double get_merging_radius(int halonr, int mother_halonr, int p)
{
int central_halonr;
double SatelliteRadius, MotherHaloRvir;
/* recipe updated for more accurate merging time (see BT eq 7.26),
now satellite radius at previous timestep is included */
central_halonr = Halo[Halo[halonr].Descendant].FirstProgenitor;
if(Gal[p].Type == 1)
central_halonr=mother_halonr;
if(central_halonr == halonr)
terminate("central_halonr == halonr");
/* in physical length (/(1 + ZZ[Halo[halonr].SnapNum]))*/
SatelliteRadius = separation_halo(central_halonr,halonr)/(1 + ZZ[Halo[halonr].SnapNum]);
MotherHaloRvir = get_virial_radius(mother_halonr);
if(SatelliteRadius > MotherHaloRvir)
SatelliteRadius = MotherHaloRvir;
return SatelliteRadius;
}
double estimate_merging_time(int halonr, int mother_halonr, int p)
{
int central_halonr;
double coulomb, mergtime, SatelliteMass, SatelliteRadius, MotherHaloRvir;
/** @brief Binney & Tremaine 1987 - 7.26 merging time for satellites due to
* dynamical friction. After Delucia2007 *2, shown to agree with
* Kolchin2008 simulations in Delucia2010. This is set when a galaxy
* becomes a type 2 or being a type 1 \f$M_{\rm{star}}>M_{\rm{vir}}\f$.
* In DeLucia2007 they could only merge into a type 0, now (after
* guo2010) they can merge into a type 1. */
/* recipe updated for more accurate merging time (see BT eq 7.26),
now satellite radius at previous timestep is included */
central_halonr = Halo[Halo[halonr].Descendant].FirstProgenitor;
if(Gal[p].Type == 1)
central_halonr=mother_halonr;
if(central_halonr == halonr)
{
terminate("can't be...!\n");
}
coulomb = log(Halo[mother_halonr].Len / ((double) Halo[halonr].Len) + 1);
/* should include stellar+cold gas in SatelliteMass! */
SatelliteMass = get_virial_mass(halonr)+(Gal[p].DiskMass+Gal[p].BulgeMass);
SatelliteRadius = separation_halo(central_halonr,halonr)/(1 + ZZ[Halo[halonr].SnapNum]);
int j;
for (j = 0; j < 3; j++)
Gal[p].DistanceToCentralGal[j] = wrap(Halo[central_halonr].Pos[j] - Halo[halonr].Pos[j], BoxSize);
MotherHaloRvir = get_virial_radius(mother_halonr);
if(SatelliteRadius > MotherHaloRvir)
SatelliteRadius = MotherHaloRvir;
if(SatelliteMass > 0.0) {
mergtime = 1.17 * SatelliteRadius * SatelliteRadius * get_virial_velocity(mother_halonr) /
(coulomb * G * SatelliteMass); // Binney & Tremaine Eq.7.26
/* change introduced by Delucia2007 to fit observations */
mergtime = 2.*mergtime;
}
else
mergtime = -99999.9;
return mergtime;
}
void prepare_galaxy_for_output(int n, struct GALAXY *g, struct GALAXY_OUTPUT *o)
#endif
{
int j,ibin;
#ifndef NO_PROPS_OUTPUTS
o->Type = g->Type;
o->SnapNum = g->SnapNum;
o->CentralMvir = get_virial_mass(Halo[g->HaloNr].FirstHaloInFOFgroup);
o->CentralRvir = get_virial_radius(Halo[g->HaloNr].FirstHaloInFOFgroup);
o->Mvir = g->Mvir;
o->Rvir = g->Rvir;
o->Vvir = g->Vvir;
for(j = 0; j < 3; j++)
{
o->Pos[j] = g->Pos[j];
o->DistanceToCentralGal[j] = wrap(Halo[Halo[g->HaloNr].FirstHaloInFOFgroup].Pos[j] - g->Pos[j],BoxSize);;
}
o->ColdGas = g->ColdGas;
o->DiskMass = g->DiskMass;
o->BulgeMass = g->BulgeMass;
o->HotGas = g->HotGas;
o->BlackHoleMass = g->BlackHoleMass;
