R/write.flux.measurements.table.R
In AngusWright/LAMBDAR: Measure galaxy fluxes from an arbitrary FITS image using input aperture locations and dimensions
Defines functions
write.flux.measurements.table
Documented in
write.flux.measurements.table
write.flux.measurements.table <-
function(env=NULL,filename) {
#Write out a table containing the flux results for each galaxy
# Load Parameter Space
if(!is.null(env)) {
attach(env, warn.conflicts=FALSE)
}
sz=length(cat.ra)
janskyConv<-10^(-(mag.zp-8.9)/2.5)
#Get distance from image edge {{{
#X-axis {{{
#Distance from low side in pixels {{{
dx.pix.lo<-x.pix
#}}}
#Distance from high side in pixels {{{
dx.pix.hi<-astr.struc$NAXIS[1]-x.pix
#}}}
#Which apertures are closer to the high side {{{
index_x<-which(dx.pix.hi < dx.pix.lo)
#}}}
#Distances {{{
dx.pix<-dx.pix.lo
dx.pix[index_x]<-dx.pix.hi[index_x]
#}}}
#}}}
#Y-axis {{{
#Distance from low side in pixels {{{
dy.pix.lo<-y.pix
#}}}
#Distance from high side in pixels {{{
dy.pix.hi<-astr.struc$NAXIS[2]-y.pix
#}}}
#Which apertures are closer to the high side {{{
index_y<-which(dy.pix.hi < dy.pix.lo)
#}}}
#Distances {{{
dy.pix<-dy.pix.lo
dy.pix[index_y]<-dy.pix.hi[index_y]
#}}}
#}}}
#}}}
notes<-sub(".csv","_notes.txt",filename)
sink(type="output",file=notes)
on.exit(sink(type='output'),add=TRUE)
today <- Sys.Date()
cat(paste0("# Notes file for LAMBDAR (v ",packageVersion('LAMBDAR'),") Catalogue created ", format(today, format="%B %d %Y"),"\n"))
cat(paste0("# Below lists all parameters in the accompaning catalogue, and what they represent.\n"))
if (!psf.weighted) {
cat(paste0("# NB: This run of LAMBDAR did not request PSF Weighted Apertures. As such, each aperture was passed through a binary-filter which\n",
"# converted the contiguous apertures into TopHat apertures. The filter point was requested at ", paste(ap.limit),", which means that\n",
"# pixels contained within the ", paste(ap.limit*100),"% contour was set to 1, and the rest were set to 0.\n",
"# IMPORTANT: Because of this, all references below to the 'Post-Convolution Aperture' (i.e. SFA & DFA) are also after the aperture was binary-filtered.\n"))
}
if (magnitudes) {
cat(paste0("# As magnitudes were requested, all values below have been provided converted to Jansky from image units.\n",
"# The image-to-jansky conversion factor is ",janskyConv,"\n"))
}
if (verbose.out) {
####CATALOGUE PARAMETER
newtable<-data.frame(CATA_INDEX = cat.id)
colnames(newtable)<-cata.lab; cat(paste0(cata.lab," #Catalogue ID. Duplicates are prepended with 'DuplicatedID_'\n"))
newtable[[ra.lab]] = cat.ra; cat(paste0(ra.lab," #Right Ascention. Same as provided in the input catalogue\n"))
newtable[[dec.lab]] = cat.dec; cat(paste0(dec.lab," #Declination. Same as provided in the input catalogue\n"))
newtable[[theta.lab]] = cat.theta; cat(paste0(theta.lab," #Aperture Orientation Angle. Same as provided in the input catalogue\n"))
newtable[[semimaj.lab]] = cat.a; cat(paste0(semimaj.lab," #Aperture SemiMajor Axis length, in arcseconds. Same as provided in the input catalogue\n"))
newtable[[semimin.lab]] = cat.b; cat(paste0(semimin.lab," #Aperture SemiMinor Axis length, in arcseconds. Same as provided in the input catalogue\n"))
if (exists("contam")) { newtable[[contam.lab]] = contams; cat(paste0(contam.lab," #Contaminant Flag. Same as provided in the input catalogue\n")) }
if (exists("groups")) { newtable[[group.lab]] = groups; cat(paste0(group.lab," #Grouping Flag. Same as provided in the input catalogue\n")) }
