def __init__(self,clustername):
self.prefix=clustername
self.image24=homedir+'research/LocalClusters/Images/'+self.prefix+'/24um/Full'+self.prefix+'ch1rf_mosaic_minus_median_extract.fits'
self.noise24=homedir+'research/LocalClusters/Images/'+self.prefix+'/24um/Full'+self.prefix+'ch1rf_mosaic_unc.fits'
if (clustername.find('A1367') > -1):
self.image24='/home/rfinn/research/LocalClusters/Images/'+self.prefix+'/24um/'+self.prefix+'ch1r1_mosaic_minus_median_extract.fits'
self.noise24='/home/rfinn/research/LocalClusters/Images/'+self.prefix+'/24um/'+self.prefix+'ch1r1_mosaic_unc.fits'
elif (clustername.find('Herc')>-1):#for Abell 1367 and Hercules cluster
self.image24='/home/rfinn/research/LocalClusters/Images/'+self.prefix+'/24um/'+self.prefix+'ch1r1_mosaic_minus_median_extract.fits'
self.noise24='/home/rfinn/research/LocalClusters/Images/'+self.prefix+'/24um/'+self.prefix+'ch1r1_mosaic_unc.fits'
# read NSA table for each cluster
infile=homedir+'research/NSA/'+self.prefix+'_NSA.Fits'
self.ndat=atpy.Table(infile,type='fits')
self.nsadir=homedir+'research/NSA/'
self.cra=clusterRA[self.prefix]
self.cdec=clusterDec[self.prefix]
self.cz=clusterz[self.prefix]
self.biweightvel=clusterbiweightcenter[self.prefix]
self.biweightscale=clusterbiweightscale[self.prefix]
self.r200=2.02*(self.biweightscale)/1000./sqrt(OmegaL+OmegaM*(1.+self.cz)**3)*H0/70. # in Mpc
self.r200deg=self.r200*1000./my.DA(self.cz,h)/3600.
self.cdMpc=self.biweightvel/H0
self.cdcm=self.cdMpc*3.e24
self.csigma=self.biweightscale
self.mcl=my.clusterMass(self.csigma,self.cz,h)
self.AngDistance=my.DA(self.cz,h)
def __init__(self,clustername):
#Get current path so program can tell if this is being run on Becky or Rose's computer
self.prefix=clustername
self.cra=clusterRA[self.prefix]
self.cdec=clusterDec[self.prefix]
self.cz=clusterz[self.prefix]
self.biweightvel=clustercbi[self.prefix]
self.biweightscale=clustersbi[self.prefix]
self.r200=2.02*(self.biweightscale)/1000./sqrt(OmegaL+OmegaM*(1.+self.cz)**3)*H0/70. # in Mpc
self.r200deg=self.r200*1000./my.DA(self.cz,h)/3600.
self.cdMpc=self.biweightvel/H0
self.cdcm=self.cdMpc*3.e24
self.csigma=self.biweightscale
self.mcl=my.clusterMass(self.csigma,self.cz,h)
self.AngDistance=my.DA(self.cz,h)
mastertable=homedir+'research/LocalClusters/MasterTables/'+clustername+'mastertable.fits'
def __init__(self, clustername):
self.prefix = clustername
# read NSA table for each cluster
infile = homedir + 'research/NSA/' + self.prefix + '_NSA.Fits'
self.ndat = fits.getdata(infile)
self.nsadir = homedir + 'research/NSA/'
self.cra = clusterRA[self.prefix]
self.cdec = clusterDec[self.prefix]
self.cz = clusterz[self.prefix]
self.biweightvel = clusterbiweightcenter[self.prefix]
self.biweightscale = clusterbiweightscale[self.prefix]
self.r200 = 2.02 * (self.biweightscale) / 1000. / sqrt(
OmegaL + OmegaM * (1. + self.cz)**3) * H0 / 70. # in Mpc
self.r200deg = self.r200 * 1000. / my.DA(self.cz, h) / 3600.
self.cdMpc = self.biweightvel / H0
self.cdcm = self.cdMpc * 3.e24
self.csigma = self.biweightscale
self.mcl = my.clusterMass(self.csigma, self.cz, h)
self.AngDistance = my.DA(self.cz, h)
self.sdssflag = (self.ndat.ISDSS > -1) & (self.ndat.ABSMAG[:, 4] <
args.magnitudecut)
def __init__(self,clustername):
#Get current path so program can tell if this is being run on Becky or Rose's computer
self.prefix=clustername
self.john_prefix=john_prefix[self.prefix]
self.cra=clusterRA[self.prefix]
self.cdec=clusterDec[self.prefix]
self.cz=clusterz[self.prefix]
self.biweightvel=clusterbiweightcenter[self.prefix]
self.biweightscale=clusterbiweightscale[self.prefix]
self.r200=2.02*(self.biweightscale)/1000./sqrt(OmegaL+OmegaM*(1.+self.cz)**3)*H0/70. # in Mpc
self.r200deg=self.r200*1000./my.DA(self.biweightvel/3.e5,h)/3600.
self.cdMpc=self.biweightvel/H0
self.cdcm=self.cdMpc*3.e24
self.csigma=self.biweightscale
self.mcl=my.clusterMass(self.biweightscale,self.biweightvel/3.e5,h)
self.cLx=clusterLx[self.prefix]
self.mingalaxysize=mingalaxysize_kpc/my.DA(self.biweightvel/3.e5,h)
#infile=homedir+'research/LocalClusters/NSAmastertables/'+clustername+'_NSAmastertable.fits'
infile=homedir+'research/LocalClusters/NSAmastertables/NSAwithAGC/'+clustername+'_NSAmastertable_topcat.fits'
self.cutoutpath=homedir+'research/LocalClusters/cutouts/'+self.prefix+'/'
#infile='/home/rfinn/LocalClusters/MasterTables/'+clustername+'mastertable.fits'
self.n=atpy.Table(infile)
infile=homedir+'research/LocalClusters/NSAmastertables/'+clustername+'_NSAmastertable.fits'
self.nsa=atpy.Table(infile)
# read in WISE catalogs
infile=homedir+'research/LocalClusters/NSAmastertables/WISETables/'+clustername+'_WISE_NSA.fits'
self.wise=atpy.Table(infile)
# read in Galaxy Zoo catalogs
infile=homedir+'research/LocalClusters/NSAmastertables/GalaxyZooTables/'+clustername+'_GalaxyZoo.fits'
self.zoo=atpy.Table(infile)
#self.zooflag=self.zoo.zoo_match_flag | self.zoo.zoo_phot_match_flag
# read in GIM2D catalogs
infile=homedir+'research/LocalClusters/NSAmastertables/SimardGIM2D/'+clustername+'_GIM2D.fits'
self.gim2d=atpy.Table(infile)
# fields with _1 are from bulge+disk; fields with _2 are from pure sersic fit
infile=homedir+'research/LocalClusters/NSAmastertables/Sex24Tables/'+clustername+'_sex24.fits'
self.sex24=atpy.Table(infile)
infile=homedir+'research/LocalClusters/NSAmastertables/AGCTables/'+clustername+'_AGC.fits'
self.agc=atpy.Table(infile)
sersicparam24_file=homedir+'research/LocalClusters/NSAmastertables/GalfitSersicResults/'+self.prefix+'_GalfitSersicParam_24.fits'
self.galfit24=atpy.Table(sersicparam24_file)
infile=homedir+'research/LocalClusters/NSAmastertables/LocalDensityTables/'+clustername+'_localdensity.fits'
self.ld=atpy.Table(infile)
infile=homedir+'research/LocalClusters/NSAmastertables/CharyElbazTables/'+clustername+'_ce_lir.fits'
self.ce=atpy.Table(infile)
self.snrse=abs(self.ce.FLUX24/self.ce.FLUX24ERR)
# read in John's Lir catalogs - for his members only
infile=homedir+'research/LocalClusters/NSAmastertables/MoustakasLir/'+self.john_prefix+'_lir.fits'
self.lir=atpy.Table(infile,type='fits')
self.memb_id=self.lir.NSAID
# calculating magnitudes from fluxes provided from NSA
#
# m = 22.5 - 2.5 log_10 (flux_nanomaggies)
# from http://www.sdss3.org/dr8/algorithms/magnitudes.php#nmgy
self.nsamag=22.5-2.5*log10(self.n.NMGY)
self.sdssLr=10.**(-1*(self.n.ABSMAG[:,4]-SolarMag['r'])/2.5)
a,b=bellgr['r']
self.stellarmass=10.**(-1.*a+b*(self.n.ABSMAG[:,3]-self.n.ABSMAG[:,4]))*self.sdssLr
self.sdssLu=10.**(-1*(self.n.ABSMAG[:,2]-SolarMag['u'])/2.5)
self.sdssLg=10.**(-1*(self.n.ABSMAG[:,3]-SolarMag['g'])/2.5)
self.sdssLi=10.**(-1*(self.n.ABSMAG[:,5]-SolarMag['i'])/2.5)
self.sdssLz=10.**(-1*(self.n.ABSMAG[:,6]-SolarMag['z'])/2.5)
self.AngDistanceCl=my.DA(self.cz,h)
self.AngDistanceAll=zeros(len(self.n.ZDIST),'f')
for i in range(len(self.n.ZDIST)):
self.AngDistanceAll[i]=my.DA(self.n.ZDIST[i],h)
# FOR BACKWARDS COMPATABILITY WITH EXISTING CODE
# data from AGC-based mastertables
self.agcflag=self.agc.AGCMATCHFLAG
self.HIflag=(self.agc.FLUX100 > 0)
self.sdssflag=self.n.SDSSflag
self.sdssphotflag=self.n.SDSSphotflag
self.mpaflag=self.n.MPAFLAG
self.apexflag=self.n.APEXflag
self.sexsdssflag=self.n.SEXSDSSflag
self.sex24flag=self.n.SEX24FLAG
self.agcvoptflag=(self.agc.VOPT > 0)
self.agcnumber=self.agc.AGCNUMBER
self.raagc=self.agc.RA
self.decagc=self.agc.DEC
self.a100=self.agc.A100
self.b100=self.agc.B100
self.mag10=self.agc.MAG10
self.posang=self.agc.POSANG
self.bsteintype=self.agc.BSTEINTYPE
self.vopt=self.agc.VOPT
self.verr=self.agc.VERR
self.vsource=self.agc.VSOURCE
self.flux100=self.agc.FLUX100
self.rms100=self.agc.RMS100
self.v21=self.agc.V21
self.width=self.agc.WIDTH
self.widtherr=self.agc.WIDTHERR
#sdss info
self.sdssra=self.n.SDSSRA
self.sdssdec=self.n.SDSSDEC
self.sdssphotra=self.n.SDSSphotRA
self.sdssphotdec=self.n.SDSSphotDEC
self.sdssmag=self.n.SDSSMAG
self.sdssu=self.sdssmag[:,0]
self.sdssg=self.sdssmag[:,1]
self.sdssr=self.sdssmag[:,2]
self.sdssi=self.sdssmag[:,3]
self.sdssz=self.sdssmag[:,4]
self.sdssmagerr=self.n.SDSSMAGERR