#endif
#ifdef COMPUTE_SPECPHOT_PROPERTIES
#ifndef POST_PROCESS_MAGS
#ifdef OUTPUT_REST_MAGS
/* Luminosities are converted into Mags in various bands */
for(j = 0; j < NMAG; j++)
o->Mag[j] = lum_to_mag(g->Lum[j][n]);
#endif
#endif //ndef POST_PROCESS_MAGS
#endif //COMPUTE_SPECPHOT_PROPERTIES
#ifndef LIGHT_OUTPUT
#ifndef NO_PROPS_OUTPUTS
#ifdef GALAXYTREE
o->HaloID = HaloIDs[g->HaloNr].HaloID;
o->Redshift = ZZ[g->SnapNum];
int ii = (int) floor(o->Pos[0] * ScaleFactor);
int jj = (int) floor(o->Pos[1] * ScaleFactor);
int kk = (int) floor(o->Pos[2] * ScaleFactor);
o->PeanoKey = peano_hilbert_key(ii, jj, kk, Hashbits);
o->SubID = calc_big_db_subid_index(g->SnapNum, Halo[g->HaloNr].FileNr, Halo[g->HaloNr].SubhaloIndex);
int tmpfirst = Halo[g->HaloNr].FirstHaloInFOFgroup;
int lenmax = 0;
int next = tmpfirst;
while(next != -1)
{
if(Halo[next].Len > lenmax)
{
lenmax = Halo[next].Len;
tmpfirst = next;
}
next = Halo[next].NextHaloInFOFgroup;
}
o->MMSubID = calc_big_db_subid_index(g->SnapNum, Halo[tmpfirst].FileNr, Halo[tmpfirst].SubhaloIndex);
#endif
o->LookBackTimeToSnap = NumToTime(g->SnapNum)*UnitTime_in_years/Hubble_h;
o->InfallVmax = g->InfallVmax;
o->InfallSnap = g->InfallSnap;
o-> InfallHotGas = g-> InfallHotGas;
o->HotRadius = g->HotRadius;
#ifdef HALOPROPERTIES
o->HaloM_Mean200 = g->HaloM_Mean200;
o->HaloM_Crit200 = g->HaloM_Crit200;
o->HaloM_TopHat = g->HaloM_TopHat;
o->HaloVelDisp = g->HaloVelDisp;
o->HaloVmax = g->HaloVmax;
#endif
o->Len = g->Len;
o->Vmax = g->Vmax;
o->BulgeSize = g->BulgeSize;
o->EjectedMass = g->EjectedMass;
o->BlackHoleGas = g->BlackHoleGas;
for(j = 0; j < 3; j++)
{
o->Vel[j] = g->Vel[j];
#ifdef HALOSPIN
o->HaloSpin[j] = g->HaloSpin[j];
#endif
#ifndef H2_AND_RINGS
o->GasSpin[j] = g->GasSpin[j];
o->StellarSpin[j] = g->StellarSpin[j];
#else
o->DiskSpin[j] = g->DiskSpin[j];
#endif
#ifdef HALOPROPERTIES
o->HaloPos[j] = g->HaloPos[j];
o->HaloVel[j] = g->HaloVel[j];
o->HaloSpin[j] = g->HaloSpin[j];
#endif
}
o->XrayLum = g->XrayLum;
o->GasDiskRadius = g->GasDiskRadius;
o->StellarDiskRadius = g->StellarDiskRadius;
o->CoolingRadius = g->CoolingRadius;
o->ICM = g->ICM;
//o->MetalsICM = CORRECTDBFLOAT(g->MetalsICM);
o->MetalsICM = g->MetalsICM;
o->QuasarAccretionRate = g->QuasarAccretionRate * UnitMass_in_g / UnitTime_in_s * SEC_PER_YEAR / SOLAR_MASS;
o->RadioAccretionRate = g->RadioAccretionRate * UnitMass_in_g / UnitTime_in_s * SEC_PER_YEAR / SOLAR_MASS;
o->CosInclination = g->CosInclination;
if(g->Type == 2 || (g->Type == 1 && g->MergeOn == 1)) {
o->OriMergTime=g->OriMergTime;
o->MergTime = g->MergTime;
}
else {
o->OriMergTime=0.0;
o->MergTime = 0.0;
}
#ifndef GALAXYTREE
o->HaloIndex = g->HaloNr;
#endif
#ifdef MBPID
o->MostBoundID = g->MostBoundID;
#endif
#ifdef GALAXYTREE
o->DisruptOn = g->DisruptOn;
#endif
#ifdef MERGE01
o->MergeOn = g->MergeOn;
#endif
//METALS
/*o->MetalsColdGas = CORRECTDBFLOAT(g->MetalsColdGas);
o->MetalsDiskMass = CORRECTDBFLOAT(g->MetalsDiskMass);
o->MetalsBulgeMass = CORRECTDBFLOAT(g->MetalsBulgeMass);
o->MetalsHotGas = CORRECTDBFLOAT(g->MetalsHotGas);
o->MetalsEjectedMass = CORRECTDBFLOAT(g->MetalsEjectedMass);