# IMAGE PARAMETERS
newtable[["X.IMAGE"]] = cat.x; cat(paste0("X.IMAGE"," #Aperture Location in Image Coordinates; X-axis\n"))
newtable[["Y.IMAGE"]] = cat.y; cat(paste0("Y.IMAGE"," #Aperture Location in Image Coordinates; Y-axis\n"))
newtable[["NX_PIX2EDGE"]] = dx.pix; cat(paste0("NX_PIX2EDGE"," #Number of Pixels to the Nearest Edge of the Image; X-Axis. Useful for avoiding selection effects at image edges\n"))
newtable[["NY_PIX2EDGE"]] = dy.pix; cat(paste0("NY_PIX2EDGE"," #Number of Pixels to the Nearest Edge of the Image; Y-Axis. Useful for avoiding selection effects at image edges\n"))
newtable[["StampDiameter_pix"]] = stamplen; cat(paste0("StampDiameter_pix"," #Diameter of the Aperture Stamp, in Pixels.\n"))
# APERTURE SUMS & INTERMEDIATE SUMS
newtable[["SumPSF"]] = spsf; cat(paste0("SumPSF"," #Integral of the PSF. Should be the same for every object\n"))
newtable[["SumSA"]] = ssa; cat(paste0("SumSA"," #Integral of the Catalogue Aperture (i.e. the 'Prior') in pixels\n"))
newtable[["SumSFA"]] = ssfa; cat(paste0("SumSFA"," #Integral of the Post-Convolution Aperture.\n"))
newtable[["SumDFA"]] = sdfa; cat(paste0("SumDFA"," #Integral of the Deblended Post-Convolution Aperture.\n"))
if (diagnostic) {
newtable[["SumSFAsq"]] = ssfa2; cat(paste0("SumSFAsq"," #Integral of the Post-Convolution Aperture squared.\n"))
newtable[["SumDFAsq"]] = sdfa2; cat(paste0("SumDFAsq"," #Integral of the Deblended Post-Convolution Aperture squared.\n"))
}
newtable[["SumSFAxPSF"]] = ssfap; cat(paste0("SumSFAxPSF"," #Integral of the Post-Convolution Aperture times the PSF. Used in calculating the Minimum Aperture Correction.\n"))
newtable[["SumPSFxData"]] = spsfd; cat(paste0("SumPSFxData"," #Integral of the PSF times the Data Image. The point-source-estimated flux.\n"))
newtable[["SumSFAxData"]] = ssfad; cat(paste0("SumSFAxData"," #Integral of the Post-Convolution Aperture times the Data Image. The simplest flux LAMBDAR provides.\n"))
newtable[["SumDFAxData"]] = sdfad; cat(paste0("SumDFAxData"," #Integral of the Deblended Post-Convolution Aperture times the Data Image. The raw deblended flux LAMBDAR.\n"))
if (diagnostic) {
newtable[["SumSFAxError"]] = ssfae; cat(paste0("SumSFAxError"," #Integral of the Post-Convolution Aperture times the Error Image.\n"))
newtable[["SumDFAxError"]] = sdfae; cat(paste0("SumDFAxError"," #Integral of the Deblended Post-Convolution Aperture times the Error Image\n"))
newtable[["SumSFAxErrorsq"]] = ssfae2; cat(paste0("SumSFAxErrorsq"," #Integral of the Post-Convolution Aperture times the Error Image squared\n"))
newtable[["SumDFAxErrorsq"]] = sdfae2; cat(paste0("SumDFAxErrorsq"," #Integral of the Deblended Post-Convolution Aperture times the Error Image squared\n"))
}
if (magnitudes) {
newtable[["ApproxShot_Jy"]] = quick.shot*janskyConv; cat(paste0("ApproxShot"," #Approximate shot noise uncertainty sqrt(DFAFlux)/gain, in Jansky\n"))
} else {
newtable[["ApproxShot"]] = quick.shot; cat(paste0("ApproxShot"," #Approximate shot noise uncertainty sqrt(DFAFlux)/gain\n"))
}
newtable[["SumSFAsqxErrorsq"]] = ssfa2e2; cat(paste0("SumSFAsqxErrorsq"," #Integral of the Post-Convolution Aperture squared times the Error Image squared\n"))
newtable[["SumDFAsqxErrorsq"]] = sdfa2e2; cat(paste0("SumDFAsqxErrorsq"," #Integral of the Deblended Post-Convolution Aperture squared times the Error Image squared\n"))
