about
Impact of baryon physics on dark matter structures: a detailed simulation study of halo density profilesThe clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the Fourier space wedges of the final sampleDark matter halo concentrations in theWilkinson Microwave Anisotropy Probeyear 5 cosmologyErratum: Dark matter halo concentrations in the Wilkinson Microwave Anisotropy Probe year 5 cosmologyThe physics driving the cosmic star formation historyModelling neutral hydrogen in galaxies using cosmological hydrodynamical simulationsSupermassive black holes in the EAGLE Universe. Revealing the observables of their growthThe APOSTLE simulations: solutions to the Local Group's cosmic puzzlesMolecular hydrogen abundances of galaxies in the EAGLE simulationsThe alignment and shape of dark matter, stellar, and hot gas distributions in the EAGLE and cosmo-OWLS simulationsColours and luminosities ofz = 0.1 galaxies in the eagle simulationThe effect of baryons on the inner density profiles of rich clustersBaryon effects on the internal structure of ΛCDM haloes in the EAGLE simulationsThe EAGLE simulations of galaxy formation: calibration of subgrid physics and model variationsBent by baryons: the low-mass galaxy-halo relationThe EAGLE project: simulating the evolution and assembly of galaxies and their environmentsThe origin of discs and spheroids in simulated galaxiesnIFTy galaxy cluster simulations – IV. Quantifying the influence of baryons on halo propertiesnIFTy galaxy cluster simulations – I. Dark matter and non-radiative modelsThe clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the configuration-space clustering wedgesThe distribution of atomic hydrogen in eagle galaxies: morphologies, profiles, and H i holesThe eagle simulations of galaxy formation: the importance of the hydrodynamics schemeQuenching cluster cooling flows with recurrent hot plasma bubblesPhysical properties of simulated galaxy populations at z = 2 – I. Effect of metal-line cooling and feedback from star formation and AGNPhysical properties of simulated galaxy populations at z = 2 – II. Effects of cosmology, reionization and ISM physicsFeedback and the structure of simulated galaxies at redshift z= 2Galaxies���intergalactic medium interaction calculation ��� I. Galaxy formation as a function of large-scale environmentThe origin of extended disc galaxies atz= 2The drop in the cosmic star formation rate below redshift 2 is caused by a change in the mode of gas accretion and by active galactic nucleus feedbackThe rates and modes of gas accretion on to galaxies and their gaseous haloesThe impact of different physical processes on the statistics of Lyman-limit and damped Lyman α absorbersAbsorption signatures of warm-hot gas at low redshift: broad H i Lyα absorbersThrough thick and Thin--H I absorption in cosmological simulationsAbsorption signatures of warm-hot gas at low redshift: O viThe enrichment history of cosmic metalsMetal-line emission from the warm-hot intergalactic medium - II. UltravioletMetal-line emission from the warm-hot intergalactic medium - I. Soft X-raysChemical enrichment in cosmological, smoothed particle hydrodynamics simulationsThe Aurora radiation-hydrodynamical simulations of reionization: calibration and first resultsSpatially adaptive radiation-hydrodynamical simulations of galaxy formation during cosmological reionization
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Q55969474-851213C0-9027-45F7-AC40-81CF054E07A7Q56079014-70760F15-7888-48A0-884F-34D656AA0A3BQ56866015-E5271B0B-2E74-4138-9392-F46ABC67C675Q56866016-1EF98C16-B995-408A-81E0-82D943D49D70Q56866017-BFE46AFC-FD9C-41F9-8E5C-3C78C45F29CFQ56866018-3658BE7B-E900-4C99-9E55-0D063EFA633AQ56907566-3D8F2286-A54D-4EAE-9ADB-B08D01661179Q56907714-3E6F77DF-4AAA-4741-BC91-2801920885BCQ56907847-70DF0718-2E76-4BE6-B368-0462880E1C3FQ56907869-523EDBEC-7AD4-4E3B-9320-66FB28379EF6Q56907885-4B2B1F40-3A55-46EA-B36A-99C6E8F25358Q56907903-D8234694-8C0A-4520-B936-0C042342C160Q56907910-38EFB8B1-F568-4255-A9CF-920626A7E1F6Q56907928-B5863969-DE41-43D2-BDE9-323CCB1A2F41Q56907945-0ABE9082-683F-4223-B0FD-286D8676BE5FQ56908014-2E74A9AA-BB03-43CB-A07D-E00F2AC8BE74Q56908383-982F4213-D50F-4ECE-90A4-C0E944BCCA53Q57758338-BBF7817F-AC53-4F38-A014-C953469F8498Q57758344-DA3F3AC9-A355-4B51-B1EA-388700D7FB9BQ58262127-39182035-D134-4166-AAE5-ACF350A145EEQ58923203-CDBA6DE7-FCD5-45DB-BAB5-AEF60760EA87Q58923209-F224771D-6DBD-46EC-B50A-6904C230679CQ58923403-95B737FB-F7A3-4FBE-84A9-1C88AE470EE9Q59421327-E0EB1031-FF66-4A1F-BBC7-4F80192D8897Q59421328-71C9EB9D-7F19-449D-AC83-9B1C847659BCQ59421435-35CE866D-782E-4570-9DC6-640F0BE40986Q59421492-C6B23F35-1D88-455B-B628-F2A3343439F4Q59421500-9F53F15F-BDEA-4B43-95D0-54E8D3AC49A1Q59796692-C1CF3FB0-ED79-4E1A-BA2F-8A6FA1C2DF41Q59796696-EA0E25E4-C5B2-4C1D-B5F3-B356442D51C5Q60737951-5A431ED9-EBD4-4BF1-97A0-2539461E8D1CQ60737973-98A87D55-98C1-4212-8199-77A4DA57CDFAQ60737989-CCC59337-E368-4B8A-A691-F3126B358554Q60738000-36E7931B-68A5-4681-BB52-2FD372D964C1Q60738010-9B97D2FB-5CD2-4E98-B4F5-BDE8BD4A10F8Q60738014-433D7E21-FB54-42F9-9C49-6CD6E1F8C4A9Q60738017-1A05777A-4855-48DD-8CAE-86EE1AC7BB59Q60738029-F355D162-BED7-4C9D-B7F1-3A5AA140A3AAQ62779266-56AB815D-E12A-48F5-8E75-B6EF2A227AEAQ62779307-D1128EF3-D468-464F-A5AF-AB0D39683AD7
P50
description
onderzoeker
@nl
researcher
@en
հետազոտող
@hy
name
Claudio Dalla Vecchia
@ast
Claudio Dalla Vecchia
@en
Claudio Dalla Vecchia
@es
Claudio Dalla Vecchia
@nl
type
label
Claudio Dalla Vecchia
@ast
Claudio Dalla Vecchia
@en
Claudio Dalla Vecchia
@es
Claudio Dalla Vecchia
@nl
prefLabel
Claudio Dalla Vecchia
@ast
Claudio Dalla Vecchia
@en
Claudio Dalla Vecchia
@es
Claudio Dalla Vecchia
@nl
P106
P21
P31
P496
0000-0002-2620-7056