#ifdef METALS_SELF
o->MetalsHotGasSelf = CORRECTDBFLOAT(g->MetalsHotGasSelf);
#endif*/
o->MetalsColdGas = g->MetalsColdGas;
o->MetalsDiskMass = g->MetalsDiskMass;
o->MetalsBulgeMass = g->MetalsBulgeMass;
o->MetalsHotGas = g->MetalsHotGas;
o->MetalsEjectedMass = g->MetalsEjectedMass;
#ifdef METALS_SELF
o->MetalsHotGasSelf = g->MetalsHotGasSelf;
#endif
#ifdef TRACK_BURST
o->BurstMass=g->BurstMass;
#endif
#ifdef H2_AND_RINGS
for(j=0; j<RNUM; j++)
{
o->H2fractionr[j] = g -> H2fractionr[j];
o->ColdGasr[j] = g->ColdGasr[j];
o->DiskMassr[j] = g->DiskMassr[j];
o->MetalsColdGasr[j] = g->MetalsColdGasr[j];
o->MetalsDiskMassr[j] = g->MetalsDiskMassr[j];
}
#endif
//STAR FORMATION HISTORIES / RATES
#ifdef STAR_FORMATION_HISTORY
o->sfh_ibin=g->sfh_ibin;
ibin=0;
for (j=0;j<=o->sfh_ibin;j++) {
#ifndef NORMALIZEDDB
// o->sfh_time[j]=(g->sfh_t[j]+g->sfh_dt[j]/2.-NumToTime(g->SnapNum))*UnitTime_in_years/Hubble_h; //Time from middle of this sfh bin to snapshot - converted from code units to years
//o->sfh_time[j]=(g->sfh_t[j]+g->sfh_dt[j]/2.)*UnitTime_in_years/Hubble_h; //ROB: Lookback time to middle of SFH bin, in years //ROB: Now use LookBackTimeToSnap + sfh_time instead.
// o->sfh_dt[j]=g->sfh_dt[j]*UnitTime_in_years/Hubble_h;
o->sfh_DiskMass[j]=g->sfh_DiskMass[j];
o->sfh_BulgeMass[j]=g->sfh_BulgeMass[j];
o->sfh_ICM[j]=g->sfh_ICM[j];
o->sfh_MetalsDiskMass[j]=g->sfh_MetalsDiskMass[j];
o->sfh_MetalsBulgeMass[j]=g->sfh_MetalsBulgeMass[j];
o->sfh_MetalsICM[j]=g->sfh_MetalsICM[j];
//#ifdef DETAILED_METALS_AND_MASS_RETURN
#ifdef INDIVIDUAL_ELEMENTS
o->sfh_ElementsDiskMass[j]=g->sfh_ElementsDiskMass[j];
o->sfh_ElementsBulgeMass[j]=g->sfh_ElementsBulgeMass[j];
o->sfh_ElementsICM[j]=g->sfh_ElementsICM[j];
#endif
//#endif
#ifdef TRACK_BURST
o->sfh_BurstMass[j]=g->sfh_BurstMass[j];
#endif
#else // NORMALIZEDDB
sfh_bin[j].sfh_DiskMass = g->sfh_DiskMass[j];
sfh_bin[j].sfh_BulgeMass = g->sfh_BulgeMass[j];
sfh_bin[j].sfh_ICM = g->sfh_ICM[j];
sfh_bin[j].sfh_MetalsDiskMass = g->sfh_MetalsDiskMass[j];
sfh_bin[j].sfh_MetalsBulgeMass = g->sfh_MetalsBulgeMass[j];
sfh_bin[j].sfh_MetalsICM = g->sfh_MetalsICM[j];
sfh_bin[j].sfh_ibin = j;
sfh_bin[j].snapnum = g->SnapNum;
sfh_bin[j].GalID = -1; // TODO must be reset
#endif // NORMALIZEDDB
}
//Set all non-used array elements to zero:
// important if we want to read files in database that all values are valid SQLServer floats
for (j=o->sfh_ibin+1;j<SFH_NBIN;j++) {
#ifndef NORMALIZEDDB
// o->sfh_time[j]=0.;
// o->sfh_dt[j]=0.;
o->sfh_DiskMass[j]=0.;
o->sfh_BulgeMass[j]=0.;
o->sfh_ICM[j]=0.;
o->sfh_MetalsDiskMass[j]=metals_init();
o->sfh_MetalsBulgeMass[j]=metals_init();
o->sfh_MetalsICM[j]=metals_init();
#ifdef INDIVIDUAL_ELEMENTS
o->sfh_ElementsDiskMass[j]=elements_init();
o->sfh_ElementsBulgeMass[j]=elements_init();
o->sfh_ElementsICM[j]=elements_init();
#endif
#ifdef TRACK_BURST
o->sfh_BurstMass[j]=0.;
#endif
#else
sfh_bin[j].sfh_DiskMass=0;
sfh_bin[j].sfh_BulgeMass=0;
sfh_bin[j].sfh_ICM=0;
sfh_bin[j].sfh_ibin = 0;
sfh_bin[j].snapnum = g->SnapNum;
// TODO other elements not important, are not being written anyway. Or are they used elsewhere?