if (do.sky.est | get.sky.rms) {
if (magnitudes) {
# SKY PARAMETERS: Jansky
newtable[["SkyLocal_Jy"]] = skylocal*janskyConv; cat(paste0("SkyLocal_Jy"," #The measured Median Sky Level, in Jansky.\n"))
newtable[["SkyLocal_Mean_Jy"]] = skylocal.mean*janskyConv; cat(paste0("SkyLocal_Mean_Jy"," #The measured Mean Sky Level, in Jansky.\n"))
newtable[["SkyFlux_Jy"]] = skyflux*janskyConv; cat(paste0("SkyFlux_Jy"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Uses the measured Median Sky Level.\n"))
newtable[["SkyFlux_Mean_Jy"]] = skyflux.mean*janskyConv; cat(paste0("SkyFlux_Mean_Jy"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Uses the measured Mean Sky Level.\n"))
newtable[["SkyError_Jy"]] = skyerr*janskyConv; cat(paste0("SkyError_Jy"," #Error on the Median Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Determined by measuring the Error on the Median Sky Level.\n"))
newtable[["SkyError_Mean_Jy"]] = skyerr.mean*janskyConv; cat(paste0("SkyError_Mean_Jy"," #Error on the Mean Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Determined by measuring the Error on the Mean Sky Level.\n"))
newtable[["SkyRMS_Jy"]] = skyrms*janskyConv; cat(paste0("SkyRMS_Jy"," #RMS of the Sky Pixels calculated during the Median Sky Level calculation, in Jansky.\n"))
newtable[["SkyRMS_Mean_Jy"]] = skyrms.mean*janskyConv; cat(paste0("SkyRMS_Mean_Jy"," #RMS of the Sky Pixels calculated during the Mean Sky Level calculation, in Jansky.\n"))
} else {
# SKY PARAMETERS: units
newtable[["SkyLocal_units"]] = skylocal; cat(paste0("SkyLocal_units"," #The measured Median Sky Level, in image units.\n"))
newtable[["SkyLocal_Mean_units"]] = skylocal.mean; cat(paste0("SkyLocal_Mean_units"," #The measured Mean Sky Level, in image units.\n"))
newtable[["SkyFlux_units"]] = skyflux; cat(paste0("SkyFlux_units"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Uses the measured Median Sky Level.\n"))
newtable[["SkyFlux_Mean_units"]] = skyflux.mean; cat(paste0("SkyFlux_Mean_units"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Uses the measured Mean Sky Level.\n"))
newtable[["SkyError_units"]] = skyerr; cat(paste0("SkyError_units"," #Error on the Median Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Determined by measuring the Error on the Median Sky Level.\n"))
newtable[["SkyError_Mean_units"]] = skyerr.mean; cat(paste0("SkyError_Mean_units"," #Error on the Mean Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Determined by measuring the Error on the Mean Sky Level.\n"))
newtable[["SkyRMS_units"]] = skyrms; cat(paste0("SkyRMS_units"," #RMS of the Sky Pixels calculated during the Median Sky Level calculation, in image units.\n"))
newtable[["SkyRMS_Mean_units"]] = skyrms.mean; cat(paste0("SkyRMS_Mean_units"," #RMS of the Sky Pixels calculated during the Mean Sky Level calculation, in image units.\n"))
}
# SKY PARAMETERS: General
newtable[["SkyRMSpval"]] = skypval; cat(paste0("SkyRMSpval"," #p-value resulting from a Pearson's Test of Normality on Sky Pixels used in Median Sky Level calculations. Useful in determining behaviour of sky pixels\n"))
newtable[["SkyRMSpval_Mean"]] = skypval.mean; cat(paste0("SkyRMSpval_Mean"," #p-value resulting from a Pearson's Test of Normality on Sky Pixels used in Mean Sky Level calculations. Useful in determining behaviour of sky pixels\n"))
newtable[["NearSkyBins"]] = skyNBinNear; cat(paste0("NearSkyBins"," #Number of Sky Bins equal to the Sky Estimate (within uncertainties), during Median Sky Level Calculations. Max 10.\n"))
