Changing the makefile options might change the output structure. Always make sure you are trying to read the correct
LGalaxies_struct in your plotting routines.
Options that control I/O and speed:
- OPT += -DOVERWRITE_OUTPUT: overwrite output files if they exist
- OPT += -DNOUT=28: define the number of output snapshots (read from /input/desired_output_redshifts.txt).
- OPT += -DPARALLEL: if ON, the code will be run in parallel. Each processor will run on a different dark matter tree file.
- OPT += -DGALAXYTREE: the entire galaxy tree (including long long IDs will be outputted)
- OPT += -DLOADIDS: loads the tree_dbids files. This is needed for OPT += -DGALAXYTREE and is useful if one needs to follow
progenitors/descendants while running the code.
- OPT += -DUPDATETYPETWO: uses information from the most bounded particle at the time haloes get disrupted to track the dynamics
of orphan galaxies. Crucial to properly track the dynamics of satellites in simulations with resolution below MRII.
Options to choose the dark matter simulation:
- OPT += -DMRII: run the model on the MillenniumII Simulation (when combined with input_MRII_***.par input files)
- OPT += -DPHOENIX:
Options to run pre-defined models:
- OPT += -DGUO10: run the Guo2011 model (when combined with input_Guo11_***.par input files)
- OPT += -DGUO13: run the Guo2013 model (when combined with input_Guo13_***.par input files)
- OPT += -DHENRIQUES13: run the Henriques2013 model (when combined with input_Henriques13_***.par input files)
Option to control the output of star formation histories:
- OPT += -DSTAR_FORMATION_HISTORY: star formation histories are recorded. Option required in order to use OPT += -DPOST_PROCESS_MAGS and
detailed chemical enrichment. The number of bins to be outputted is defined in allvars.h, default: SFH_NMERGE 3, SFH_NBIN 20.
Options that control the output of emission properties:
- OPT += -DCOMPUTE_SPECPHOT_PROPERTIES: needs to be ON for any emission properties to be computed.
- OPT += -DPOST_PROCESS_MAGS: Compute the magnitudes in post-processing. If ON, magnitudes are computed from
star formation histories after galaxy evolution has been computed. It speeds up the code significantly and requires OPT += -DSTAR_FORMATION_HISTORY.
Emission properties in the code are calculated from pre-computed photometry tables. These give the emission in different filters,
per unit solar mass, as a function of age and metallicity. For a given episode of star formation, the metallicity and age of the
population at the output redshifts are interpolated in the tables to give the right emission properties. For observed-frame magnitudes,
it is also necessary to compute a table of redshifted emission, as a function of age and metallicity, for each filter and for each
output redshift. For the list of snapshots in the Millennium and MillenniumII simulations, photometric tables are already available for
WMAP1, WMAP7 and PLANCK cosmologies (you can use OPT += -DPHOTTABLES_PRECOMPUTED). For other simulations, or cosmologies, tables need
to be computed on the fly using OPT += -DSPEC_PHOTABLES_ON_THE_FLY.
- OPT += -DPHOTTABLES_PRECOMPUTED: use pre-computed photometry tables.
- OPT += -DSPEC_PHOTABLES_ON_THE_FLY: compute photometry tables on the fly
- OPT += -DFULL_SPECTRA: output full spectra, instead of magnitudes in different filters.
- OPT += -DAB: compute emission properties in the AB reference system.
- OPT += -DVEGA: compute emission properties in the Vega reference system.
Type of photometric properties to be computed. The list of magnitudes is read from ./input/Filter_Names.txt
and the number of magnitudes is given my the Makefile option NMAG.
- OPT += -DOUTPUT_REST_MAGS: output rest-frame magnitudes.
- OPT += -DCOMPUTE_OBS_MAGS: compute observed-frame magnitudes.
- OPT += -DOUTPUT_OBS_MAGS: output observed-frame magnitudes.
- OPT += -DICL: output luminosities for the intra-cluster light
- OPT += -DOUTPUT_MOMAF_INPUTS: output luminosities for lightcone construction.
- OPT += -DKITZBICHLER: output luminosities for lightcone construction.
Choose the stellar population synthesis model to use. PhotPrefix in input_***.par needs to be changed accordingly.
- OPT += -DM05: use Maraston 2005 stellar populations.
- OPT += -DBC03: use Bruzual & Charlot 2003 stellar populations.
- OPT += -DCB07: use Charlot & Bruzual 2007 stellar populations.
- OPT += -DNMAG: number of filters for which luminosities will be computed.
Detailed Chemical Enrichment:
- OPT += -DDETAILED_METALS_AND_MASS_RETURN: Switches on the detailed chemical enrichment model described in Yates et al. 2013.
This option incorporates a detailed calculation of chemical enrichment into the galaxy formation model. Instead of assuming that a fixed
yield of metals is formed and immediately returned into the ISM in each star formation event, the mass of each element produced in stars
of different masses (i.e. ages) and initial metallicities is computed. The fraction of mass and elements returned into the ISM is then
computed over time taking into account stellar evolution. Stellar winds and the death of stars in different types of SN will then return
different elements and inject energy into the surrounding medium.