#endif
}
#endif //STAR_FORMATION_HISTORY
#ifdef INDIVIDUAL_ELEMENTS
/*for (j=0;j<ELEMENT_NUM;j++)
{
o->DiskMass_elements[j]=g->DiskMass_elements[j];
o->BulgeMass_elements[j]=g->BulgeMass_elements[j];
o->ColdGas_elements[j]=g->ColdGas_elements[j];
o->HotGas_elements[j]=g->HotGas_elements[j];
o->EjectedMass_elements[j]=g->EjectedMass_elements[j];
o->ICM_elements[j]=g->ICM_elements[j];
}*/
/*o->DiskMass_elements = CORRECTDBFLOAT(g->DiskMass_elements);
o->BulgeMass_elements = CORRECTDBFLOAT(g->BulgeMass_elements);
o->ColdGas_elements = CORRECTDBFLOAT(g->ColdGas_elements);
o->HotGas_elements = CORRECTDBFLOAT(g->HotGas_elements);
o->ICM_elements = CORRECTDBFLOAT(g->ICM_elements);*/
o->DiskMass_elements = g->DiskMass_elements;
o->BulgeMass_elements = g->BulgeMass_elements;
o->ColdGas_elements = g->ColdGas_elements;
o->HotGas_elements = g->HotGas_elements;
o->EjectedMass_elements = g->EjectedMass_elements;
o->ICM_elements = g->ICM_elements;
#endif
o->PrimordialAccretionRate = CORRECTDBFLOAT(g->PrimordialAccretionRate * UnitMass_in_g / UnitTime_in_s * SEC_PER_YEAR / SOLAR_MASS);
o->CoolingRate = CORRECTDBFLOAT(g->CoolingRate * UnitMass_in_g / UnitTime_in_s * SEC_PER_YEAR / SOLAR_MASS);
o->CoolingRate_beforeAGN = CORRECTDBFLOAT(g->CoolingRate_beforeAGN * UnitMass_in_g / UnitTime_in_s * SEC_PER_YEAR / SOLAR_MASS);
//NOTE: in Msun/yr
#ifdef SAVE_MEMORY
o->Sfr = CORRECTDBFLOAT(g->Sfr * UnitMass_in_g / UnitTime_in_s * SEC_PER_YEAR / SOLAR_MASS);
o->SfrBulge = CORRECTDBFLOAT(g->SfrBulge * UnitMass_in_g / UnitTime_in_s * SEC_PER_YEAR / SOLAR_MASS);
#ifdef H2_AND_RINGS
for(j=0; j<RNUM; j++) o->Sfrr[j] = g->Sfrr[j] * UnitMass_in_g / UnitTime_in_s * SEC_PER_YEAR / SOLAR_MASS;
#endif
#else
o->Sfr = CORRECTDBFLOAT(g->Sfr[n] * UnitMass_in_g / UnitTime_in_s * SEC_PER_YEAR / SOLAR_MASS);
o->SfrBulge = CORRECTDBFLOAT(g->SfrBulge[n] * UnitMass_in_g / UnitTime_in_s * SEC_PER_YEAR / SOLAR_MASS);
#endif
#endif //NO_PROPS_OUTPUTS
//MAGNITUDES
#ifdef COMPUTE_SPECPHOT_PROPERTIES
#ifdef POST_PROCESS_MAGS
/* int N_vespa_files=29, N_vespa_AgeBins=16;
double vespa_age[17]={0.000125893, 0.02000, 0.03000, 0.04800, 0.07400, 0.11500,
0.17700, 0.27500, 0.42500, 0.65800, 1.02000, 1.57000,
2.44000, 3.78000, 5.84000, 9.04000, 14.0000};
int vespa_sfh_IDs[29]={0, 1, 12, 16, 2, 22, 23, 27, 29, 36,
42, 44, 50, 53, 54, 55, 56, 57, 61, 62,
63, 64, 65, 71, 81, 82, 90, 94, 99};
double vespa_sfh[N_vespa_AgeBins], vespa_metal[N_vespa_AgeBins], dumb[6];
int ii, jj, kk;
char buf[1000], sbuf[1000];
FILE *fa;
for (ii=1;ii<N_vespa_files;ii++)
{
sprintf(buf, "./devel/vespa_sfh/disc_good_%d.txt", vespa_sfh_IDs[ii]);
if(!(fa = fopen(buf, "r")))
{
char sbuf[1000];
sprintf(sbuf, "can't open file `%s'\n", buf);
terminate(sbuf);
}
for(jj=0;jj<6;jj++)
fgets(buf, 300, fa);
//read vespa SFH and metallicities
for (jj=0;jj<N_vespa_AgeBins;jj++)
{
vespa_sfh[jj]=0.;
vespa_metal[jj]=0.;