newtable[["NearSkyBins_Mean"]] = skyNBinNear.mean; cat(paste0("NearSkyBins_Mean"," #Number of Sky Bins equal to the Sky Estimate (within uncertainties), during Mean Sky Level Calculations. Max 10.\n"))
}
if (!magnitudes) {
# FLUXES: Units
newtable[["PSFFlux_units"]] = psfflux; cat(paste0("PSFFlux_units"," #Final Point Source Flux, in image units.\n"))
newtable[["PSFErr_units"]] = psferr; cat(paste0("PSFErr_units"," #Error on Final Point Source Flux, in image units. Incorporates Sky Subtraction, and Sky RMS Uncertainty \n"))
newtable[["SFAFlux_units"]] = sfaflux; cat(paste0("SFAFlux_units"," #Final Blended Flux, in image units.\n"))
newtable[["SFAErr_units"]] = sfaerr; cat(paste0("SFAErr_units"," #Error on Final Blended Flux, in image units. Incorporates Shot Noise, Sky Subtraction, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DFAFlux_units"]] = dfaflux; cat(paste0("DFAFlux_units"," #Final Deblended Flux, in image units.\n"))
newtable[["DFAErr_units"]] = dfaerr; cat(paste0("DFAErr_units"," #Error on Final Deblended Flux, in image units. Incorporates Shot Noise, Sky Subtraction, Deblending, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DeblendErr_units"]] = deblerr; cat(paste0("DeblendErr_units"," #Absolute Flux Uncertainty caused by the Deblend of the Deblended Post-Convolution Aperture.\n"))
if (iterate.fluxes) {
cat(paste0(paste("DFAFlux_Iter<i>_units",sep="")," #Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. NB: These values are *not* sky subtracted and/or aperture corrected. In image units.\n"))
cat(paste0(paste("DFAErr_Iter<i>_units",sep="")," #Error on Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. In image units.\n"))
cat(paste0(paste("SumDFA_Iter<i>",sep="")," #Sum of the Deblended Post-Convolution Model after <i> iterations of Measurement, Fluxweighting, and Deblending. In pixels\n"))
if (length(dim(fluxiters))>1) {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_units",sep="")]] = fluxiters[,i];
newtable[[paste("DFAErr_Iter",i,"_units",sep="")]] = erriters[,i];
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[,i];
}
} else {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_units",sep="")]] = fluxiters[i];
newtable[[paste("DFAErr_Iter",i,"_units",sep="")]] = erriters[i];
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[i];
}
}
}
} else {
# FLUXES: Jansky
newtable[["PSFFlux_Jy"]] = psfflux*janskyConv; cat(paste0("PSFFlux_Jy"," #Final Point Source Flux, in Jansky.\n"))
newtable[["PSFErr_Jy"]] = psferr*janskyConv; cat(paste0("PSFErr_Jy"," #Error on Final Point Source Flux, in Jansky. Incorporates Sky Subtraction, and Sky RMS Uncertainty \n"))
newtable[["SFAFlux_Jy"]] = sfaflux*janskyConv; cat(paste0("SFAFlux_Jy"," #Final Blended Flux, in Jansky.\n"))
newtable[["SFAErr_Jy"]] = sfaerr*janskyConv; cat(paste0("SFAErr_Jy"," #Error on Final Blended Flux, in Jansky. Incorporates Shot Noise, Sky Subtraction, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DFAFlux_Jy"]] = dfaflux*janskyConv; cat(paste0("DFAFlux_Jy"," #Final Deblended Flux, in Jansky.\n"))
newtable[["DFAErr_Jy"]] = dfaerr*janskyConv; cat(paste0("DFAErr_Jy"," #Error on Final Deblended Flux, in Jansky. Incorporates Shot Noise, Sky Subtraction, Deblending, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DeblendErr_Jy"]] = deblerr*janskyConv; cat(paste0("DeblendErr_Jy"," #Absolute Flux Uncertainty caused by the Deblend of the Deblended Post-Convolution Aperture, in Jansky.\n"))
