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J/ApJ/837/106 UV background photoionization & photoheating rates (Onorbe+, 2017)

Self-consistent modeling of reionization in cosmological hydrodynamical simulations. Onorbe J., Hennawi J.F., Lukic Z. <Astrophys. J., 837, 106-106 (2017)> =2017ApJ...837..106O (SIMBAD/NED BibCode)
ADC_Keywords: Models ; Ultraviolet ; Redshifts Keywords: early universe; galaxies: evolution; galaxies: formation; intergalactic medium; large-scale structure of universe; methods: numerical Abstract: The ultraviolet background (UVB) emitted by quasars and galaxies governs the ionization and thermal state of the intergalactic medium (IGM), regulates the formation of high-redshift galaxies, and is thus a key quantity for modeling cosmic reionization. The vast majority of cosmological hydrodynamical simulations implement the UVB via a set of spatially uniform photoionization and photoheating rates derived from UVB synthesis models. We show that simulations using canonical UVB rates reionize and, perhaps more importantly, spuriously heat the IGM, much earlier (z∼15) than they should. This problem arises because at z>6, where observational constraints are nonexistent, the UVB amplitude is far too high. We introduce a new methodology to remedy this issue, and we generate self-consistent photoionization and photoheating rates to model any chosen reionization history. Following this approach, we run a suite of hydrodynamical simulations of different reionization scenarios and explore the impact of the timing of reionization and its concomitant heat injection on the thermal state of the IGM. We present a comprehensive study of the pressure smoothing scale of IGM gas, illustrating its dependence on the details of both hydrogen and helium reionization, and argue that it plays a fundamental role in interpreting Lyα forest statistics and the thermal evolution of the IGM. The premature IGM heating we have uncovered implies that previous work has likely dramatically overestimated the impact of photoionization feedback on galaxy formation, which sets the minimum halo mass able to form stars at high redshifts. We make our new UVB photoionization and photoheating rates publicly available for use in future simulations. Description: In this paper we have presented results from optically thin cosmological hydrodynamical simulations using the Nyx code (Almgren+ 2013ApJ...765...39A ; Lukic+ 2015MNRAS.446.3697L). As commonly done in multiple intergalactic medium (IGM) and galaxy formation studies, the UV background is modeled as a uniform and isotropic field that evolves with redshift. Operationally, the ultraviolet background (UVB) determines the photoionization and photoheating rates of HI, HeI, and HeII, which are inputs to the code. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 86 301 Tabulated UV background for late HI reionization (zreion,HI=6.55), ΔTHI=2e4K; HeA reionization, ΔTHeII=1.5e4K table4.dat 86 301 Tabulated UV background for middle HI reionization (zreion,HI=8.30), ΔTHI=2e4 K; HeA reionization, ΔTHeII=1.5e4K table5.dat 86 301 Tabulated UV background for early HI reionization (zreion,HI=9.70), ΔTHI=2e4K; HeA reionization, ΔTHeII=1.5e4K
See also: J/A+A/318/347 : Absorption lines in QSO 0000-2619 (Savaglio+, 1997) J/AJ/131/1 : Binary quasars in the SDSS (Hennawi+, 2006) J/ApJ/662/72 : Lyman alpha forest of 55 QSOs (Becker+, 2007) J/ApJS/168/213 : Ionization states and cooling efficiencies (Gnat+, 2007) J/ApJ/719/1672 : SDSS binary quasars at high redshift. I. (Hennawi+, 2010) J/MNRAS/404/1295 : Impact of gas pressure on transverse structure (Peeples+, 2010) J/ApJ/775/78 : Lyman limit absorption systems in z∼3 QSOs (Fumagalli+, 2013) J/ApJ/765/137 : HST survey for Lyman limit systems. II. (O'Meara+, 2013) J/A+A/559/A85 : 1D Lya forest power spectrum (Palanque-Delabrouille+, 2013) J/ApJ/814/40 : Nearby galaxy filaments with UV obs. (Wakker+, 2015) J/AJ/150/111 : KODIAQ DR1 (O'Meara+, 2015) Byte-by-byte Description of file: table[345].dat
Bytes Format Units Label Explanations
1- 8 F8.6 [-] log(z+1) [0/1.21] Log redshift plus one 10- 21 E12.6 s-1 GammaHI [0/1.3e-12] H I photoionization rate 23- 34 E12.6 s-1 GammaHeI [0/7.3e-13] He I photoionization rate 36- 47 E12.6 s-1 GammaHeII [0/4.4e-15] He II photoionization rate 49- 60 E12.6 10-7W qdotHI [0/7.8e-24] H I photoheating rate; erg/s 62- 73 E12.6 10-7W qdotHeI [0/9.5e-24] He I photoheating rate; erg/s 75- 86 E12.6 10-7W qdotHeII [0/1.5e-25] He II photoheating rate; erg/s
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 19-Oct-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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