fscanf(fa,"%lg %lg %lg %lg %lg %lg %lg %lg\n", &dumb[0], &dumb[1], &vespa_sfh[jj], &dumb[2], &vespa_metal[jj],
&dumb[3], &dumb[4], &dumb[5]);
}
fclose(fa);
for (jj=0;jj<SFH_NBIN;jj++)
{
if(jj<N_vespa_AgeBins)
{
o->sfh_time[jj]=(vespa_age[jj]+vespa_age[jj+1])/2.*1.e9;
o->sfh_dt[jj]=(vespa_age[jj+1]-vespa_age[jj])/2.*1.e9;
o->sfh_DiskMass[jj]=vespa_sfh[jj];
o->sfh_BulgeMass[jj]=0.;
o->sfh_MetalsDiskMass[jj]=vespa_metal[jj]*o->sfh_DiskMass[jj];
o->sfh_MetalsBulgeMass[jj]=metals_init();
}
else
{
o->sfh_time[jj]=0.;
o->sfh_dt[jj]=0.;
o->sfh_DiskMass[jj]=0.;
o->sfh_BulgeMass[jj]=0.;
o->sfh_MetalsDiskMass[jj]=metals_init();
o->sfh_MetalsBulgeMass[jj]=metals_init();
}
}
post_process_spec_mags(o);
sprintf(buf, "./devel/vespa_sfh/output_spectradisc_good_%d.txt", vespa_sfh_IDs[ii]);
if(!(fa = fopen(buf, "w")))
{
char sbuf[1000];
sprintf(sbuf, "can't open file `%s'\n", buf);
terminate(sbuf);
}
for(jj=0;jj<NMAG;jj++)
fprintf(fa,"%e\n",o->Mag[jj]);
fclose(fa);
exit(0);
}
*/
//Convert recorded star formation histories into mags
#ifdef NORMALIZEDDB
post_process_spec_mags(o, &(sfh_bin[0]));
#else
post_process_spec_mags(o);
#endif
#else //ndef POST_PROCESS_MAGS
#ifdef OUTPUT_REST_MAGS
// Luminosities are converted into Mags in various bands
for(j = 0; j < NMAG; j++)
{
//o->Mag[j] = lum_to_mag(g->Lum[j][n]); -> DONE ON TOP FOR LIGHT_OUTPUT AS WELL
o->MagBulge[j] = lum_to_mag(g->LumBulge[j][n]);
o->MagDust[j] = lum_to_mag(g->LumDust[j][n]);
#ifdef ICL
o->MagICL[j] = lum_to_mag(g->ICLLum[j][n]);
#endif
}
#if defined(READXFRAC) || defined(WITHRADIATIVETRANSFER)
o->Xfrac3d = g->Xfrac3d;
#endif
#endif //OUTPUT_REST_MAGS
#ifdef OUTPUT_OBS_MAGS
#ifdef COMPUTE_OBS_MAGS
// Luminosities in various bands
for(j = 0; j < NMAG; j++)
{
o->ObsMag[j] = lum_to_mag(g->ObsLum[j][n]);
o->ObsMagBulge[j] = lum_to_mag(g->ObsLumBulge[j][n]);
o->ObsMagDust[j] = lum_to_mag(g->ObsLumDust[j][n]);
#ifdef ICL
o->ObsMagICL[j] = lum_to_mag(g->ObsICL[j][n]);
#endif
#ifdef OUTPUT_MOMAF_INPUTS
o->dObsMag[j] = lum_to_mag(g->dObsLum[j][n]);
o->dObsMagBulge[j] = lum_to_mag(g->dObsLumBulge[j][n]);
o->dObsMagDust[j] = lum_to_mag(g->dObsLumDust[j][n]);
#ifdef ICL
o->dObsMagICL[j] = lum_to_mag(g->dObsICL[j][n]);
#endif
#endif
}
#endif //COMPUTE_OBS_MAGS
#endif //OUTPUT_OBS_MAGS
#endif //ndef POST_PROCESS_MAGS
#endif //COMPUTE_SPECPHOT_PROPERTIES
#ifndef NO_PROPS_OUTPUTS
if((g->DiskMass+g->BulgeMass)> 0.0)
{
o->MassWeightAge = g->MassWeightAge[n] / (g->DiskMass+g->BulgeMass);
o->MassWeightAge = o->MassWeightAge / 1000. * UnitTime_in_Megayears / Hubble_h; //Age in Gyr
}
else
o->MassWeightAge = 0.;
#endif
#ifdef FIX_OUTPUT_UNITS
fix_units_for_ouput(o);
#endif
#endif //ndef LIGHT_OUTPUT
// DEBUG
// printf(" EXIT sfh_bin %d %f\n",sfh_bin,sfh_bin[0].sfh_DiskMass);
}
void prepare_galaxy_for_output(int filenr, int tree, struct GALAXY *g, struct GALAXY_OUTPUT *o)
{
int j, step;
o->SnapNum = g->SnapNum;
o->Type = g->Type;