if (iterate.fluxes) {
cat(paste0(paste("DFAFlux_Iter<i>_Jy",sep="")," #Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. NB: These values are *not* sky subtracted and/or aperture corrected. In Jansky.\n"))
cat(paste0(paste("DFAErr_Iter<i>_Jy",sep="")," #Error on Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. In Jansky.\n"))
cat(paste0(paste("SumDFA_Iter<i>",sep="")," #Sum of the Deblended Post-Convolution Model after <i> iterations of Measurement, Fluxweighting, and Deblending. In pixels\n"))
if (length(dim(fluxiters))>1) {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_Jy",sep="")]] = fluxiters[,i]*janskyConv;
newtable[[paste("DFAErr_Iter",i,"_Jy",sep="")]] = erriters[,i]*janskyConv;
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[,i];
}
} else {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_Jy",sep="")]] = fluxiters[i]*janskyConv;
newtable[[paste("DFAErr_Iter",i,"_Jy",sep="")]] = erriters[i]*janskyConv;
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[i];
}
}
}
newtable[["ABMagDFA"]] = mags; cat(paste0("ABMagDFA"," #AB Magnitude of Final Deblended Flux\n"))
newtable[["ABMagErrDFA"]] = (2.5/log(10))*(dfaerr/dfaflux); cat(paste0("ABMagErrDFA"," #Error on the AB Magnitude of Final Deblended Flux\n"))
}
# BLANKS CORRECTION
if (blank.cor) {
if (magnitudes) {
newtable[["BlanksMeanMean_Jy"]] = blanks$randMean.mean*janskyConv; cat(paste0("BlanksMeanMean_Jy"," #Mean Value of the Mean Pixel Values in <n> Blank Apertures. In Jansky.\n"))
newtable[["BlanksMeanSD_Jy"]] = blanks$randMean.SD*janskyConv; cat(paste0("BlanksMeanSD_Jy"," #Standard Deviation of the Mean Pixel Values in <n> Blank Apertures. In Jansky.\n"))
newtable[["BlanksMeanMAD_Jy"]] = blanks$randMean.MAD*janskyConv; cat(paste0("BlanksMeanMAD_Jy"," #Median Absolute Deviation from Median of the Mean Pixel Values in <n> Blank Apertures. In Jansky.\n"))
newtable[["BlanksApMean"]] = blanks$randAp.mean; cat(paste0("BlanksApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApSD"]] = blanks$randAp.SD; cat(paste0("BlanksApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApMAD"]] = blanks$randAp.MAD; cat(paste0("BlanksApMAD"," #Median Absolute Deviation from Median of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
} else {
newtable[["BlanksMeanMean_units"]] = blanks$randMean.mean; cat(paste0("BlanksMeanMean_units"," #Mean Value of the Mean Pixel Values in <n> Blank Apertures. In image units.\n"))
newtable[["BlanksMeanSD_units"]] = blanks$randMean.SD; cat(paste0("BlanksMeanSD_units"," #Standard Deviation of the Mean Pixel Values in <n> Blank Apertures. In image units.\n"))
newtable[["BlanksMeanMAD_units"]] = blanks$randMean.MAD; cat(paste0("BlanksMeanMAD_Jy"," #Median Absolute Deviation from Median of the Mean Pixel Values in <n> Blank Apertures.\n"))
newtable[["BlanksApMean"]] = blanks$randAp.mean; cat(paste0("BlanksApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApSD"]] = blanks$randAp.SD; cat(paste0("BlanksApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApMAD"]] = blanks$randAp.MAD; cat(paste0("BlanksApMAD"," #Median Absolute Deviation from Median of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
}
newtable[["NumberMeasuredBlanks"]] = blanks$nRand; cat(paste0("NumberMeasuredBlanks"," #Number of Blank Apertures measured per object. Varies object to object due to source masking.\n"))
