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input.MR
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%------------------------------------------
%----- SA model inputs --------------
%------------------------------------------
FileNameGalaxies SA
FirstFile 5
LastFile 5
FileWithOutputRedshifts ./input/desired_output_redshifts.txt
McFile ./input/Mc.txt
CoolFunctionsDir ../../Development_Branch/CoolFunctions/
SpecPhotDir ../../Development_Branch/SpecPhotTables/
PhotPrefix PLANCK_M05 ; WMAP7_BC03 ;WMAP7_CB07
SpecPhotIMF Chabrier ; Salpeter ; Kroupa
FileWithFilterNames ./input/Filter_Names.txt
%-------------------------------------------------
%----- Simulation input/output files ------------
%-------------------------------------------------
SimulationDir /lustre/scratch/astro/virgo/Trees/MR
LastDarkMatterSnapShot 63
Hashbits 8 ;needed for Peano hilbert key output with the GALAXYTREE option
OutputDir /lustre/scratch/astro/ap629/test_rmol/no_GG/MR/
MaxMemSize 3000 ; 70000 ; 100000 galtree
%-------------------------------------------------
%----- Scaling options ------------
%-------------------------------------------------
ScalePos 0.960558
ScaleMass 1.11671
------------------------------------------
%----- Cosmological paramters ------------
%------------------------------------------
%NEW COSMOLOGY: PLANCK1
BaryonFrac 0.155
Sigma8 0.826
FileWithZList ./input/zlists/zlist_planck_MR.txt
PartMass 0.0961104 ;should be changed according to the dark matter simulation being used ;new
BoxSize 480.279
Omega 0.315
OmegaLambda 0.685
Hubble_h 0.673
%ORIGINAL COSMOLOGY: WMAP1
FileWithZList_OriginalCosm ./input/zlists/zlist_MR.txt
PartMass_OriginalCosm 0.0860657 ;should be changed according to the dark matter simulation being used
BoxSize_OriginalCosm 500.
Omega_OriginalCosm 0.25
OmegaLambda_OriginalCosm 0.75
Hubble_h_OriginalCosm 0.73
%----------------------------------------------------
%----- Switches for different physical models -------
%----------------------------------------------------
ReionizationModel 0 ;
%*0 -- Okamoto 2008 (Guo2010),
% 1 -- Gnedin reionization (Delucia2007),
% 2 -- no reionization
DiskRadiusModel 0 ;method to calculate disk radius
%*0 -- use each component (stellar or gas) spin to get disk radius,
% 1 -- use halo spin parameter to get disk scale radius,
% 2 -- disk_radius = Gal[p].Rvir / 10.0
StarFormationModel 0 ;
%*0 -- Croton2006, Delucia2007, Guo2011
% 1 -- Alternative SF law
FeedbackReheatingModel 0 ;
%*0 -- Guo 2010 (reheating scheme used in delucia 2007, plus Vmax dependence)
% 1 -- Alternative reheating model
FeedbackEjectionModel 0 ;
%*0 -- Guo 2010 (ejection scheme used in delucia 2007, plus Vmax dependence)
% 1 -- Constant velocity model
FateOfSatellitesGas 0 ;choice of ejection of satellite galaxies.
%*0 -- ejected gas of satellites distribute between type 1 and type 0,
% according to the fraction of dark matter retained in subhalos (Guo2010).
% 1 -- ejected gas of satellite galaxies contributes to
% the ejected component of type 0 (Delucia2007);
ReIncorporationModel 0 ;reincorporation time scale
%*0 -- Henriques2012 (Mdot_eject=-gama_ej*M_ejected*M_vir)
% 1 -- Guo2010 (suppression in small halos)
% 2 -- Delucia2007
AGNRadioModeModel 0 ;if > 0 grow black hole during mergers,
%*0 -- Phenomenological AGN feedback scaling with Mhot*Mbh
% as in Henriques2013b + AGN heating from satellites,
% 2 -- Phenomenological accretion & AGN feedback as in Croton 2006,
% 3 -- Bondi-Hoyle accretion,
% 4 -- Cold cloud accretion
% 5 -- No cooling supression,
DiskInstabilityModel 0 ;allow bulges to form when the stellar disks become unstable
%*0 -- stability criteria of the stellar disk from Mo, Mao & White (1998)
% 1 -- no disk instabilities
BHGrowthInDiskInstabilityModel 0 ; accretion of gas into the BH due to disk instabilities
%*0 -- no BH growth in disk instabilities
% 1 -- cold gas moved into the BH in the same fraction as disk stars moved to bulge
HotGasStripingModel 0 ;choice of stripping of satellite galaxies
%*0 -- gradual stripping (cooling in type 1's) (Guo2010)
% Ejected gas of satellites distributed between type 1 and type 0,
% according to the fraction of dark matter retained in subhalos (Guo2010).