// assume that because there are so many files, the trees per file will be less than 100000
// required for limits of long long
if(LastFile>=10000)
{
assert( g->GalaxyNr < TREE_MUL_FAC ); // breaking tree size assumption
assert(tree < (FILENR_MUL_FAC/10)/TREE_MUL_FAC);
o->GalaxyIndex = g->GalaxyNr + TREE_MUL_FAC * tree + (FILENR_MUL_FAC/10) * filenr;
assert( (o->GalaxyIndex - g->GalaxyNr - TREE_MUL_FAC*tree)/(FILENR_MUL_FAC/10) == filenr );
assert( (o->GalaxyIndex - g->GalaxyNr -(FILENR_MUL_FAC/10)*filenr) / TREE_MUL_FAC == tree );
assert( o->GalaxyIndex - TREE_MUL_FAC*tree - (FILENR_MUL_FAC/10)*filenr == g->GalaxyNr );
o->CentralGalaxyIndex = HaloGal[HaloAux[Halo[g->HaloNr].FirstHaloInFOFgroup].FirstGalaxy].GalaxyNr + TREE_MUL_FAC * tree + (FILENR_MUL_FAC/10) * filenr;
}
else
{
assert( g->GalaxyNr < TREE_MUL_FAC ); // breaking tree size assumption
assert(tree < FILENR_MUL_FAC/TREE_MUL_FAC);
o->GalaxyIndex = g->GalaxyNr + TREE_MUL_FAC * tree + FILENR_MUL_FAC * filenr;
assert( (o->GalaxyIndex - g->GalaxyNr - TREE_MUL_FAC*tree)/FILENR_MUL_FAC == filenr );
assert( (o->GalaxyIndex - g->GalaxyNr -FILENR_MUL_FAC*filenr) / TREE_MUL_FAC == tree );
assert( o->GalaxyIndex - TREE_MUL_FAC*tree - FILENR_MUL_FAC*filenr == g->GalaxyNr );
o->CentralGalaxyIndex = HaloGal[HaloAux[Halo[g->HaloNr].FirstHaloInFOFgroup].FirstGalaxy].GalaxyNr + TREE_MUL_FAC * tree + FILENR_MUL_FAC * filenr;
}
o->SAGEHaloIndex = g->HaloNr;
o->SAGETreeIndex = tree;
o->SimulationHaloIndex = Halo[g->HaloNr].MostBoundID;
o->mergeType = g->mergeType;
o->mergeIntoID = g->mergeIntoID;
o->mergeIntoSnapNum = g->mergeIntoSnapNum;
o->dT = g->dT * UnitTime_in_s / SEC_PER_MEGAYEAR;
for(j = 0; j < 3; j++)
{
o->Pos[j] = g->Pos[j];
o->Vel[j] = g->Vel[j];
o->Spin[j] = Halo[g->HaloNr].Spin[j];
}
o->Len = g->Len;
o->Mvir = g->Mvir;
o->CentralMvir = get_virial_mass(Halo[g->HaloNr].FirstHaloInFOFgroup);
o->Rvir = get_virial_radius(g->HaloNr); // output the actual Rvir, not the maximum Rvir
o->Vvir = get_virial_velocity(g->HaloNr); // output the actual Vvir, not the maximum Vvir
o->Vmax = g->Vmax;
o->VelDisp = Halo[g->HaloNr].VelDisp;
o->ColdGas = g->ColdGas;
o->StellarMass = g->StellarMass;
o->BulgeMass = g->BulgeMass;
o->HotGas = g->HotGas;
o->EjectedMass = g->EjectedMass;
o->BlackHoleMass = g->BlackHoleMass;
o->ICS = g->ICS;
o->MetalsColdGas = g->MetalsColdGas;
o->MetalsStellarMass = g->MetalsStellarMass;
o->MetalsBulgeMass = g->MetalsBulgeMass;
o->MetalsHotGas = g->MetalsHotGas;
o->MetalsEjectedMass = g->MetalsEjectedMass;
o->MetalsICS = g->MetalsICS;
o->SfrDisk = 0.0;
o->SfrBulge = 0.0;
o->SfrDiskZ = 0.0;
o->SfrBulgeZ = 0.0;
// NOTE: in Msun/yr
for(step = 0; step < STEPS; step++)
{
o->SfrDisk += g->SfrDisk[step] * UnitMass_in_g / UnitTime_in_s * SEC_PER_YEAR / SOLAR_MASS / STEPS;
o->SfrBulge += g->SfrBulge[step] * UnitMass_in_g / UnitTime_in_s * SEC_PER_YEAR / SOLAR_MASS / STEPS;