}
if (ran.cor) {
if (magnitudes) {
newtable[["RandomsMeanMean_Jy"]] = randoms$randMean.mean*janskyConv; cat(paste0("RandomsMeanMean_Jy"," #Mean Value of the Mean Pixel Values in <n> Random Apertures. In Jansky.\n"))
newtable[["RandomsMeanSD_Jy"]] = randoms$randMean.SD*janskyConv; cat(paste0("RandomsMeanSD_Jy"," #Standard Deviation of the Mean Pixel Values in <n> Random Apertures. In Jansky.\n"))
newtable[["RandomsApMean"]] = randoms$randAp.mean; cat(paste0("RandomsApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
newtable[["RandomsApSD"]] = randoms$randAp.SD; cat(paste0("RandomsApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
} else {
newtable[["RandomsMeanMean_units"]] = randoms$randMean.mean; cat(paste0("RandomsMeanMean_units"," #Mean Value of the Mean Pixel Values in <n> Random Apertures. In image units.\n"))
newtable[["RandomsMeanSD_units"]] = randoms$randMean.SD; cat(paste0("RandomsMeanSD_units"," #Standard Deviation of the Mean Pixel Values in <n> Random Apertures. In image units.\n"))
newtable[["RandomsApMean"]] = randoms$randAp.mean; cat(paste0("RandomsApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
newtable[["RandomsApSD"]] = randoms$randAp.SD; cat(paste0("RandomsApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
}
}
if (!no.psf) {
newtable[["MinApCorr"]] = ApCorr; cat(paste0("MinApCorr"," #Value of the Multiplicative Minimum Aperture Correction. This correction is important, and can _only_ improve an objects flux determination.\n"))
newtable[["MaxApCorr"]] = WtCorr; cat(paste0("MaxApCorr"," #Value of the Multiplicative Maximum Aperture Correction. This correction can cause excess flux-boosting systematically as a function of object morphology, and is provided __as a guide only__\n"))
}
# Misc.
if (magnitudes) {
newtable[["DetecThres_5sig_Jy"]] = detecthres*janskyConv; cat(paste0("DetecThres_5sig"," #Flux contained in this aperture, assuming a 5-sigma Detection, in Jansky\n"))
newtable[["DetecThres_5sig_Mag"]] = detecthres.mag; cat(paste0("DetecThres_5sig_Mag"," #AB Magnitude of an object in this aperture assimung a 5-sigma Detection.\n"))
} else {
newtable[["DetecThres_5sig_units"]] = detecthres; cat(paste0("DetecThres_5sig"," #Flux contained in this aperture, assuming a 5-sigma Detection, in image units\n"))
}
if (magnitudes) {
cat(paste0("QuarteredPhot#_Jy"," #Flux contained in Four Quadrants of the Post-Convolution aperture, split along the stamp centre in x & y directions, in Jansky. Useful in diagnosis of bad apertures/deblends.\n"))
cat(paste0("QuarteredPhot#_Deblended_Jy"," #Flux contained in Four Quadrants of the Deblended Post-Convolution aperture, split along the stamp centre in x & y directions, in Jansky. Useful in diagnosis of bad apertures/deblends.\n"))
if (length(dim(qssfad))>1) {
newtable[["QuarteredPhot1_Jy"]] = qssfad[,1]*janskyConv;
newtable[["QuarteredPhot2_Jy"]] = qssfad[,2]*janskyConv;
newtable[["QuarteredPhot3_Jy"]] = qssfad[,3]*janskyConv;
newtable[["QuarteredPhot4_Jy"]] = qssfad[,4]*janskyConv;
newtable[["QuarteredPhot1_Deblended_Jy"]] = qsdfad[,1]*janskyConv;
newtable[["QuarteredPhot2_Deblended_Jy"]] = qsdfad[,2]*janskyConv;
newtable[["QuarteredPhot3_Deblended_Jy"]] = qsdfad[,3]*janskyConv;
newtable[["QuarteredPhot4_Deblended_Jy"]] = qsdfad[,4]*janskyConv;
} else {
newtable[["QuarteredPhot1_Jy"]] = qssfad[1]*janskyConv;
newtable[["QuarteredPhot2_Jy"]] = qssfad[2]*janskyConv;