self.sdssuerr=self.sdssmagerr[:,0]
self.sdssgerr=self.sdssmagerr[:,1]
self.sdssrerr=self.sdssmagerr[:,2]
self.sdssierr=self.sdssmagerr[:,3]
self.sdsszerr=self.sdssmagerr[:,4]
self.sdssspecz=self.n.SDSSSPECZ
self.sdssvopt=self.n.SDSSVOPT
self.sdsshaew=self.n.SDSSHAEW
self.sdsshaewerr=self.n.SDSSHAEWERR
self.sdssplate=self.n.SDSSPLATE
self.sdssfiberid=self.n.SDSSFIBERID
self.sdsstile=self.n.SDSSTILE
self.sdssrun=self.n.SDSSRUN
self.sdssrerun=self.n.SDSSRERUN
self.sdsscamcol=self.n.SDSSCAMCOL
self.sdssfield=self.n.SDSSFIELD
self.mpahalpha=self.n.MPAHALPHA
self.mpahbeta=self.n.MPAHBETA
self.mpao3=self.n.MPAOIII
self.mpan2=self.n.MPANII
#sextractor info
self.numberser=self.n.NUMBERSER
self.ximageser=self.n.XIMAGESER
self.yimageser=self.n.YIMAGESER
self.xminimageser=self.n.XMINIMAGESER
self.xmaximageser=self.n.XMAXIMAGESER
self.yminimageser=self.n.YMINIMAGESER
self.raser=self.n.RASER
self.decser=self.n.DECSER
self.fluxisoser=self.n.FLUXISOSER
self.fluxerrisoser=self.n.FLUXERRISOSER
self.magisoser=self.n.MAGISOSER
self.magerrisoser=self.n.MAGERRISOSER
self.fluxautoser=self.n.FLUXAUTOSER
self.fluxerrautoser=self.n.FLUXERRAUTOSER
self.magautoser=self.n.MAGAUTOSER
self.magerrautoser=self.n.MAGERRAUTOSER
self.fluxpetroser=self.n.FLUXPETROSER
self.fluxerrpetroser=self.n.FLUXERRPETROSER
self.magpetroser=self.n.MAGPETROSER
self.magerrpetroser=self.n.MAGERRPETROSER
self.kronradser=self.n.KRONRADSER#kron radius
self.petroradser=self.n.PETRORADSER#petrosian radius
self.fluxradser=self.n.FLUXRADSER#1/2 light radius
self.isoareaser=self.n.ISOAREASER
self.aworldser=self.n.AWORLDSER
self.bworldser=self.n.BWORLDSER
self.thetaser=self.n.THETASER
self.errthetaser=self.n.ERRTHETASER
self.thetaj2000ser=self.n.THETAJ2000SER
self.errthetaj2000ser=self.n.ERRTHETAJ2000SER
self.elongser=self.n.ELONGATIONSER
self.elliptser=self.n.ELLIPTICITYSER
self.fwhmser=self.n.FWHMSER
self.flagsser=self.n.FLAGSSER
self.classstarser=self.n.CLASSSTARSER
#SEXTRACTOR output 24 micron data
self.numberse24=self.n.NUMBERSE24
self.ximagese24=self.n.XIMAGESE24
self.yimagese24=self.n.YIMAGESE24
self.xminimagese24=self.n.XMINIMAGESE24
self.xmaximagese24=self.n.XMAXIMAGESE24
self.xminimagese24=self.n.YMINIMAGESE24
self.rase24=self.n.RASE24
self.decse24=self.n.DECSE24
self.fluxisose24=self.n.FLUXISOSE24
self.fluxerrisose24=self.n.FLUXERRISOSE24
self.magisose24=self.n.MAGISOSE24
self.magerrisose24=self.n.MAGERRISOSE24
self.fluxautose24=self.n.FLUXAUTOSE24
self.fluxerrautose24=self.n.FLUXERRAUTOSE24
self.magautose24=self.n.MAGAUTOSE24
self.magerrautose24=self.n.MAGERRAUTOSE24
self.fluxpetrose24=self.n.FLUXPETROSE24
self.fluxerrpetrose24=self.n.FLUXERRPETROSE24
self.magpetrose24=self.n.MAGPETROSE24
self.magerrpetrose24=self.n.MAGERRPETROSE24
self.kronradse24=self.n.KRONRADSE24
self.petroradse24=self.n.PETRORADSE24
self.fluxradse24=self.n.FLUXRADSE24
self.isoarease24=self.n.ISOAREASE24
self.aworldse24=self.n.AWORLDSE24
self.bworldse24=self.n.BWORLDSE24
self.thetase24=self.n.THETASE24
self.errthetase24=self.n.ERRTHETASE24
self.thetaj2000se24=self.n.THETAJ2000SE24
self.errthetaj2000se24=self.n.ERRTHETAJ2000SE24
self.elongse24=self.n.ELONGATIONSE24
self.elliptse24=self.n.ELLIPTICITYSE24
self.fwhmse24=self.n.FWHMSE24
self.flagsse24=self.n.FLAGSSE24
self.classstarse24=self.n.CLASSSTARSE24
self.f24dist=self.fluxautose24[self.sex24flag]
#apex output
self.mipsra=self.n.MIPSRA
self.mipsdec=self.n.MIPSDEC
self.mipsflux=self.n.MIPSFLUX
self.mipsfluxerr=self.n.MIPSFLUXERR
self.mipssnr=self.n.MIPSSNR
self.mipsdeblend=self.n.MIPSDEBLEND
self.mipsfluxap1=self.n.MIPSFLUXAP1
self.mipsfluxap1err=self.n.MIPSFLUXAP1ERR
self.mipsfluxap2=self.n.MIPSFLUXAP2
self.mipsfluxap2err=self.n.MIPSFLUXAP2ERR
self.mipsfluxap3=self.n.MIPSFLUXAP3
self.mipsfluxap4err=self.n.MIPSFLUXAP3ERR
self.On24ImageFlag_AGC=self.n.On24ImageFlag_2
self.On24ImageFlag=self.n.On24ImageFlag_1
self.supervopt=self.n.SUPERVOPT
self.ra=self.n.RA
self.dec=self.n.DEC
#self.stellarmass=self.n.STELLARMASS
#self.stellarmass_cl=self.n.STELLARMASS_CL
self.sdssabsmag=self.n.SDSSABSMAG
self.sdssMu=self.sdssabsmag[:,0]
self.sdssMg=self.sdssabsmag[:,1]
self.sdssMr=self.sdssabsmag[:,2]
self.sdssMi=self.sdssabsmag[:,3]
self.sdssMz=self.sdssabsmag[:,4]
self.sdsslum=self.n.SDSSLUM
self.sdssLu=self.sdsslum[:,0]
self.sdssLg=self.sdsslum[:,1]
self.sdssLr=self.sdsslum[:,2]
self.sdssLi=self.sdsslum[:,3]
self.sdssLz=self.sdsslum[:,4]
self.sdssabsmag_cl=self.n.SDSSABSMAG_CL
self.sdssMu=self.sdssabsmag_cl[:,0]
self.sdssMg=self.sdssabsmag_cl[:,1]
self.sdssMr=self.sdssabsmag_cl[:,2]
self.sdssMi=self.sdssabsmag_cl[:,3]
self.sdssMz=self.sdssabsmag_cl[:,4]
self.sdsslum_cl=self.n.SDSSLUM_CL
self.sdssLu_cl=self.sdsslum_cl[:,0]
self.sdssLg_cl=self.sdsslum_cl[:,1]
self.sdssLr_cl=self.sdsslum_cl[:,2]
self.sdssLi_cl=self.sdsslum_cl[:,3]
self.sdssLz_cl=self.sdsslum_cl[:,4]
self.sdsscolc=self.n.SDSSCOLC
self.sdssrowc=self.n.SDSSROWC
self.membflag =self.n.MEMBFLAG
self.morphflag =self.n.MORPHFLAG
self.morph =self.n.MORPH
self.disturb =self.n.DISTURB
self.agn1 =self.n.AGNKAUFF
self.agn2 =self.n.AGNKEWLEY
self.agn3 =self.n.AGNSTASIN
self.n2halpha=(self.mpan2/self.mpahalpha)
self.o3hbeta=(self.mpao3/self.mpahbeta)
self.logn2halpha=log10(self.mpan2/self.mpahalpha)
self.logo3hbeta=log10(self.mpao3/self.mpahbeta)
self.ellipseflag24 =self.n.ELLIPSEFLAG24
self.ellipseflagsdss =self.n.ELLIPSEFLAGSDSS
self.ellipseflag =self.n.ELLIPSEFLAG
#new SDSS fields that quantify radial extent of galaxy
self.sdssIsoAr =self.n.SDSSISOAR
self.sdssIsoBr =self.n.SDSSISOBR
self.sdssIsoPhir =self.n.SDSSISOPHIR
self.sdssIsoPhirErr =self.n.SDSSISOPHIERRR
self.sdssExpRadr =self.n.SDSSEXPRADR
self.sdssExpABr =self.n.SDSSEXPABR
self.sdssExpABrErr =self.n.SDSSEXPABRERR
self.sdssExpPhir =self.n.SDSSEXPPHIR
self.sdssExpPhirErr =self.n.SDSSEXPPHIERRR
self.sdssPetroMag=self.n.SDSSPETROMAG
self.sdssPetroMagr=self.sdssPetroMag[:,2]
self.sdssPetroRad=self.n.SDSSPETRORAD
self.sdssPetroRadr=self.sdssPetroRad[:,2]
self.sdssPetroR50=self.n.SDSSPETROR50
self.sdssPetroR50r=self.sdssPetroR50[:,2]
self.sdssPetroR90=self.n.SDSSPETROR90
self.sdssPetroR90r=self.sdssPetroR90[:,2]
#de-redened magnitudes
self.sdssdered=self.n.SDSSDERED
self.sdssumag=self.sdssdered[:,0]
self.sdssgmag=self.sdssdered[:,1]
self.sdssrmag=self.sdssdered[:,2]
self.sdssimag=self.sdssdered[:,3]
self.sdsszmag=self.sdssdered[:,4]
conv=4*pi*(self.cdcm**2)*1.e-6*1.e-23*(3.e8/24.e-6)/Lsol
print 'conversion from F24 to L24 = ',conv
self.L24_cl=array(self.sex24.FLUX_BEST*conv*mipsconv_MJysr_to_uJy,'d')
#self.L24_cl=array(t,'d')
self.L24err_cl=self.sex24.FLUXERR_BEST*conv*mipsconv_MJysr_to_uJy
self.Lir_cl=self.L24_cl*8.#approx conv from papovich
self.Lirerr_cl=self.L24err_cl*8.#approx conv from papovich
self.SFR24_cl=self.Lir_cl*4.5e-44*Lsol#approx conv from papovich
self.SFR24err_cl=self.Lirerr_cl*4.5e-44*Lsol#approx conv from papovich
#self.SFR24se_cl=(fluxautose24*141*conv)*8.*4.5e-44*Lsol#approx conv from papovich
#self.SFR24seerr_cl=(fluxerrautose24*141*conv)*8.*4.5e-44*Lsol#approx conv from papovich
#self.snr24se=abs(self.SFR24se_cl/self.SFR24seerr_cl)
#self.superSFR24_cl=self.SFR24_cl*apexflag+self.SFR24se_cl*(~apexflag&sex24flag)
#self.superSFR24err_cl=self.SFR24err_cl*apexflag+self.SFR24seerr_cl*(~apexflag&sex24flag)
#self.sSFR_cl=self.SFR24_cl/self.stellarmassr_cl
# other Lum and SFR
self.HImass=self.n.HIMASS
self.L24=self.n.L24
self.L24err=self.n.L24ERR
self.Lir=self.n.LIR
self.Lirerr=self.n.LIRERR
self.SFR24=self.n.SFR24
self.SFR24err=self.n.SFR24ERR
self.SuperSFR24=self.n.SUPERSFR24
self.SuperSFR24err=self.n.SUPERSFR24ERR
self.HImass_cl=self.n.HIMASS_CL
#self.L24_cl=self.n.L24_CL
#self.L24err_cl=self.n.L24ERR_CL
#self.Lir_cl=self.n.LIR_CL
#self.Lirerr_cl=self.n.LIRERR_CL
#self.SFR24_cl=self.n.SFR24_CL
#self.SFR24err_cl=self.n.SFR24ERR_CL
#self.SuperSFR24_cl=self.n.SUPERSFR24_CL
#self.SuperSFR24err_cl=self.n.SUPERSFR24ERR_CL
#define red, green and blue galaxies
ur=self.n.ABSMAG[:,2]-self.n.ABSMAG[:,4]
self.redflag=(ur > 2.3)
self.greenflag=(ur > 1.8) & (ur < 2.3)
self.blueflag=(ur<1.8)
#end of master table!
