubble time and therefore memory of $$ reionization is retained [ref] .","intent_p":0.98,"contests_p":null},{"arxiv_id":"2004.02927","title":"Revised estimates of CMB $B$-mode polarization induced by patchy reionization","url":"/paper/2004.02927","section":"Reionization model calibrated to Lyman-Lg forest data","sentence":"Fortunately, the absence of coupling between the radiative transfer and the hydrodynamic response to reionization heating is unlikely to affect the calibration of the simulation to the forest data [ref] as the pressure smoothing scale at redshifts $z>5$ for our chosen UV background is less than $100h^-1 ckpc$ [ref] , approximately equal to the cell size of our grid (described below).","intent_p":0.97,"contests_p":null}]},{"kind":"background","label":"Cites it as background","papers":3,"sentences":3,"quotes":[{"arxiv_id":"1703.08633","title":"Constraining Reionization with the $z \\sim 5-6$ Lyman-$\\alpha$ Forest Power Spectrum: the Outlook after Planck","url":"/paper/1703.08633","section":"Introduction","sentence":"In an expanding universe with an evolving thermal state at a given epoch, this scale depends on the entire thermal history of IGM because fluctuations at earlier times expand or fail to collapse depending on the IGM temperature at that epoch [ref] .","intent_p":0.87,"contests_p":null},{"arxiv_id":"2402.03794","title":"Simulating the epoch of Helium Reionization in photon-conserving semi-numerical code SCRIPT","url":"/paper/2402.03794","section":"Introduction","sentence":"The UV background models are an important input to hydrodynamical simulations of structure formation to efficiently model the ionization and thermal state of the IGM [ref] .","intent_p":0.92,"contests_p":null},{"arxiv_id":"2306.05471","title":"PRIYA: A New Suite of Lyman-alpha Forest Simulations for Cosmology","url":"/paper/2306.05471","section":"Introduction","sentence":"Astrophysical applications include measuring the thermal history of the Universe [ref] , ionizing background models [ref] , the timing of reionization [ref] , and creating 3D maps of neutral hydrogen density [ref] .","intent_p":0.88,"contests_p":null}]}],"unlabelled_sentences":24},"outgoing":{"papers":10,"sentences":22,"groups":[{"kind":"contests","label":"Contests","papers":1,"sentences":1,"quotes":[{"arxiv_id":"1511.05992","title":"Models of the Thermal Evolution of the Intergalactic Medium After Reionization","url":"/paper/1511.05992","section":"Comparison to Previous Work","sentence":"Finally, we want to point out that both the [ref] and [ref] final conclusions on possible $$ reionization scenarios are based only on [ref] measurements at high redshift ($z>4$), ignoring the constraints on $T_0$ given by [ref] , which point to a much hotter IGM.","intent_p":0.97,"contests_p":0.78}]},{"kind":"data_used","label":"Uses data or values from","papers":2,"sentences":4,"quotes":[{"arxiv_id":"1605.02985","title":"Planck intermediate results. 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Cosmological parameters","url":"/paper/1502.01589","section":"Ionization and Thermal Histories of Common UVB Models","sentence":"The observational constraints on $$ coming from the CMB [ref] are indicated by a gray band[During the making of this paper, new constraints on reionization from Planck were published [ref] , moving these constraints to a lower value and reducing the errors: $=0.058±0.012$.","intent_p":0.9,"contests_p":null}]},{"kind":"background","label":"Cites as background","papers":5,"sentences":5,"quotes":[{"arxiv_id":"1511.00011","title":"Cosmic Dawn (CoDa): the First Radiation-Hydrodynamics Simulation of Reionization and Galaxy Formation in the Local Universe","url":"/paper/1511.00011","section":"Introduction","sentence":"Despite significant progress on this front [ref] these simulations are still too costly for sensible exploration of the parameter space.","intent_p":0.9,"contests_p":null},{"arxiv_id":"1604.01418","title":"MUFASA: Galaxy Formation Simulations With Meshless Hydrodynamics","url":"/paper/1604.01418","section":"Ionization and Thermal Histories of Common UVB Models","sentence":"These include simulations focusing on the properties of the IGM [ref] , but also simulations modeling galaxy formation and evolution [ref] .","intent_p":0.88,"contests_p":null},{"arxiv_id":"0810.5614","title":"Intergalactic dust and its photoelectric heating","url":"/paper/0810.5614","section":"Conclusions","sentence":"These models could include Population III stars [ref] , X-ray pre-heating coming from from starburst galaxies, supernova remnants, or miniquasars [ref] , dark matter annihilation or decay [ref] or cosmic rays [ref] , from the intergalactic absorption of blazar TeV photons [ref] , or from broadband intergalactic dust absorption [ref] .","intent_p":0.89,"contests_p":null},{"arxiv_id":"1604.02457","title":"The Darkest Hour Before Dawn: Contributions to Cosmic Reionization from Dark Matter Annihilation and Decay","url":"/paper/1604.02457","section":"Conclusions","sentence":"These models could include Population III stars [ref] , X-ray pre-heating coming from from starburst galaxies, supernova remnants, or miniquasars [ref] , dark matter annihilation or decay [ref] or cosmic rays [ref] , from the intergalactic absorption of blazar TeV photons [ref] , or from broadband intergalactic dust absorption [ref] .","intent_p":0.89,"contests_p":null},{"arxiv_id":"1502.01589","title":"Planck 2015 results. 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