- OPT += -DFEEDBACK_COUPLED_WITH_MASS_RETURN: Switches on coupling between SN feedback and the chemical enrichment model.
This option makes the SN feedback dependent on the actual amount of material released by SNe and stellar winds at time t, rather
than on the amount of mass formed into stars at time t. This allows the feedback from an given stellar population to be more
realistically delayed and distributed over time.
- OPT += -DINDIVIDUAL_ELEMENTS: Switches on tracking of individual chemical elements. This option allows the 11 chemical
elements (H, He, C , N, O, Ne, Mg, Si, S, Ca, and Fe) considered to be self-consistently tracked, as they are produced and
distributioned through the various components of a galaxy. When switched off, only the total metal mass (i.e. the sum of
the individual elements considered) is tracked.
- OPT += -DMETALRICHWIND: Switches on galactic winds with a metallicity independent of that in the ISM. This option allows
a user-defined (or see -DGASDENSITYWIND) fraction, f_wind, of the ejecta from SNe-II in the stellar disc to be deposited directly
in the hot gas of a galaxy. If -DINDIVIDUAL_ELEMENTS is on, the chemical composition of this 'metal-rich wind' is identical to the
composition of the SNe-II ejecta. Note that any SNe exploding in the stellar bulge directly enrich the hot gas
(but see -DBULGE_TO_COLD). Direct depositing of ejecta from SN-Ia in the stellar disc into the hot gas is controlled by the
-DSNIATOHOT option. Ejecta from AGB stars in the stellar disc is always assumed to only enrich the cold gas.
- OPT += -DMAINELEMENTS: Switches on tracking of only five key chemical elements (H, He, O, Mg, and Fe). Only works when the
-DINDIVIDUAL_ELEMENTS option is on.
- OPT += -DSNIATOHOT: Switches on direct enrichment of the CGM/ICM by SNe-Ia in the stellar disc. This option allows 100% of the
ejecta from SNe-Ia in the stellar disc to be directly deposited into the hot gas. When off, 100% of this ejecta is deposited into
the cold gas. Note that any SNe exploding in the stellar bulge directly enrich the hot gas (but see -DBULGE_TO_COLD). Direct depositing
of ejecta from SN-II in the stellar disc into the hot gas is controlled by the -DMETALRICHWIND option. Ejecta from AGB stars in the
stellar disc is always assumed to only enrich the cold gas.
- OPT += -DGASDENSITYFWIND: Switches on metal-rich galactic winds with a strength inversely proportional to the density of the ISM
(see Yates et al. 2013, section 6.3.3). This option allows the value of f_wind (the fraction of SN-II ejecta directly deposited into the
hot gas) to be inversely proportional to the gas density of the cold gas.
- OPT += -DBULGE_TO_COLD: Switches on enrichment of the ISM by stars in the stellar bulge. This option allows SNe-Ia, SNe-II, and AGB
stars in the stellar bulge to directly enrich the cold gas. When off, their ejecta directly enriches the hot gas.
- OPT += -DPORTINARI: Switches on the SN-II stellar yields of Portinari et al. (1999). This option loads the SN-II stellar yield
tables provided by Portinari et al. (1998) for use in the chemical enrichment model.
- OPT += -DCHIEFFI: Switches on the SN-II stellar yields of Chieffi et al. (2004). This option loads the SN-II stellar yield tables
provided by Chieffi et al. (2004) for use in the chemical enrichment model.
- OPT += -DBIMODALDTD: Switches on the bi-modal SN-Ia DTD of Mannucci et al. (2006) (see Yates et al. 2013, section 4.1). This option
makes the chemical enrichment model assume a bi-modal SN-Ia delay-time distribution (DTD) when calculating the amount of SN-Ia ejecta
released at any given time after star formation.
- OPT += -DGAUSSIANDTD: Switches on the narrow Gaussian SN-Ia DTD of Strolger et al. (2004) (see Yates et al. 2013, section 4.1).
This option makes the chemical enrichment model assume a narrow Gaussian SN-Ia delay-time distribution (DTD) when calculating the amount of
SN-Ia ejecta released at any given time after star formation.
- OPT += -DPOWERLAWDTD: Switches on the power-law SN-Ia DTD of Maoz et al. (2012) (see Yates et al. 2013, section 4.1). This option
makes the chemical enrichment model assume a power-law SN-Ia delay-time distribution (DTD) when calculating the amount of SN-Ia ejecta
released at any given time after star formation.
- OPT += -DRUITERDTD: Switches on the bi-modal SN-Ia DTD of Ruiter et al. (2011). This option makes the chemical enrichment model
assume a bi-modal SN-Ia delay-time distribution (DTD), based on the sub-Chandrasekhar-mass detonation model described by
Ruiter et al. (2011), when calculating the amount of SN-Ia ejecta released at any given time after star formation.