#self.spiralFlag=self.On24ImageFlag & self.galzooflag & self.ellipseflag & (self.galzoopcsdebiased > 0.6)
self.clustername=clustername
self.clusterra=clusterRA[clustername]
self.clusterdec=clusterDec[clustername]
self.dr=sqrt((self.ra-self.clusterra)**2+(self.dec-self.clusterdec)**2)
self.drR200=self.dr/self.r200deg
self.clustervel=clusterbiweightcenter[clustername]
self.clustersigma=clusterbiweightscale[clustername]
self.clustervmin=self.clustervel-3.*self.clustersigma
self.clustervmax=self.clustervel+3.*self.clustersigma
self.dist=sqrt((self.clusterra-self.ra)**2 + (self.clusterdec-self.dec)**2)
self.flagHI = (self.flux100 > 0.)
self.vopt=self.n.Z*3.e5
self.dv=abs(self.vopt-self.biweightvel)/self.biweightscale
#self.dvflag = ((self.vopt > self.clustervmin) & (self.vopt < self.clustervmax))
self.dvflag = (self.dv < 3.)
self.dist3d=sqrt(self.drR200**2 + (self.dv)**2)
self.membflag=self.dvflag & (self.drR200 < 1)
self.nmemb=len(self.dist[self.membflag & self.On24ImageFlag])
self.nfield=len(self.dist[self.On24ImageFlag])-self.nmemb
self.agcdict=dict((a,b) for a,b in zip(self.agcnumber,arange(len(self.agcnumber))))
self.nsadict=dict((a,b) for a,b in zip(self.n.NSAID,arange(len(self.n.NSAID))))
self.spiralflag=(self.zoo.p_cs > 0.6)
self.ellipticalflag=(self.zoo.p_el > 0.7)
# set spiral flag for galaxies that are clearly spiral but have zoo.p_cs < .6
slist=spiral_nozoo[self.prefix]
for i in slist:
self.spiralflag[self.nsadict[i]]=1
elist=elliptical_nozoo[self.prefix]
for i in elist:
self.ellipticalflag[self.nsadict[i]]=1
print self.clustername,": ","N members = ",self.nmemb," N field = ",self.nfield
#print ' N spirals = ',sum(self.spiralFlag),' Nspiral members = ',sum(self.spiralFlag&self.membflag)
print ' N spirals on 24um image = ',sum(self.spiralflag & self.On24ImageFlag),' Nspiral members = ',sum(self.spiralflag&self.membflag & self.On24ImageFlag)
print ' N galaxies on 24um image = ',sum(self.On24ImageFlag),' N members on 24um image = ',sum(self.membflag & self.On24ImageFlag)
#self.L24=zeros(len(self.mipsflux),'d')
#self.L24err=zeros(len(self.mipsflux),'d')
# calculate HI deficiency using Toribio et al 2011 results
# their relation is
# log(M_HI/Msun) = 8.72 + 1.25 log(D_25,r/kpc)
# and
# log D_25 = log D_25(obs) + beta log(b/a), where beta = 0.35 in r-band
# NOTE: SDSS isophotal radii are given in pixels!!!!
a=self.sdssIsoAr
b=self.sdssIsoBr
# convert from arcsec to kpc with self.AngDistance (which is in units of kpc/arcsec)
# multiply by 2 to convert from radius to diameter
# multiply by sdss pixel scale (0.39) b/c isophotal radii are given in pixels
self.D25obskpc=2.*self.sdssIsoAr*sdsspixelscale*self.AngDistanceCl
self.D25obskpcall=2.*self.sdssIsoAr*sdsspixelscale*self.AngDistanceAll
# apply correction from toribio et al 2011
self.logD25kpc=log10(self.D25obskpc) + 0.35*log10(b/a)
self.logD25kpcall=log10(self.D25obskpcall) + 0.35*log10(b/a)
# use toribio et al relation to predict the expected HI mass, including factor of 2 correction
self.HImassExpected = 10.**(8.72 + 1.25*(self.logD25kpc-log10(2.)))
self.HImassExpectedall = 10.**(8.72 + 1.25*(self.logD25kpcall-log10(2.)))
self.HImassExpFromMr=10.**(6.44-0.18*self.sdssMr)
self.HImassExpFromgr=10.**(8.84+1.81*(self.sdssgmag-self.sdssrmag))
# calculate deficiency as log expected - log observed
self.HIDef = log10(self.HImassExpected) - log10(self.HImass)
self.HIDef_zdist = log10(self.HImassExpectedall) - log10(self.HImass)
self.myHIDef = log10(self.HImassExpected -self.HImass)
# HI upper limit for clusters observed in alpha 40 sample (MKW11, A2052, A2063)
# M(HI lim) = 2.36e5 * d^2 (W50 * 20)^(1/2) sigma_rms * S/N lim
# W50 = W50,0 * sin(i)
# cos^2(i) = ((b/a)^2 - q^2)/(1-q^2)
# W50,0 = 100 km/s
# sigma rms = 10 km/s
# q = 0.32 for Sa
# q = 0.23 for Sab
# q = 0.18 for Sb-Sc (from Gavazzi et al 2013)
# assign upper limits for each galaxy based on its B/A
W50=70.
sigma_rms=2.1e-3
snlim=6.5
self.clHImass_ulim= 2.36e5*(self.cdMpc)**2*sqrt(W50*20.)*sigma_rms*snlim
self.HIDef_ulim=log10(self.HImassExpected)-log10(self.clHImass_ulim)
#self.agnflag=self.agn1#use Kauffmann et al 2003 cut
self.agnflag=self.agn2#use Kewley
self.irflag = self.apexflag & self.membflag
#set flag fot galaxies with dv < 3 sigma
writesdssradec=0
if writesdssradec:
# extra function for writing out RA and Dec to upload into SDSS query page
# http://skyserver.sdss3.org/dr9/en/tools/search/IQS.asp
offset=30./60.
outfile=homedir+'research/LocalClusters/NSAmastertables/RADecfiles/'+self.prefix+'_RADEC.csv'
out1=open(outfile,'w')
out1.write('ra, dec, sep \n')
for i in range(len(self.n.RA)):
out1.write('%12.8f, %12.8f, %12.8f \n'%(self.n.RA[i],self.n.DEC[i],offset))
out1.close
# calculate the angle between major axis and ellipse center
# call is clusterphi (see page in ResearchNotes.nb entitles 'Angle between galaxy's major axis and cluster center')
# in notes I call the angle psi, but a little too painful for a variable
# if cluster_phi = 90 - galaxy falling face-on into cluster
# if cluster_phi = 0 - galaxy falling edge-on into cluster
self.delta_dec=self.dec-self.cdec
self.delta_ra=self.ra-self.cra
r=sqrt(self.delta_dec**2+self.delta_ra**2)
self.theta=arctan(abs(self.delta_dec)/abs(self.delta_ra))*180./pi
self.cluster_phi=zeros(len(self.ra),'f')
#for i in range(len(self.ra)):
# if (self.delta_dec[i]*self.delta_ra[i] > 1.):
# self.cluster_phi[i] = abs(90.- self.n.SERSIC_PHI[i] + self.theta[i])
# else:
# self.cluster_phi[i] = abs(self.n.SERSIC_PHI[i] - 90. + self.theta[i])
phi=self.n.SERSIC_PHI/180.*pi # in radians
theta=self.theta/180.*pi
self.cluster_phi=arccos(abs(sin(phi)*-1.*cos(theta)+cos(phi)*sin(theta)))*180./pi
self.readsnr24NSA()
self.snr24flag=self.snr24 > 1.5
# define a blue flag based on NUV-r vs mass plot
color=self.n.ABSMAG[:,1]-self.n.ABSMAG[:,4]
self.NUVr_color=self.n.ABSMAG[:,1]-self.n.ABSMAG[:,4]
mag=log10(self.stellarmass)
self.blueflag = color < (.6*(mag-9)+3.3)
# define a blue flag based on NUV-r vs Mr plot
mag=self.n.ABSMAG[:,4]
#yb=1.73-0.17*xl-2.
self.blueflag = color < (1.73-0.17*mag-2.)
self.redflag = color > (1.73-0.17*mag-.5)
self.greenflag= (color > (1.73-0.17*mag-2.)) & (color < (1.73-0.17*mag-.5))
# 80% completeness
self.f80=clusterf80MJysr[self.prefix]*mipsconv_MJysr_to_uJy # in micro Jy
print self.biweightvel/3.e5,self.f80
self.Lir80,self.SFRir80=chary.chary_elbaz_24um(array([self.biweightvel/3.e5],'f'),array([self.f80],'f'))
#
best_distance=self.membflag * self.cdMpc + ~self.membflag*(self.n.ZDIST*3.e5/H0)
self.M24=self.sex24.MAG_BEST-25-5.*log10(best_distance)
self.M24zdist=self.sex24.MAG_BEST-25-5.*log10(self.n.ZDIST*3.e5/H0)
def __init__(self, clustername):
#Get current path so program can tell if this is being run on Becky or Rose's computer
self.prefix = clustername
self.john_prefix = john_prefix[self.prefix]
self.cra = clusterRA[self.prefix]
self.cdec = clusterDec[self.prefix]
self.cz = clusterz[self.prefix]
self.biweightvel = clusterbiweightcenter[self.prefix]
self.biweightscale = clusterbiweightscale[self.prefix]
self.r200 = 2.02 * (self.biweightscale) / 1000. / sqrt(
OmegaL + OmegaM * (1. + self.cz)**3) * H0 / 70. # in Mpc
self.r200deg = self.r200 * 1000. / my.DA(self.biweightvel / 3.e5,
h) / 3600.