% This also determines where the ejected gas from type 2 ends up in mergers
% (maybe it should be a different option).
% 1-- immediate stripping (Delucia2007)
% Ejected gas of satellite galaxies contributes to the
% ejected component of type 0 if within Rvir
DisruptionModel 0 ;tidal disruption of type 2 galaxies
%*0 -- disruption of stars and cold gas in type 2 galaxies as in Guo11
% 1-- no disruption
StarBurstModel 0 ;recipe for starbursts during mergers
%*0 -- starbursts in major AND minor mergers as in Somerville 2001
BulgeFormationInMinorMergersOn 1 ;option for bulges to form in minor mergers as well as major
% 0 -- bulges only formed in major mergers
%*1 -- bulge formation in major AND minor mergers
MetallicityOption 1 ;Photometric tables from SPS models
% 0 -- only solar metallicity,
%*1 -- range of metallicities;
%------------------------------------------
%----- Parameters of physical model -------
%------------------------------------------
%-------------------------------------------
%% Reionization ;NOT USED if ReionizationModel=0
%-------------------------------------------
Reionization_z0 7.0
Reionization_zr 6.0
%-------------------------------------------
%% Star formation
%-------------------------------------------
SfrEfficiency 0.025 ;(eq. S14 in Henriques15)
SfrColdCrit 0.24 ;(eq. S15 in Henriques15) In units of 10^10Msun
%-------------------------------------------
%% Star formation bursts during mergers
%-------------------------------------------
SfrBurstEfficiency 0.60 ;(eq. S33 in Henriques15)
SfrBurstSlope 1.9 ;(eq. S33 in Henriques15)
%-------------------------------------------
% BH growth and AGN feedback
%-------------------------------------------
AgnEfficiency 5.3e-3 ;(eq. S24 in Henriques15) Quiescent accretion in the radio mode
BlackHoleGrowthRate 0.041 ;(eq. S23 in Henriques15) Fraction of cold gas added to the BH during mergers
BlackHoleCutoffVelocity 750. ;(eq. S23 in Henriques15)
BlackHoleSeedMass 1e-7 ;10^10 Msun/h
%-------------------------------------------
%% SN feedback
%-------------------------------------------
% Heating of cold gas to hot
FeedbackReheatingEpsilon 2.6 ;(eq. S18 in Henriques15) Mass of cold gas reheated due to SF (see Martin 1999)
ReheatPreVelocity 480. ;(eq. S19 in Henriques15) Normalization of SN feedback
ReheatSlope 0.72 ;(eq. S19 in Henriques15) Slope of the dependence of SN feedback on Vvir
% Ejection of gas from halo
FeedbackEjectionEfficiency 0.62 ;(eq. S16 in Henriques15) Fraction SN energy used in reheat and eject
EjectPreVelocity 100. ;(eq. S17 in Henriques15) Normalization of total SN
EjectSlope 0.80 ;(eq. S17 in Henriques15) Slope of total SN
ReIncorporationFactor 3.0e+10 ;(eq. S22 in Henriques15) Fraction of ejected mass reincorporated per dynamical time to hot
%-------------------------------------------
%% IMF
%-------------------------------------------
Yield 0.046 ;(section 1.9 in Henriques15) Fraction of metals instantaneously returned after SF (produced by short lived massive stars)
RecycleFraction 0.43 ;(section 1.6 in Henriques15) Fraction of SF mass instantaneously recycled back to cold - IMF dependent
%-------------------------------------------
%% Mergers
%-------------------------------------------
ThreshMajorMerger 0.1 ;(section 1.12.2 in Henriques15) Major merger when mass ratio gt this
MergerTimeMultiplier 2.5 ;(eq. S32 in Henriques15) Adjust the dynamical friction merging time
%-------------------------------------------
%%Hot Gas stripping
%-------------------------------------------
RamPressureStrip_CutOffMass 1.2e+4 ;(section 1.11.1 in Henriques15) In code Units of 10^10 (mass above which there is stripping)
EnergySN 1.0e51 ;(section 1.7 in Henriques15)
EtaSN 8.0e-3