if(g->SfrDiskColdGas[step] > 0.0)
o->SfrDiskZ += g->SfrDiskColdGasMetals[step] / g->SfrDiskColdGas[step] / STEPS;
if(g->SfrBulgeColdGas[step] > 0.0)
o->SfrBulgeZ += g->SfrBulgeColdGasMetals[step] / g->SfrBulgeColdGas[step] / STEPS;
}
o->DiskScaleRadius = g->DiskScaleRadius;
if (g->Cooling > 0.0)
o->Cooling = log10(g->Cooling * UnitEnergy_in_cgs / UnitTime_in_s);
else
o->Cooling = 0.0;
if (g->Heating > 0.0)
o->Heating = log10(g->Heating * UnitEnergy_in_cgs / UnitTime_in_s);
else
o->Heating = 0.0;
o->QuasarModeBHaccretionMass = g->QuasarModeBHaccretionMass;
o->TimeOfLastMajorMerger = g->TimeOfLastMajorMerger * UnitTime_in_Megayears;
o->TimeOfLastMinorMerger = g->TimeOfLastMinorMerger * UnitTime_in_Megayears;
o->OutflowRate = g->OutflowRate * UnitMass_in_g / UnitTime_in_s * SEC_PER_YEAR / SOLAR_MASS;
//infall properties
if(g->Type != 0)
{
o->infallMvir = g->infallMvir;
o->infallVvir = g->infallVvir;
o->infallVmax = g->infallVmax;
}
else
{
o->infallMvir = 0.0;
o->infallVvir = 0.0;
o->infallVmax = 0.0;
}
}
int join_galaxies_of_progenitors(int halonr, int ngalstart)
{
int ngal, prog, mother_halo=-1, i, j, first_occupied, lenmax, lenoccmax, centralgal;
double previousMvir, previousVvir, previousVmax;
int step;
lenmax = 0;
lenoccmax = 0;
first_occupied = Halo[halonr].FirstProgenitor;
prog = Halo[halonr].FirstProgenitor;
if(prog >=0)
if(HaloAux[prog].NGalaxies > 0)
lenoccmax = -1;
// Find most massive progenitor that contains an actual galaxy
// Maybe FirstProgenitor never was FirstHaloInFOFGroup and thus has no galaxy
while(prog >= 0)
{
if(Halo[prog].Len > lenmax)
{
lenmax = Halo[prog].Len;
mother_halo = prog;
}
if(lenoccmax != -1 && Halo[prog].Len > lenoccmax && HaloAux[prog].NGalaxies > 0)
{
lenoccmax = Halo[prog].Len;
first_occupied = prog;
}
prog = Halo[prog].NextProgenitor;
}
ngal = ngalstart;
prog = Halo[halonr].FirstProgenitor;
while(prog >= 0)
{
for(i = 0; i < HaloAux[prog].NGalaxies; i++)
{
assert(ngal < FoF_MaxGals);
// This is the cruical line in which the properties of the progenitor galaxies
// are copied over (as a whole) to the (temporary) galaxies Gal[xxx] in the current snapshot
// After updating their properties and evolving them
// they are copied to the end of the list of permanent galaxies HaloGal[xxx]
Gal[ngal] = HaloGal[HaloAux[prog].FirstGalaxy + i];
Gal[ngal].HaloNr = halonr;
Gal[ngal].dT = -1.0;
// this deals with the central galaxies of (sub)halos
if(Gal[ngal].Type == 0 || Gal[ngal].Type == 1)
{
// this halo shouldn't hold a galaxy that has already merged; remove it from future processing
if(Gal[ngal].mergeType != 0)
{
Gal[ngal].Type = 3;
continue;
}
// remember properties from the last snapshot
previousMvir = Gal[ngal].Mvir;
previousVvir = Gal[ngal].Vvir;
previousVmax = Gal[ngal].Vmax;
if(prog == first_occupied)
{
// update properties of this galaxy with physical properties of halo
Gal[ngal].MostBoundID = Halo[halonr].MostBoundID;