self.cdMpc = self.biweightvel / H0
self.cdcm = self.cdMpc * 3.e24
self.csigma = self.biweightscale
self.mcl = my.clusterMass(self.biweightscale, self.biweightvel / 3.e5,
h)
self.cLx = clusterLx[self.prefix]
self.mingalaxysize = mingalaxysize_kpc / my.DA(self.biweightvel / 3.e5,
h)
#infile=homedir+'research/LocalClusters/NSAmastertables/'+clustername+'_NSAmastertable.fits'
infile = homedir + 'research/LocalClusters/NSAmastertables/NSAwithAGC/' + clustername + '_NSAmastertable_topcat.fits'
self.cutoutpath = homedir + 'research/LocalClusters/cutouts/' + self.prefix + '/'
#infile='/home/rfinn/LocalClusters/MasterTables/'+clustername+'mastertable.fits'
self.n = atpy.Table(infile)
infile = homedir + 'research/LocalClusters/NSAmastertables/' + clustername + '_NSAmastertable.fits'
self.nsa = atpy.Table(infile)
# read in WISE catalogs
infile = homedir + 'research/LocalClusters/NSAmastertables/WISETables/' + clustername + '_WISE_NSA.fits'
self.wise = atpy.Table(infile)
# read in Galaxy Zoo catalogs
infile = homedir + 'research/LocalClusters/NSAmastertables/GalaxyZooTables/' + clustername + '_GalaxyZoo.fits'
self.zoo = atpy.Table(infile)
#self.zooflag=self.zoo.zoo_match_flag | self.zoo.zoo_phot_match_flag
# read in GIM2D catalogs
infile = homedir + 'research/LocalClusters/NSAmastertables/SimardGIM2D/' + clustername + '_GIM2D.fits'
self.gim2d = atpy.Table(infile)
# fields with _1 are from bulge+disk; fields with _2 are from pure sersic fit
infile = homedir + 'research/LocalClusters/NSAmastertables/Sex24Tables/' + clustername + '_sex24.fits'
self.sex24 = atpy.Table(infile)
infile = homedir + 'research/LocalClusters/NSAmastertables/AGCTables/' + clustername + '_AGC.fits'
self.agc = atpy.Table(infile)
sersicparam24_file = homedir + 'research/LocalClusters/NSAmastertables/GalfitSersicResults/' + self.prefix + '_GalfitSersicParam_24.fits'
self.galfit24 = atpy.Table(sersicparam24_file)
infile = homedir + 'research/LocalClusters/NSAmastertables/LocalDensityTables/' + clustername + '_localdensity.fits'
self.ld = atpy.Table(infile)
infile = homedir + 'research/LocalClusters/NSAmastertables/CharyElbazTables/' + clustername + '_ce_lir.fits'
self.ce = atpy.Table(infile)
self.snrse = abs(self.ce.FLUX24 / self.ce.FLUX24ERR)
# read in John's Lir catalogs - for his members only
infile = homedir + 'research/LocalClusters/NSAmastertables/MoustakasLir/' + self.john_prefix + '_lir.fits'
self.lir = atpy.Table(infile, type='fits')
self.memb_id = self.lir.NSAID
# calculating magnitudes from fluxes provided from NSA
#
# m = 22.5 - 2.5 log_10 (flux_nanomaggies)
# from http://www.sdss3.org/dr8/algorithms/magnitudes.php#nmgy
self.nsamag = 22.5 - 2.5 * log10(self.n.NMGY)
self.sdssLr = 10.**(-1 * (self.n.ABSMAG[:, 4] - SolarMag['r']) / 2.5)
a, b = bellgr['r']
self.stellarmass = 10.**(
-1. * a + b *
(self.n.ABSMAG[:, 3] - self.n.ABSMAG[:, 4])) * self.sdssLr
self.sdssLu = 10.**(-1 * (self.n.ABSMAG[:, 2] - SolarMag['u']) / 2.5)
self.sdssLg = 10.**(-1 * (self.n.ABSMAG[:, 3] - SolarMag['g']) / 2.5)
self.sdssLi = 10.**(-1 * (self.n.ABSMAG[:, 5] - SolarMag['i']) / 2.5)
self.sdssLz = 10.**(-1 * (self.n.ABSMAG[:, 6] - SolarMag['z']) / 2.5)
self.AngDistanceCl = my.DA(self.cz, h)
self.AngDistanceAll = zeros(len(self.n.ZDIST), 'f')
for i in range(len(self.n.ZDIST)):
self.AngDistanceAll[i] = my.DA(self.n.ZDIST[i], h)
# FOR BACKWARDS COMPATABILITY WITH EXISTING CODE
# data from AGC-based mastertables
self.agcflag = self.agc.AGCMATCHFLAG
self.HIflag = (self.agc.FLUX100 > 0)
self.sdssflag = self.n.SDSSflag
self.sdssphotflag = self.n.SDSSphotflag
self.mpaflag = self.n.MPAFLAG
self.apexflag = self.n.APEXflag
self.sexsdssflag = self.n.SEXSDSSflag
self.sex24flag = self.n.SEX24FLAG
self.agcvoptflag = (self.agc.VOPT > 0)
self.agcnumber = self.agc.AGCNUMBER
self.raagc = self.agc.RA
self.decagc = self.agc.DEC
self.a100 = self.agc.A100
self.b100 = self.agc.B100
self.mag10 = self.agc.MAG10
self.posang = self.agc.POSANG
self.bsteintype = self.agc.BSTEINTYPE
self.vopt = self.agc.VOPT
self.verr = self.agc.VERR
self.vsource = self.agc.VSOURCE
self.flux100 = self.agc.FLUX100
self.rms100 = self.agc.RMS100
self.v21 = self.agc.V21
self.width = self.agc.WIDTH
self.widtherr = self.agc.WIDTHERR
#sdss info
self.sdssra = self.n.SDSSRA
self.sdssdec = self.n.SDSSDEC
self.sdssphotra = self.n.SDSSphotRA
self.sdssphotdec = self.n.SDSSphotDEC
self.sdssmag = self.n.SDSSMAG
self.sdssu = self.sdssmag[:, 0]
self.sdssg = self.sdssmag[:, 1]
self.sdssr = self.sdssmag[:, 2]
self.sdssi = self.sdssmag[:, 3]
self.sdssz = self.sdssmag[:, 4]
self.sdssmagerr = self.n.SDSSMAGERR
self.sdssuerr = self.sdssmagerr[:, 0]
self.sdssgerr = self.sdssmagerr[:, 1]
self.sdssrerr = self.sdssmagerr[:, 2]
self.sdssierr = self.sdssmagerr[:, 3]
self.sdsszerr = self.sdssmagerr[:, 4]
self.sdssspecz = self.n.SDSSSPECZ
self.sdssvopt = self.n.SDSSVOPT
self.sdsshaew = self.n.SDSSHAEW
self.sdsshaewerr = self.n.SDSSHAEWERR
self.sdssplate = self.n.SDSSPLATE
self.sdssfiberid = self.n.SDSSFIBERID
self.sdsstile = self.n.SDSSTILE
self.sdssrun = self.n.SDSSRUN
self.sdssrerun = self.n.SDSSRERUN
self.sdsscamcol = self.n.SDSSCAMCOL
self.sdssfield = self.n.SDSSFIELD
self.mpahalpha = self.n.MPAHALPHA
self.mpahbeta = self.n.MPAHBETA
self.mpao3 = self.n.MPAOIII
self.mpan2 = self.n.MPANII
#sextractor info
self.numberser = self.n.NUMBERSER
self.ximageser = self.n.XIMAGESER
self.yimageser = self.n.YIMAGESER
self.xminimageser = self.n.XMINIMAGESER
self.xmaximageser = self.n.XMAXIMAGESER
self.yminimageser = self.n.YMINIMAGESER
self.raser = self.n.RASER
self.decser = self.n.DECSER
self.fluxisoser = self.n.FLUXISOSER
self.fluxerrisoser = self.n.FLUXERRISOSER
self.magisoser = self.n.MAGISOSER
self.magerrisoser = self.n.MAGERRISOSER
self.fluxautoser = self.n.FLUXAUTOSER
self.fluxerrautoser = self.n.FLUXERRAUTOSER
self.magautoser = self.n.MAGAUTOSER
self.magerrautoser = self.n.MAGERRAUTOSER
self.fluxpetroser = self.n.FLUXPETROSER
self.fluxerrpetroser = self.n.FLUXERRPETROSER
self.magpetroser = self.n.MAGPETROSER
self.magerrpetroser = self.n.MAGERRPETROSER
self.kronradser = self.n.KRONRADSER #kron radius
self.petroradser = self.n.PETRORADSER #petrosian radius
self.fluxradser = self.n.FLUXRADSER #1/2 light radius
self.isoareaser = self.n.ISOAREASER
self.aworldser = self.n.AWORLDSER
self.bworldser = self.n.BWORLDSER
self.thetaser = self.n.THETASER
self.errthetaser = self.n.ERRTHETASER
self.thetaj2000ser = self.n.THETAJ2000SER
self.errthetaj2000ser = self.n.ERRTHETAJ2000SER
self.elongser = self.n.ELONGATIONSER
self.elliptser = self.n.ELLIPTICITYSER
self.fwhmser = self.n.FWHMSER
self.flagsser = self.n.FLAGSSER
self.classstarser = self.n.CLASSSTARSER
#SEXTRACTOR output 24 micron data
self.numberse24 = self.n.NUMBERSE24
self.ximagese24 = self.n.XIMAGESE24
self.yimagese24 = self.n.YIMAGESE24
self.xminimagese24 = self.n.XMINIMAGESE24
self.xmaximagese24 = self.n.XMAXIMAGESE24
self.xminimagese24 = self.n.YMINIMAGESE24
self.rase24 = self.n.RASE24
self.decse24 = self.n.DECSE24
self.fluxisose24 = self.n.FLUXISOSE24
self.fluxerrisose24 = self.n.FLUXERRISOSE24
self.magisose24 = self.n.MAGISOSE24
self.magerrisose24 = self.n.MAGERRISOSE24
self.fluxautose24 = self.n.FLUXAUTOSE24
self.fluxerrautose24 = self.n.FLUXERRAUTOSE24
self.magautose24 = self.n.MAGAUTOSE24
self.magerrautose24 = self.n.MAGERRAUTOSE24
self.fluxpetrose24 = self.n.FLUXPETROSE24
self.fluxerrpetrose24 = self.n.FLUXERRPETROSE24
self.magpetrose24 = self.n.MAGPETROSE24
self.magerrpetrose24 = self.n.MAGERRPETROSE24
self.kronradse24 = self.n.KRONRADSE24
self.petroradse24 = self.n.PETRORADSE24
self.fluxradse24 = self.n.FLUXRADSE24
self.isoarease24 = self.n.ISOAREASE24
self.aworldse24 = self.n.AWORLDSE24
self.bworldse24 = self.n.BWORLDSE24
self.thetase24 = self.n.THETASE24
self.errthetase24 = self.n.ERRTHETASE24
self.thetaj2000se24 = self.n.THETAJ2000SE24
self.errthetaj2000se24 = self.n.ERRTHETAJ2000SE24
self.elongse24 = self.n.ELONGATIONSE24
self.elliptse24 = self.n.ELLIPTICITYSE24
self.fwhmse24 = self.n.FWHMSE24
self.flagsse24 = self.n.FLAGSSE24
self.classstarse24 = self.n.CLASSSTARSE24
self.f24dist = self.fluxautose24[self.sex24flag]
#apex output
self.mipsra = self.n.MIPSRA
