{"arxiv_id":"1106.0538","incoming":{"papers":47,"sentences":79,"groups":[{"kind":"method_or_tool","label":"Uses its method or tool","papers":1,"sentences":1,"quotes":[{"arxiv_id":"1301.3143","title":"Angular Momentum Acquisition in Galaxy Halos","url":"/paper/1301.3143","section":"Angular Momentum Acquisition","sentence":"Instead of choosing matter with recent infall times, we instead compute a velocity-weighted average for $j$ for all particles in the inner halo ($0.5 < R/< 1.0$) that posses in-flowing radial velocities with respect to the halo center: [equation] similar to the definition of “accretion-weighted” angular momentum performed by [ref] .","intent_p":0.98,"contests_p":null}]},{"kind":"data_used","label":"Uses its data or values","papers":2,"sentences":3,"quotes":[{"arxiv_id":"1211.3124","title":"Angular momentum transfer to a Milky Way disk at high redshift","url":"/paper/1211.3124","section":"High redshift contributions to the present day mass and angular momentum of the disk from the run","sentence":"Multiplying the modulus of the total baryonic specific angular momentum contributions within the $0.1r_vir$ region at $z=0$ from the [ref] study by the relevant component masses yields an estimate of the total baryonic angular momentum signal: $J_b(z=0)∼4.4×10^13 M_ kpc km s^-1$.","intent_p":0.94,"contests_p":null},{"arxiv_id":"1602.06983","title":"Simulated stellar kinematics studies of high-redshift galaxies with the HARMONI Integral Field Spectrograph","url":"/paper/1602.06983","section":"The simulation","sentence":"The data were extracted from the simulations, described in detail by [ref] . is a suite of high resolution cosmological simulations of a Milky Way-like galaxy forming at the intersection of three filaments in a $Λ$CDM cosmology.","intent_p":0.85,"contests_p":null}]},{"kind":"comparison","label":"Compares with it","papers":2,"sentences":4,"quotes":[{"arxiv_id":"1407.7129","title":"Four phases of angular-momentum buildup in high-z galaxies: from cosmic-web streams through an extended ring to disc and bulge","url":"/paper/1407.7129","section":"Cold gas outside the halo","sentence":"A similar phenomenon has been detected in other simulations [ref] .","intent_p":0.8,"contests_p":null},{"arxiv_id":"1405.0552","title":"Escape fraction of ionizing photons during reionization: effects due to supernova feedback and runaway OB stars","url":"/paper/1405.0552","section":"Feedback-regulated Escape of Ionizing Photons","sentence":"Although the direct comparison may be difficult due to a different initial condition used, it is worth noting that the conversion efficiency is about a factor of 7 smaller than that found in the NutFB run [ref] , shown as a star in Figure [ref].","intent_p":0.97,"contests_p":null}]},{"kind":"supports_this_paper","label":"Cites it as support","papers":2,"sentences":2,"quotes":[{"arxiv_id":"1612.00513","title":"Gas Accretion and Angular Momentum","url":"/paper/1612.00513","section":"Introduction","sentence":"In particular—as it relates to this chapter—under this developing paradigm of filamentary versus isotropic gas accretion, halo gas (and particularly gas accreted in the cold mode) tends to show considerably higher specific angular momentum than the dark matter in the halo [ref] .","intent_p":0.97,"contests_p":null},{"arxiv_id":"1301.3143","title":"Angular Momentum Acquisition in Galaxy Halos","url":"/paper/1301.3143","section":"Conclusion","sentence":"Motivated by recent findings that the specific angular momentum of gaseous halos are considerably higher than that of the dark matter halo [ref] we focus on how reservoirs of cold-mode gas in galaxy halos grow and evolve over time, and how the angular momentum of this material differs from the canonical scenario for angular momentum growth in galaxies.","intent_p":0.99,"contests_p":null}]},{"kind":"background","label":"Cites it as 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Now","url":"/paper/1207.7072","section":"Introduction","sentence":"Only recently have hydrodynamic simulations of galaxy formation been run with enough resolution to study this in detail for up to a few tens of galaxies [ref] .","intent_p":0.87,"contests_p":null},{"arxiv_id":"2306.03966","title":"The Structure and Dynamics of Massive High-$z$ Cosmic-Web Filaments: Three Radial Zones in Filament Cross-Sections","url":"/paper/2306.03966","section":"Introduction","sentence":"These include halo spin, galaxy angular momentum growth and disk formation [ref] , the shape and alignment of galaxies and haloes [ref] , driving and sustaining turbulence and disk instabilities [ref] , and the emission and absorption signatures of the CGM [ref] .","intent_p":0.91,"contests_p":null}]}],"unlabelled_sentences":65},"outgoing":{"papers":0,"sentences":0,"groups":[],"unlabelled_sentences":0},"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/1106.0538"}}