for(j = 0; j < 3; j++)
{
Gal[ngal].Pos[j] = Halo[halonr].Pos[j];
Gal[ngal].Vel[j] = Halo[halonr].Vel[j];
}
Gal[ngal].Len = Halo[halonr].Len;
Gal[ngal].Vmax = Halo[halonr].Vmax;
Gal[ngal].deltaMvir = get_virial_mass(halonr) - Gal[ngal].Mvir;
if(get_virial_mass(halonr) > Gal[ngal].Mvir)
{
Gal[ngal].Rvir = get_virial_radius(halonr); // use the maximum Rvir in model
Gal[ngal].Vvir = get_virial_velocity(halonr); // use the maximum Vvir in model
}
Gal[ngal].Mvir = get_virial_mass(halonr);
Gal[ngal].Cooling = 0.0;
Gal[ngal].Heating = 0.0;
Gal[ngal].QuasarModeBHaccretionMass = 0.0;
Gal[ngal].OutflowRate = 0.0;
Gal[ngal].Lx_bol = 0.0;
for(step = 0; step < STEPS; step++)
{
Gal[ngal].SfrDisk[step] = Gal[ngal].SfrBulge[step] = 0.0;
Gal[ngal].SfrDiskColdGas[step] = Gal[ngal].SfrDiskColdGasMetals[step] = 0.0;
Gal[ngal].SfrBulgeColdGas[step] = Gal[ngal].SfrBulgeColdGasMetals[step] = 0.0;
}
if(halonr == Halo[halonr].FirstHaloInFOFgroup)
{
// a central galaxy
Gal[ngal].mergeType = 0;
Gal[ngal].mergeIntoID = -1;
Gal[ngal].MergTime = 999.9;
Gal[ngal].DiskScaleRadius = get_disk_radius(halonr, ngal);
Gal[ngal].Type = 0;
}
else
{
// a satellite with subhalo
Gal[ngal].mergeType = 0;
Gal[ngal].mergeIntoID = -1;
if(Gal[ngal].Type == 0) // remember the infall properties before becoming a subhalo
{
Gal[ngal].infallMvir = previousMvir;
Gal[ngal].infallVvir = previousVvir;
Gal[ngal].infallVmax = previousVmax;
}
if(Gal[ngal].Type == 0 || Gal[ngal].MergTime > 999.0)
// here the galaxy has gone from type 1 to type 2 or otherwise doesn't have a merging time.
Gal[ngal].MergTime = estimate_merging_time(halonr, Halo[halonr].FirstHaloInFOFgroup, ngal);
Gal[ngal].Type = 1;
}
}
else
{
// an orhpan satellite galaxy - these will merge or disrupt within the current timestep
Gal[ngal].deltaMvir = -1.0*Gal[ngal].Mvir;
Gal[ngal].Mvir = 0.0;
if(Gal[ngal].MergTime > 999.0 || Gal[ngal].Type == 0)
{
// here the galaxy has gone from type 0 to type 2 - merge it!
Gal[ngal].MergTime = 0.0;
Gal[ngal].infallMvir = previousMvir;
Gal[ngal].infallVvir = previousVvir;
Gal[ngal].infallVmax = previousVmax;
}
Gal[ngal].Type = 2;
}
}
ngal++;
}
prog = Halo[prog].NextProgenitor;
}
if(ngal == 0)
{
// We have no progenitors with galaxies. This means we create a new galaxy.
init_galaxy(ngal, halonr);
ngal++;
}
// Per Halo there can be only one Type 0 or 1 galaxy, all others are Type 2 (orphan)
// In fact, this galaxy is very likely to be the first galaxy in the halo if
// first_occupied==FirstProgenitor and the Type0/1 galaxy in FirstProgenitor was also the first one
// This cannot be guaranteed though for the pathological first_occupied!=FirstProgenitor case
for(i = ngalstart, centralgal = -1; i < ngal; i++)
{
if(Gal[i].Type == 0 || Gal[i].Type == 1)
{
assert(centralgal == -1);
centralgal = i;
}
}
for(i = ngalstart; i < ngal; i++)
Gal[i].CentralGal = centralgal;
return ngal;
}