self.mipsdec = self.n.MIPSDEC
self.mipsflux = self.n.MIPSFLUX
self.mipsfluxerr = self.n.MIPSFLUXERR
self.mipssnr = self.n.MIPSSNR
self.mipsdeblend = self.n.MIPSDEBLEND
self.mipsfluxap1 = self.n.MIPSFLUXAP1
self.mipsfluxap1err = self.n.MIPSFLUXAP1ERR
self.mipsfluxap2 = self.n.MIPSFLUXAP2
self.mipsfluxap2err = self.n.MIPSFLUXAP2ERR
self.mipsfluxap3 = self.n.MIPSFLUXAP3
self.mipsfluxap4err = self.n.MIPSFLUXAP3ERR
self.On24ImageFlag_AGC = self.n.On24ImageFlag_2
self.On24ImageFlag = self.n.On24ImageFlag_1
self.supervopt = self.n.SUPERVOPT
self.ra = self.n.RA
self.dec = self.n.DEC
#self.stellarmass=self.n.STELLARMASS
#self.stellarmass_cl=self.n.STELLARMASS_CL
self.sdssabsmag = self.n.SDSSABSMAG
self.sdssMu = self.sdssabsmag[:, 0]
self.sdssMg = self.sdssabsmag[:, 1]
self.sdssMr = self.sdssabsmag[:, 2]
self.sdssMi = self.sdssabsmag[:, 3]
self.sdssMz = self.sdssabsmag[:, 4]
self.sdsslum = self.n.SDSSLUM
self.sdssLu = self.sdsslum[:, 0]
self.sdssLg = self.sdsslum[:, 1]
self.sdssLr = self.sdsslum[:, 2]
self.sdssLi = self.sdsslum[:, 3]
self.sdssLz = self.sdsslum[:, 4]
self.sdssabsmag_cl = self.n.SDSSABSMAG_CL
self.sdssMu = self.sdssabsmag_cl[:, 0]
self.sdssMg = self.sdssabsmag_cl[:, 1]
self.sdssMr = self.sdssabsmag_cl[:, 2]
self.sdssMi = self.sdssabsmag_cl[:, 3]
self.sdssMz = self.sdssabsmag_cl[:, 4]
self.sdsslum_cl = self.n.SDSSLUM_CL
self.sdssLu_cl = self.sdsslum_cl[:, 0]
self.sdssLg_cl = self.sdsslum_cl[:, 1]
self.sdssLr_cl = self.sdsslum_cl[:, 2]
self.sdssLi_cl = self.sdsslum_cl[:, 3]
self.sdssLz_cl = self.sdsslum_cl[:, 4]
self.sdsscolc = self.n.SDSSCOLC
self.sdssrowc = self.n.SDSSROWC
self.membflag = self.n.MEMBFLAG
self.morphflag = self.n.MORPHFLAG
self.morph = self.n.MORPH
self.disturb = self.n.DISTURB
self.agn1 = self.n.AGNKAUFF
self.agn2 = self.n.AGNKEWLEY
self.agn3 = self.n.AGNSTASIN
self.n2halpha = (self.mpan2 / self.mpahalpha)
self.o3hbeta = (self.mpao3 / self.mpahbeta)
self.logn2halpha = log10(self.mpan2 / self.mpahalpha)
self.logo3hbeta = log10(self.mpao3 / self.mpahbeta)
self.ellipseflag24 = self.n.ELLIPSEFLAG24
self.ellipseflagsdss = self.n.ELLIPSEFLAGSDSS
self.ellipseflag = self.n.ELLIPSEFLAG
#new SDSS fields that quantify radial extent of galaxy
self.sdssIsoAr = self.n.SDSSISOAR
self.sdssIsoBr = self.n.SDSSISOBR
self.sdssIsoPhir = self.n.SDSSISOPHIR
self.sdssIsoPhirErr = self.n.SDSSISOPHIERRR
self.sdssExpRadr = self.n.SDSSEXPRADR
self.sdssExpABr = self.n.SDSSEXPABR
self.sdssExpABrErr = self.n.SDSSEXPABRERR
self.sdssExpPhir = self.n.SDSSEXPPHIR
self.sdssExpPhirErr = self.n.SDSSEXPPHIERRR
self.sdssPetroMag = self.n.SDSSPETROMAG
self.sdssPetroMagr = self.sdssPetroMag[:, 2]
self.sdssPetroRad = self.n.SDSSPETRORAD
self.sdssPetroRadr = self.sdssPetroRad[:, 2]
self.sdssPetroR50 = self.n.SDSSPETROR50
self.sdssPetroR50r = self.sdssPetroR50[:, 2]
self.sdssPetroR90 = self.n.SDSSPETROR90
self.sdssPetroR90r = self.sdssPetroR90[:, 2]
#de-redened magnitudes
self.sdssdered = self.n.SDSSDERED
self.sdssumag = self.sdssdered[:, 0]
self.sdssgmag = self.sdssdered[:, 1]
self.sdssrmag = self.sdssdered[:, 2]
self.sdssimag = self.sdssdered[:, 3]
self.sdsszmag = self.sdssdered[:, 4]
conv = 4 * pi * (self.cdcm**
2) * 1.e-6 * 1.e-23 * (3.e8 / 24.e-6) / Lsol
print 'conversion from F24 to L24 = ', conv
self.L24_cl = array(
self.sex24.FLUX_BEST * conv * mipsconv_MJysr_to_uJy, 'd')
#self.L24_cl=array(t,'d')
self.L24err_cl = self.sex24.FLUXERR_BEST * conv * mipsconv_MJysr_to_uJy
self.Lir_cl = self.L24_cl * 8. #approx conv from papovich
self.Lirerr_cl = self.L24err_cl * 8. #approx conv from papovich
self.SFR24_cl = self.Lir_cl * 4.5e-44 * Lsol #approx conv from papovich
self.SFR24err_cl = self.Lirerr_cl * 4.5e-44 * Lsol #approx conv from papovich
#self.SFR24se_cl=(fluxautose24*141*conv)*8.*4.5e-44*Lsol#approx conv from papovich
#self.SFR24seerr_cl=(fluxerrautose24*141*conv)*8.*4.5e-44*Lsol#approx conv from papovich
#self.snr24se=abs(self.SFR24se_cl/self.SFR24seerr_cl)
#self.superSFR24_cl=self.SFR24_cl*apexflag+self.SFR24se_cl*(~apexflag&sex24flag)
#self.superSFR24err_cl=self.SFR24err_cl*apexflag+self.SFR24seerr_cl*(~apexflag&sex24flag)
#self.sSFR_cl=self.SFR24_cl/self.stellarmassr_cl
# other Lum and SFR
self.HImass = self.n.HIMASS
self.L24 = self.n.L24
self.L24err = self.n.L24ERR
self.Lir = self.n.LIR
self.Lirerr = self.n.LIRERR
self.SFR24 = self.n.SFR24
self.SFR24err = self.n.SFR24ERR
self.SuperSFR24 = self.n.SUPERSFR24
self.SuperSFR24err = self.n.SUPERSFR24ERR
self.HImass_cl = self.n.HIMASS_CL
#self.L24_cl=self.n.L24_CL
#self.L24err_cl=self.n.L24ERR_CL
#self.Lir_cl=self.n.LIR_CL
#self.Lirerr_cl=self.n.LIRERR_CL
#self.SFR24_cl=self.n.SFR24_CL
#self.SFR24err_cl=self.n.SFR24ERR_CL
#self.SuperSFR24_cl=self.n.SUPERSFR24_CL
#self.SuperSFR24err_cl=self.n.SUPERSFR24ERR_CL
#define red, green and blue galaxies
ur = self.n.ABSMAG[:, 2] - self.n.ABSMAG[:, 4]
self.redflag = (ur > 2.3)
self.greenflag = (ur > 1.8) & (ur < 2.3)
self.blueflag = (ur < 1.8)
#end of master table!
#self.spiralFlag=self.On24ImageFlag & self.galzooflag & self.ellipseflag & (self.galzoopcsdebiased > 0.6)
self.clustername = clustername
self.clusterra = clusterRA[clustername]
self.clusterdec = clusterDec[clustername]
self.dr = sqrt((self.ra - self.clusterra)**2 +
(self.dec - self.clusterdec)**2)
self.drR200 = self.dr / self.r200deg
self.clustervel = clusterbiweightcenter[clustername]
self.clustersigma = clusterbiweightscale[clustername]
self.clustervmin = self.clustervel - 3. * self.clustersigma
self.clustervmax = self.clustervel + 3. * self.clustersigma
self.dist = sqrt((self.clusterra - self.ra)**2 +
(self.clusterdec - self.dec)**2)
self.flagHI = (self.flux100 > 0.)
self.vopt = self.n.Z * 3.e5
self.dv = abs(self.vopt - self.biweightvel) / self.biweightscale
#self.dvflag = ((self.vopt > self.clustervmin) & (self.vopt < self.clustervmax))
self.dvflag = (self.dv < 3.)
self.dist3d = sqrt(self.drR200**2 + (self.dv)**2)
self.membflag = self.dvflag & (self.drR200 < 1)
self.nmemb = len(self.dist[self.membflag & self.On24ImageFlag])
self.nfield = len(self.dist[self.On24ImageFlag]) - self.nmemb
self.agcdict = dict(
(a, b)
for a, b in zip(self.agcnumber, arange(len(self.agcnumber))))
self.nsadict = dict(
(a, b) for a, b in zip(self.n.NSAID, arange(len(self.n.NSAID))))
self.spiralflag = (self.zoo.p_cs > 0.6)
self.ellipticalflag = (self.zoo.p_el > 0.7)
# set spiral flag for galaxies that are clearly spiral but have zoo.p_cs < .6
slist = spiral_nozoo[self.prefix]
for i in slist:
self.spiralflag[self.nsadict[i]] = 1
elist = elliptical_nozoo[self.prefix]
for i in elist:
self.ellipticalflag[self.nsadict[i]] = 1
print self.clustername, ": ", "N members = ", self.nmemb, " N field = ", self.nfield
#print ' N spirals = ',sum(self.spiralFlag),' Nspiral members = ',sum(self.spiralFlag&self.membflag)
print ' N spirals on 24um image = ', sum(
self.spiralflag & self.On24ImageFlag), ' Nspiral members = ', sum(
self.spiralflag & self.membflag & self.On24ImageFlag)
print ' N galaxies on 24um image = ', sum(
self.On24ImageFlag), ' N members on 24um image = ', sum(
self.membflag & self.On24ImageFlag)
#self.L24=zeros(len(self.mipsflux),'d')
#self.L24err=zeros(len(self.mipsflux),'d')
# calculate HI deficiency using Toribio et al 2011 results
# their relation is
# log(M_HI/Msun) = 8.72 + 1.25 log(D_25,r/kpc)
# and
# log D_25 = log D_25(obs) + beta log(b/a), where beta = 0.35 in r-band
# NOTE: SDSS isophotal radii are given in pixels!!!!
a = self.sdssIsoAr
b = self.sdssIsoBr
# convert from arcsec to kpc with self.AngDistance (which is in units of kpc/arcsec)
# multiply by 2 to convert from radius to diameter
# multiply by sdss pixel scale (0.39) b/c isophotal radii are given in pixels
self.D25obskpc = 2. * self.sdssIsoAr * sdsspixelscale * self.AngDistanceCl
self.D25obskpcall = 2. * self.sdssIsoAr * sdsspixelscale * self.AngDistanceAll
# apply correction from toribio et al 2011
self.logD25kpc = log10(self.D25obskpc) + 0.35 * log10(b / a)
self.logD25kpcall = log10(self.D25obskpcall) + 0.35 * log10(b / a)
# use toribio et al relation to predict the expected HI mass, including factor of 2 correction
self.HImassExpected = 10.**(8.72 + 1.25 * (self.logD25kpc - log10(2.)))
self.HImassExpectedall = 10.**(8.72 + 1.25 *
(self.logD25kpcall - log10(2.)))
self.HImassExpFromMr = 10.**(6.44 - 0.18 * self.sdssMr)
self.HImassExpFromgr = 10.**(8.84 + 1.81 *
(self.sdssgmag - self.sdssrmag))
# calculate deficiency as log expected - log observed
self.HIDef = log10(self.HImassExpected) - log10(self.HImass)
self.HIDef_zdist = log10(self.HImassExpectedall) - log10(self.HImass)
self.myHIDef = log10(self.HImassExpected - self.HImass)
# HI upper limit for clusters observed in alpha 40 sample (MKW11, A2052, A2063)
# M(HI lim) = 2.36e5 * d^2 (W50 * 20)^(1/2) sigma_rms * S/N lim
# W50 = W50,0 * sin(i)
# cos^2(i) = ((b/a)^2 - q^2)/(1-q^2)
# W50,0 = 100 km/s
# sigma rms = 10 km/s
# q = 0.32 for Sa
# q = 0.23 for Sab
# q = 0.18 for Sb-Sc (from Gavazzi et al 2013)
# assign upper limits for each galaxy based on its B/A
W50 = 70.
sigma_rms = 2.1e-3
snlim = 6.5
self.clHImass_ulim = 2.36e5 * (self.cdMpc)**2 * sqrt(
W50 * 20.) * sigma_rms * snlim
self.HIDef_ulim = log10(self.HImassExpected) - log10(
self.clHImass_ulim)
#self.agnflag=self.agn1#use Kauffmann et al 2003 cut
self.agnflag = self.agn2 #use Kewley
self.irflag = self.apexflag & self.membflag
#set flag fot galaxies with dv < 3 sigma
writesdssradec = 0
if writesdssradec:
# extra function for writing out RA and Dec to upload into SDSS query page
# http://skyserver.sdss3.org/dr9/en/tools/search/IQS.asp
offset = 30. / 60.
outfile = homedir + 'research/LocalClusters/NSAmastertables/RADecfiles/' + self.prefix + '_RADEC.csv'
out1 = open(outfile, 'w')
out1.write('ra, dec, sep \n')
for i in range(len(self.n.RA)):
out1.write('%12.8f, %12.8f, %12.8f \n' %
(self.n.RA[i], self.n.DEC[i], offset))
out1.close
# calculate the angle between major axis and ellipse center
# call is clusterphi (see page in ResearchNotes.nb entitles 'Angle between galaxy's major axis and cluster center')
# in notes I call the angle psi, but a little too painful for a variable
# if cluster_phi = 90 - galaxy falling face-on into cluster
# if cluster_phi = 0 - galaxy falling edge-on into cluster
self.delta_dec = self.dec - self.cdec
self.delta_ra = self.ra - self.cra
r = sqrt(self.delta_dec**2 + self.delta_ra**2)
self.theta = arctan(
abs(self.delta_dec) / abs(self.delta_ra)) * 180. / pi
self.cluster_phi = zeros(len(self.ra), 'f')
#for i in range(len(self.ra)):
# if (self.delta_dec[i]*self.delta_ra[i] > 1.):
# self.cluster_phi[i] = abs(90.- self.n.SERSIC_PHI[i] + self.theta[i])
# else:
# self.cluster_phi[i] = abs(self.n.SERSIC_PHI[i] - 90. + self.theta[i])
phi = self.n.SERSIC_PHI / 180. * pi # in radians
theta = self.theta / 180. * pi
self.cluster_phi = arccos(
abs(sin(phi) * -1. * cos(theta) +
cos(phi) * sin(theta))) * 180. / pi
self.readsnr24NSA()
self.snr24flag = self.snr24 > 1.5
# define a blue flag based on NUV-r vs mass plot
color = self.n.ABSMAG[:, 1] - self.n.ABSMAG[:, 4]
self.NUVr_color = self.n.ABSMAG[:, 1] - self.n.ABSMAG[:, 4]
mag = log10(self.stellarmass)
self.blueflag = color < (.6 * (mag - 9) + 3.3)
# define a blue flag based on NUV-r vs Mr plot
mag = self.n.ABSMAG[:, 4]
#yb=1.73-0.17*xl-2.
self.blueflag = color < (1.73 - 0.17 * mag - 2.)
self.redflag = color > (1.73 - 0.17 * mag - .5)
self.greenflag = (color > (1.73 - 0.17 * mag - 2.)) & (
color < (1.73 - 0.17 * mag - .5))
# 80% completeness
self.f80 = clusterf80MJysr[
self.prefix] * mipsconv_MJysr_to_uJy # in micro Jy
print self.biweightvel / 3.e5, self.f80
self.Lir80, self.SFRir80 = chary.chary_elbaz_24um(
array([self.biweightvel / 3.e5], 'f'), array([self.f80], 'f'))
#
best_distance = self.membflag * self.cdMpc + ~self.membflag * (
self.n.ZDIST * 3.e5 / H0)
self.M24 = self.sex24.MAG_BEST - 25 - 5. * log10(best_distance)
self.M24zdist = self.sex24.MAG_BEST - 25 - 5. * log10(
self.n.ZDIST * 3.e5 / H0)
def __init__(self, prefix):
self.prefix = prefix
self.fullname = fullname[self.prefix]
self.cra = racenter[self.prefix]
self.cdec = deccenter[self.prefix]
self.cz = redshift[self.prefix]
self.f80 = F80[self.prefix]
self.errf80 = ErrorF80[self.prefix]
self.csigma = sigma[self.prefix]
self.csigmaerrplus = errsigmaplus[self.prefix]
self.csigmaerrminus = errsigmaminus[self.prefix]
self.r200 = 2.02 * (
self.csigma) / 1000. / sqrt(OmegaL + OmegaM *
(1. + self.cz)**3) * H0 / 70. # in Mpc
if self.r200 < .5:
print 'WARNING: R200 unrealistically small for ', self.prefix
print 'resetting R200 to 0.5 Mpc'
self.r200 = .5
self.r200deg = self.r200 * 1000. / my.DA(self.cz, h) / 3600.
self.mcl = my.clusterMass(self.csigma, self.cz, h)
mastertable = mastertablepath + self.fullname + 'mastertable.fits'
tb = pyfits.open(mastertable)
tbdata = tb[1].data
tb.close()
self.ediscsID = tbdata.field('EDISCS-ID')
self.ediscsIDold = tbdata.field('EDISCS-ID-OLD')
self.ra = tbdata.field('RA')
self.dec = tbdata.field('DEC')
self.xcorr = tbdata.field('xcorr')
self.ycorr = tbdata.field('ycorr')
self.starflag = tbdata.field('starflag')
self.EW = tbdata.field('EW')
self.EWerr = tbdata.field('EWerr')
self.SFR = tbdata.field('SFR')
self.SFRerr = tbdata.field('SFRerr')
self.matchflaghalpha = tbdata.field('matchflaghalpha')
self.onHaimageflag = tbdata.field('onHaimageflag')
self.sfflag = tbdata.field('sfflag')
self.matchflag24 = tbdata.field('matchflag24')
self.on24imageflag = tbdata.field('on24imageflag')
self.flux24 = tbdata.field('flux24')
self.flux24err = tbdata.field('flux24err')
self.nmatchediscs24 = tbdata.field('nmatchediscs24')
self.snr24 = tbdata.field('snr24')
self.imagex24 = tbdata.field('imagex24')
self.imagey24 = tbdata.field('imagey24')
self.ra24 = tbdata.field('ra24')
self.dec24 = tbdata.field('dec24')
self.flux80flag = tbdata.field('flux80flag')
self.L24 = tbdata.field('L24')
self.L24err = tbdata.field('L24err')
self.Lir = tbdata.field('Lir')
self.errLir = tbdata.field('errLir')
self.SFRir = tbdata.field('SFRir')
self.SFRirerr = tbdata.field('SFRirerr')
self.matchflagediscsirac = tbdata.field('matchflagediscsirac')
self.iracf1 = tbdata.field('iracf1')
self.iracf2 = tbdata.field('iracf2')
self.iracf3 = tbdata.field('iracf3')
self.iracf4 = tbdata.field('iracf4')
self.erriracf1 = tbdata.field('erriracf1')
self.erriracf2 = tbdata.field('erriracf2')
self.erriracf3 = tbdata.field('erriracf3')
self.erriracf4 = tbdata.field('erriracf4')
self.iracsexflag0 = tbdata.field('iracsexflag0')
self.iracsexflag1 = tbdata.field('iracsexflag1')
self.iracwch1 = tbdata.field('iracwch1')
self.iracwch2 = tbdata.field('iracwch2')
self.iracwch3 = tbdata.field('iracwch3')
self.iracwch4 = tbdata.field('iracwch4')
self.iracwmin = tbdata.field('iracwmin')
self.nmatchediscsirac = tbdata.field('nmatchediscsirac')
self.matchflagmorphgimtype = tbdata.field('matchflagmorphgimtype')
self.gimtype = tbdata.field('gimtype')
self.matchflagvistype = tbdata.field('matchflagvistype')
self.vistype = tbdata.field('vistype')
self.misoV = tbdata.field('misoV')
self.misoeVapsim = tbdata.field('misoeVapsim')
self.misoR = tbdata.field('misoR')
self.misoeRapsim = tbdata.field('misoeRapsim')
self.misoI = tbdata.field('misoI')
self.misoeIapsim = tbdata.field('misoeIapsim')
self.misoJ = tbdata.field('misoJ')
self.misoeJapsim = tbdata.field('misoeJapsim')
self.misoK = tbdata.field('misoK')
self.misoeKapsim = tbdata.field('misoeKapsim')
self.magV = tbdata.field('magV')
self.mageVapsim = tbdata.field('mageVapsim')
self.magR = tbdata.field('magR')
self.mageRapsim = tbdata.field('mageRapsim')
self.magI = tbdata.field('magI')
self.mageIapsim = tbdata.field('mageIapsim')
self.magJ = tbdata.field('magJ')
self.mageJapsim = tbdata.field('mageJapsim')
self.magK = tbdata.field('magK')
self.mageKapsim = tbdata.field('mageKapsim')
self.membflag = tbdata.field('membflag')
self.newspecmatchflag = tbdata.field('newspecmatchflag')
self.defmembflag = tbdata.field('defmembflag')
self.photmembflag = tbdata.field('photmembflag')
self.supermembflag = tbdata.field('supermembflag')
self.specz = tbdata.field('specz')
self.spectype = tbdata.field('spectype')
self.specEWOII = tbdata.field('specEWOII')
self.matchflagspecediscs = tbdata.field('matchflagspecediscs')
self.specEWOIIflag = tbdata.field('specEWOIIflag')
self.bestz = tbdata.field('bestz')
self.lowz = tbdata.field('lowz')
self.highz = tbdata.field('highz')
self.wmin = tbdata.field('wmin')
self.Pclust = tbdata.field('Pclust')
self.MR = tbdata.field('MR')
self.MU = tbdata.field('MU')
self.MV = tbdata.field('MV')
self.MB = tbdata.field('MB')
self.stellarmass = tbdata.field('stellmass')
self.redflag = tbdata.field('redflag')
self.LUlowzclust = tbdata.field('LUlowzclust')
self.LUbestzclust = tbdata.field('LUbestzclust')
self.LUhighzclust = tbdata.field('LUhighzclust')
self.LBlowzclust = tbdata.field('LBlowzclust')
self.LBbestzclust = tbdata.field('LBbestzclust')
self.LBhighzclust = tbdata.field('LBhighzclust')
self.LVlowzclust = tbdata.field('LVlowzclust ')
self.LVbestzclust = tbdata.field('LVbestzclust')
self.LVhighzclust = tbdata.field('LVhighzclust')
self.LRlowzclust = tbdata.field('LRlowzclust')
self.LRbestzclust = tbdata.field('LRbestzclust')
self.LRhighzclust = tbdata.field('LRhighzclust')
self.LIlowzclust = tbdata.field('LIlowzclust')
self.LIbestzclust = tbdata.field('LIbestzclust')
self.LIhighzclust = tbdata.field('LIhighzclust')
self.LJlowzclust = tbdata.field('LJlowzclust')
self.LJbestzclust = tbdata.field('LJbestzclust')
self.LJhighzclust = tbdata.field('LJhighzclust')
self.LKlowzclust = tbdata.field('LKlowzclust')
self.LKbestzclust = tbdata.field('LKbestzclust')
self.LKhighzclust = tbdata.field('LKhighzclust')
# some extra quantities that are not included in the mastertable
dr = sqrt((self.ra - self.cra)**2 + (self.dec - self.cdec)**2)
self.drflag = (dr < self.r200deg)
def __init__(self,clustername):
#Get current path so program can tell if this is being run on Becky or Rose's computer
self.prefix=clustername
self.cra=clusterRA[self.prefix]
self.cdec=clusterDec[self.prefix]
self.cz=clusterz[self.prefix]
self.biweightvel=clustercbi[self.prefix]
self.biweightscale=clustersbi[self.prefix]
self.r200=2.02*(self.biweightscale)/1000./sqrt(OmegaL+OmegaM*(1.+self.cz)**3)*H0/70. # in Mpc
self.r200deg=self.r200*1000./my.DA(self.cz,h)/3600.
self.cdMpc=self.biweightvel/H0
self.cdcm=self.cdMpc*3.e24
self.csigma=self.biweightscale
self.mcl=my.clusterMass(self.csigma,self.cz,h)
self.AngDistance=my.DA(self.cz,h)
mypath=os.getcwd()
if mypath.find('Users') > -1:
print "Running on Rose's mac pro"
infile='/Users/rfinn/research/LocalClusters/MasterTables/'+clustername+'mastertable.fits'
homedir='/Users/rfinn/'
elif mypath.find('home') > -1:
print "Running on coma"
infile='/home/rfinn/research/LocalClusters/MasterTables/'+clustername+'mastertable.fits'
homedir='/home/rfinn/'
self.cutoutpath=homedir+'research/LocalClusters/cutouts/'+self.prefix+'/'
#infile='/home/rfinn/LocalClusters/MasterTables/'+clustername+'mastertable.fits'
tb=pyfits.open(infile)
tbdata=tb[1].data
tb.close()
self.agcflag=tbdata.field('AGCflag')
self.HIflag=tbdata.field('HIFLAG')
self.sdssflag=tbdata.field('SDSSflag')
self.sdssphotflag=tbdata.field('SDSSphotflag')
self.mpaflag=tbdata.field('MPAFLAG')
self.apexflag=tbdata.field('APEXFLAG')
self.sexsdssflag=tbdata.field('SEXSDSSflag')
self.sex24flag=tbdata.field('SEX24FLAG')
self.agcvoptflag=tbdata.field('AGCVOPTFLAG')
self.agcnumber=tbdata.field('AGCNUMBER')
self.raagc=tbdata.field('AGCRA')
self.decagc=tbdata.field('AGCDEC')
self.a100=tbdata.field('A100')
self.b100=tbdata.field('B100')
self.mag10=tbdata.field('MAG10')
self.posang=tbdata.field('POSANG')
self.bsteintype=tbdata.field('BSTEINTYPE')
self.vopt=tbdata.field('VOPT')
self.verr=tbdata.field('VERR')
self.vsource=tbdata.field('VSOURCE')
self.flux100=tbdata.field('FLUX100')
self.rms100=tbdata.field('RMS100')
self.v21=tbdata.field('V21')
self.width=tbdata.field('WIDTH')
self.widtherr=tbdata.field('WIDTHERR')
#sdss info
self.sdssra=tbdata.field('SDSSRA')
self.sdssdec=tbdata.field('SDSSDEC')
self.sdssphotra=tbdata.field('SDSSphotRA')
self.sdssphotdec=tbdata.field('SDSSphotDEC')
self.sdssmag=tbdata.field('SDSSMAG')
self.sdssu=self.sdssmag[:,0]
self.sdssg=self.sdssmag[:,1]
self.sdssr=self.sdssmag[:,2]
self.sdssi=self.sdssmag[:,3]
self.sdssz=self.sdssmag[:,4]
self.sdssmagerr=tbdata.field('SDSSMAGERR')
self.sdssuerr=self.sdssmagerr[:,0]
self.sdssgerr=self.sdssmagerr[:,1]
self.sdssrerr=self.sdssmagerr[:,2]
self.sdssierr=self.sdssmagerr[:,3]
self.sdsszerr=self.sdssmagerr[:,4]
self.sdssspecz=tbdata.field('SDSSSPECZ')
self.sdssvopt=tbdata.field('SDSSVOPT')
self.sdsshaew=tbdata.field('SDSSHAEW')
self.sdsshaewerr=tbdata.field('SDSSHAEWERR')
self.sdssplate=tbdata.field('SDSSPLATE')
self.sdssfiberid=tbdata.field('SDSSFIBERID')
self.sdsstile=tbdata.field('SDSSTILE')
self.sdssrun=tbdata.field('SDSSRUN')
self.sdssrerun=tbdata.field('SDSSRERUN')
self.sdsscamcol=tbdata.field('SDSSCAMCOL')
self.sdssfield=tbdata.field('SDSSFIELD')
self.mpahalpha=tbdata.field('MPAHALPHA')
self.mpahbeta=tbdata.field('MPAHBETA')
self.mpao3=tbdata.field('MPAOIII')
self.mpan2=tbdata.field('MPANII')
#sextractor info
self.numberser=tbdata.field('NUMBERSER')
self.ximageser=tbdata.field('XIMAGESER')
self.yimageser=tbdata.field('YIMAGESER')
self.xminimageser=tbdata.field('XMINIMAGESER')
self.xmaximageser=tbdata.field('XMAXIMAGESER')
self.yminimageser=tbdata.field('YMINIMAGESER')
self.raser=tbdata.field('RASER')
self.decser=tbdata.field('DECSER')
self.fluxisoser=tbdata.field('FLUXISOSER')
self.fluxerrisoser=tbdata.field('FLUXERRISOSER')
self.magisoser=tbdata.field('MAGISOSER')
self.magerrisoser=tbdata.field('MAGERRISOSER')
self.fluxautoser=tbdata.field('FLUXAUTOSER')
self.fluxerrautoser=tbdata.field('FLUXERRAUTOSER')
self.magautoser=tbdata.field('MAGAUTOSER')
self.magerrautoser=tbdata.field('MAGERRAUTOSER')
self.fluxpetroser=tbdata.field('FLUXPETROSER')
self.fluxerrpetroser=tbdata.field('FLUXERRPETROSER')
self.magpetroser=tbdata.field('MAGPETROSER')
self.magerrpetroser=tbdata.field('MAGERRPETROSER')
self.kronradser=tbdata.field('KRONRADSER')#kron radius
self.petroradser=tbdata.field('PETRORADSER')#petrosian radius
self.fluxradser=tbdata.field('FLUXRADSER')#1/2 light radius
self.isoareaser=tbdata.field('ISOAREASER')
self.aworldser=tbdata.field('AWORLDSER')
self.bworldser=tbdata.field('BWORLDSER')
self.thetaser=tbdata.field('THETASER')
self.errthetaser=tbdata.field('ERRTHETASER')
self.thetaj2000ser=tbdata.field('THETAJ2000SER')
self.errthetaj2000ser=tbdata.field('ERRTHETAJ2000SER')
self.elongser=tbdata.field('ELONGATIONSER')
self.elliptser=tbdata.field('ELLIPTICITYSER')
self.fwhmser=tbdata.field('FWHMSER')
self.flagsser=tbdata.field('FLAGSSER')
self.classstarser=tbdata.field('CLASSSTARSER')
#SEXTRACTOR output 24 micron data
self.numberse24=tbdata.field('NUMBERSE24')
self.ximagese24=tbdata.field('XIMAGESE24')
self.yimagese24=tbdata.field('YIMAGESE24')
self.xminimagese24=tbdata.field('XMINIMAGESE24')
self.xmaximagese24=tbdata.field('XMAXIMAGESE24')
self.xminimagese24=tbdata.field('YMINIMAGESE24')
self.rase24=tbdata.field('RASE24')
self.decse24=tbdata.field('DECSE24')
self.fluxisose24=tbdata.field('FLUXISOSE24')
self.fluxerrisose24=tbdata.field('FLUXERRISOSE24')
self.magisose24=tbdata.field('MAGISOSE24')
self.magerrisose24=tbdata.field('MAGERRISOSE24')
self.fluxautose24=tbdata.field('FLUXAUTOSE24')
self.fluxerrautose24=tbdata.field('FLUXERRAUTOSE24')
self.magautose24=tbdata.field('MAGAUTOSE24')
self.magerrautose24=tbdata.field('MAGERRAUTOSE24')
self.fluxpetrose24=tbdata.field('FLUXPETROSE24')
self.fluxerrpetrose24=tbdata.field('FLUXERRPETROSE24')
self.magpetrose24=tbdata.field('MAGPETROSE24')
self.magerrpetrose24=tbdata.field('MAGERRPETROSE24')
self.kronradse24=tbdata.field('KRONRADSE24')
self.petroradse24=tbdata.field('PETRORADSE24')
self.fluxradse24=tbdata.field('FLUXRADSE24')
self.isoarease24=tbdata.field('ISOAREASE24')
self.aworldse24=tbdata.field('AWORLDSE24')
self.bworldse24=tbdata.field('BWORLDSE24')
self.thetase24=tbdata.field('THETASE24')
self.errthetase24=tbdata.field('ERRTHETASE24')
self.thetaj2000se24=tbdata.field('THETAJ2000SE24')
self.errthetaj2000se24=tbdata.field('ERRTHETAJ2000SE24')
self.elongse24=tbdata.field('ELONGATIONSE24')
self.elliptse24=tbdata.field('ELLIPTICITYSE24')
self.fwhmse24=tbdata.field('FWHMSE24')
self.flagsse24=tbdata.field('FLAGSSE24')
self.classstarse24=tbdata.field('CLASSSTARSE24')
self.f24dist=self.fluxautose24[self.sex24flag]
#apex output
self.mipsra=tbdata.field('MIPSRA')
self.mipsdec=tbdata.field('MIPSDEC')
self.mipsflux=tbdata.field('MIPSFLUX')
self.mipsfluxerr=tbdata.field('MIPSFLUXERR')
self.mipssnr=tbdata.field('MIPSSNR')
self.mipsdeblend=tbdata.field('MIPSDEBLEND')
self.mipsfluxap1=tbdata.field('MIPSFLUXAP1')
self.mipsfluxap1err=tbdata.field('MIPSFLUXAP1ERR')
self.mipsfluxap2=tbdata.field('MIPSFLUXAP2')
self.mipsfluxap2err=tbdata.field('MIPSFLUXAP2ERR')
self.mipsfluxap3=tbdata.field('MIPSFLUXAP3')
self.mipsfluxap4err=tbdata.field('MIPSFLUXAP3ERR')
self.On24ImageFlag=tbdata.field('On24ImageFlag')
self.supervopt=tbdata.field('SUPERVOPT')
self.ra=tbdata.field('SUPERRA')
self.dec=tbdata.field('SUPERDEC')
self.stellarmass=tbdata.field('STELLARMASS')
self.stellarmass_cl=tbdata.field('STELLARMASS_CL')
self.sdssabsmag=tbdata.field('SDSSABSMAG')
self.sdssMu=self.sdssabsmag[:,0]
self.sdssMg=self.sdssabsmag[:,1]
self.sdssMr=self.sdssabsmag[:,2]
self.sdssMi=self.sdssabsmag[:,3]
self.sdssMz=self.sdssabsmag[:,4]
self.sdsslum=tbdata.field('SDSSLUM')
self.sdssLu=self.sdsslum[:,0]
self.sdssLg=self.sdsslum[:,1]
self.sdssLr=self.sdsslum[:,2]
self.sdssLi=self.sdsslum[:,3]
self.sdssLz=self.sdsslum[:,4]
self.sdssabsmag_cl=tbdata.field('SDSSABSMAG_CL')
self.sdssMu=self.sdssabsmag_cl[:,0]
self.sdssMg=self.sdssabsmag_cl[:,1]
self.sdssMr=self.sdssabsmag_cl[:,2]
self.sdssMi=self.sdssabsmag_cl[:,3]
self.sdssMz=self.sdssabsmag_cl[:,4]
self.sdsslum_cl=tbdata.field('SDSSLUM_CL')
self.sdssLu_cl=self.sdsslum_cl[:,0]
self.sdssLg_cl=self.sdsslum_cl[:,1]
self.sdssLr_cl=self.sdsslum_cl[:,2]
self.sdssLi_cl=self.sdsslum_cl[:,3]
self.sdssLz_cl=self.sdsslum_cl[:,4]
self.sdsscolc=tbdata.field('SDSSCOLC')
self.sdssrowc=tbdata.field('SDSSROWC')
self.membflag =tbdata.field('MEMBFLAG')
self.morphflag =tbdata.field('MORPHFLAG')
self.morph =tbdata.field('MORPH')
self.disturb =tbdata.field('DISTURB')
self.localdens =tbdata.field('LOCALDENS')
self.agn1 =tbdata.field('AGNKAUFF')
self.agn2 =tbdata.field('AGNKEWLEY')
self.agn3 =tbdata.field('AGNSTASIN')
self.n2halpha=(self.mpan2/self.mpahalpha)
self.o3hbeta=(self.mpao3/self.mpahbeta)
self.logn2halpha=log10(self.mpan2/self.mpahalpha)
self.logo3hbeta=log10(self.mpao3/self.mpahbeta)
self.ellipseflag24 =tbdata.field('ELLIPSEFLAG24')
self.ellipseflagsdss =tbdata.field('ELLIPSEFLAGSDSS')
self.ellipseflag =tbdata.field('ELLIPSEFLAG')
# galaxy zoo fields
self.galzooflag =tbdata.field('GALZOOFLAG')
self.galzoonvote =tbdata.field('GALZOONVOTE')
self.galzoopel =tbdata.field('GALZOOPEL')
self.galzoopcw =tbdata.field('GALZOOPCW')
self.galzoopacw =tbdata.field('GALZOOPACW')
self.galzoopedge =tbdata.field('GALZOOPEDGE')
self.galzoopdk =tbdata.field('GALZOOPDK')
self.galzoopmg =tbdata.field('GALZOOPMG')
self.galzoopcs =tbdata.field('GALZOOPCS')
self.galzoopeldebiased =tbdata.field('GALZOOPELDEBIASED')
self.galzoopcsdebiased =tbdata.field('GALZOOPCSDEBIASED')
self.galzoospiral =tbdata.field('GALZOOSPIRAL')
self.galzooelliptical =tbdata.field('GALZOOELLIPTICAL')
self.galzoouncertain =tbdata.field('GALZOOUNCERTAIN')
#new SDSS fields that quantify radial extent of galaxy
self.sdssIsoAr =tbdata.field('SDSSISOAR')
self.sdssIsoBr =tbdata.field('SDSSISOBR')
self.sdssIsoPhir =tbdata.field('SDSSISOPHIR')
self.sdssIsoPhirErr =tbdata.field('SDSSISOPHIERRR')
self.sdssExpRadr =tbdata.field('SDSSEXPRADR')
self.sdssExpABr =tbdata.field('SDSSEXPABR')
self.sdssExpABrErr =tbdata.field('SDSSEXPABRERR')
self.sdssExpPhir =tbdata.field('SDSSEXPPHIR')
self.sdssExpPhirErr =tbdata.field('SDSSEXPPHIERRR')
self.sdssPetroMag=tbdata.field('SDSSPETROMAG')
self.sdssPetroMagr=self.sdssPetroMag[:,2]
self.sdssPetroRad=tbdata.field('SDSSPETRORAD')
self.sdssPetroRadr=self.sdssPetroRad[:,2]
self.sdssPetroR50=tbdata.field('SDSSPETROR50')
self.sdssPetroR50r=self.sdssPetroR50[:,2]
self.sdssPetroR90=tbdata.field('SDSSPETROR90')
self.sdssPetroR90r=self.sdssPetroR90[:,2]
#de-redened magnitudes
self.sdssdered=tbdata.field('SDSSDERED')
self.sdssumag=self.sdssdered[:,0]
self.sdssgmag=self.sdssdered[:,1]
self.sdssrmag=self.sdssdered[:,2]
self.sdssimag=self.sdssdered[:,3]
self.sdsszmag=self.sdssdered[:,4]
# other Lum and SFR
self.HImass=tbdata.field('HIMASS')
self.L24=tbdata.field('L24')
self.L24err=tbdata.field('L24ERR')
self.Lir=tbdata.field('LIR')
self.Lirerr=tbdata.field('LIRERR')
self.SFR24=tbdata.field('SFR24')
self.SFR24err=tbdata.field('SFR24ERR')
self.SuperSFR24=tbdata.field('SUPERSFR24')
self.SuperSFR24err=tbdata.field('SUPERSFR24ERR')
self.HImass_cl=tbdata.field('HIMASS_CL')
self.L24_cl=tbdata.field('L24_CL')
self.L24err_cl=tbdata.field('L24ERR_CL')
self.Lir_cl=tbdata.field('LIR_CL')
self.Lirerr_cl=tbdata.field('LIRERR_CL')
self.SFR24_cl=tbdata.field('SFR24_CL')
self.SFR24err_cl=tbdata.field('SFR24ERR_CL')
self.SuperSFR24_cl=tbdata.field('SUPERSFR24_CL')
self.SuperSFR24err_cl=tbdata.field('SUPERSFR24ERR_CL')
#define red, green and blue galaxies
ur=self.sdssumag-self.sdssrmag
self.redflag=(ur > 2.3)
self.greenflag=(ur > 1.8) & (ur < 2.3)
self.blueflag=(ur<1.8)
#end of master table!
#self.spiralFlag=self.On24ImageFlag & self.galzooflag & self.ellipseflag & (self.galzoopcsdebiased > 0.6)
self.spiralFlag=self.galzooflag & self.galzoospiral
self.clustername=clustername
self.clusterra=clusterRA[clustername]
self.clusterdec=clusterDec[clustername]
self.dr=sqrt((self.ra-self.clusterra)**2+(self.dec-self.clusterdec)**2)
self.drR200=self.dr/self.r200deg
self.clustervel=clustervel[clustername]
self.clustersigma=clustersigma[clustername]
self.clustervmin=self.clustervel-3.*self.clustersigma
self.clustervmax=self.clustervel+3.*self.clustersigma
self.dist=sqrt((self.clusterra-self.ra)**2 + (self.clusterdec-self.dec)**2)
self.flagHI = (self.flux100 > 0.)
self.flagmemb = ((self.vopt > self.clustervmin) & (self.vopt < self.clustervmax)) | ((self.v21 > self.clustervmin) & (self.v21 < self.clustervmax))
self.dv=abs(self.supervopt-self.biweightvel)/self.biweightscale
self.allvelocity=3.e5*self.sdssspecz
for i in range(len(self.allvelocity)):
if self.sdssflag[i] < 1:
if self.v21[i] > 0:
self.allvelocity[i]=self.v21[i]
else:
self.allvelocity[i]=self.vopt[i]
self.nmemb=len(self.dist[self.membflag & self.On24ImageFlag])
self.nfield=len(self.dist[self.On24ImageFlag])-self.nmemb
print self.clustername,": ","N members = ",self.nmemb," N field = ",self.nfield
print ' N spirals = ',sum(self.spiralFlag),' Nspiral members = ',sum(self.spiralFlag&self.membflag)
print ' N spirals on 24um image = ',sum(self.spiralFlag & self.On24ImageFlag),' Nspiral members = ',sum(self.spiralFlag&self.membflag & self.On24ImageFlag)
print ' N galaxies on 24um image = ',sum(self.On24ImageFlag),' Nspiral members = ',sum(self.membflag & self.On24ImageFlag)
self.agcdict=dict((a,b) for a,b in zip(self.agcnumber,arange(len(self.agcnumber))))
#self.L24=zeros(len(self.mipsflux),'d')
#self.L24err=zeros(len(self.mipsflux),'d')
# calculate HI deficiency using Toribio et al 2011 results
# their relation is
# log(M_HI/Msun) = 8.72 + 1.25 log(D_25,r/kpc)
# and
# log D_25 = log D_25(obs) + beta log(b/a), where beta = 0.35 in r-band
# NOTE: SDSS isophotal radii are given in pixels!!!!
a=self.sdssIsoAr
b=self.sdssIsoBr
# convert from arcsec to kpc with self.AngDistance (which is in units of kpc/arcsec)
# multiply by 2 to convert from radius to diameter
# multiply by sdss pixel scale (0.39) b/c isophotal radii are given in pixels
self.D25obskpc=2.*self.sdssIsoAr*sdsspixelscale*self.AngDistance
# apply correction from toribio et al 2011
self.logD25kpc=log10(self.D25obskpc) + 0.35*log10(b/a)
# use toribio et al relation to predict the expected HI mass, including factor of 2 correction
self.HImassExpected = 10.**(8.72 + 1.25*(self.logD25kpc-log10(2.)))
self.HImassExpFromMr=10.**(6.44-0.18*self.sdssMr)
self.HImassExpFromgr=10.**(8.84+1.81*(self.sdssgmag-self.sdssrmag))
# calculate deficiency as log expected - log observed
self.HIDef = log10(self.HImassExpected) - log10(self.HImass)
self.myHIDef = log10(self.HImassExpected -self.HImass)
self.agnflag=self.agn1#use Kauffmann et al 2003 cut
self.irflag = self.apexflag & self.membflag
#set flag fot galaxies with dv < 3 sigma
self.dvflag = self.dv < 3.