newtable[["QuarteredPhot3_Jy"]] = qssfad[3]*janskyConv;
newtable[["QuarteredPhot4_Jy"]] = qssfad[4]*janskyConv;
newtable[["QuarteredPhot1_Deblended_Jy"]] = qsdfad[1]*janskyConv;
newtable[["QuarteredPhot2_Deblended_Jy"]] = qsdfad[2]*janskyConv;
newtable[["QuarteredPhot3_Deblended_Jy"]] = qsdfad[3]*janskyConv;
newtable[["QuarteredPhot4_Deblended_Jy"]] = qsdfad[4]*janskyConv;
}
newtable[["PixelFlux_Jy"]] = pixflux*janskyConv; cat(paste0("PixelFlux_Jy"," #Pixel Flux at the object RA/DEC, in Jansky.\n"))
} else {
cat(paste0("QuarteredPhot#_units"," #Flux contained in Four Quadrants of the Post-Convolution aperture, split along the stamp centre in x & y directions, in image units. Useful in diagnosis of bad apertures/deblends.\n"))
cat(paste0("QuarteredPhot#_Deblended_units"," #Flux contained in Four Quadrants of the Deblended Post-Convolution aperture, split along the stamp centre in x & y directions, in image units. Useful in diagnosis of bad apertures/deblends.\n"))
if (length(dim(qssfad))>1) {
newtable[["QuarteredPhot1_units"]] = qssfad[,1];
newtable[["QuarteredPhot2_units"]] = qssfad[,2];
newtable[["QuarteredPhot3_units"]] = qssfad[,3];
newtable[["QuarteredPhot4_units"]] = qssfad[,4];
newtable[["QuarteredPhot1_Deblended_units"]] = qsdfad[,1];
newtable[["QuarteredPhot2_Deblended_units"]] = qsdfad[,2];
newtable[["QuarteredPhot3_Deblended_units"]] = qsdfad[,3];
newtable[["QuarteredPhot4_Deblended_units"]] = qsdfad[,4];
} else {
newtable[["QuarteredPhot1_units"]] = qssfad[1];
newtable[["QuarteredPhot2_units"]] = qssfad[2];
newtable[["QuarteredPhot3_units"]] = qssfad[3];
newtable[["QuarteredPhot4_units"]] = qssfad[4];
newtable[["QuarteredPhot1_Deblended_units"]] = qsdfad[1];
newtable[["QuarteredPhot2_Deblended_units"]] = qsdfad[2];
newtable[["QuarteredPhot3_Deblended_units"]] = qsdfad[3];
newtable[["QuarteredPhot4_Deblended_units"]] = qsdfad[4];
}
newtable[["PixelFlux_units"]] = pixflux; cat(paste0("PixelFlux_units"," #Pixel Flux at the object RA/DEC, in image units\n"))
}
newtable[["PhotometryWarning"]] = photWarnFlag; cat(paste0(""," #Some Rudimentary Photometry Warnings. Read Carefully and Take Note!\n"))
cat(paste0(""," #PhotometryWarnings: Q - Quartered Photometry Warning; 70+% of source flux contained in a single quadrant\n"))
cat(paste0(""," S - Sky Estimate Warning; Sky estimate determined in by 3 or less bins\n"))
cat(paste0(""," X - Saturation Warning; Pixels in this object aperture are saturated\n"))
cat(paste0(""," I - Iteration Warning; This object was lost during iteration because its flux was measured to be <= 0.\n"))
newtable[["PhotometryBitWarning"]] = photWarnBitFlag; cat(paste0(""," #Photometry Warnings expressed as a bitflag := IXSQ; so if S only warning: bitflag := 0010 := 2 \n"))
write.csv(newtable,file=filename,na='NA',quote=FALSE,row.names=FALSE)
} else {
####CATALOGUE PARAMETER
newtable<-data.frame(CATA_INDEX = cat.id)
colnames(newtable)<-cata.lab; cat(paste0(cata.lab," #Catalogue ID. Duplicates are prepended with 'DuplicatedID_'\n"))
newtable[[ra.lab]] = cat.ra; cat(paste0(ra.lab," #Right Ascention. Same as provided in the input catalogue\n"))
newtable[[dec.lab]] = cat.dec; cat(paste0(dec.lab," #Declination. Same as provided in the input catalogue\n"))
newtable[[theta.lab]] = cat.theta; cat(paste0(theta.lab," #Aperture Orientation Angle. Same as provided in the input catalogue\n"))
newtable[[semimaj.lab]] = cat.a; cat(paste0(semimaj.lab," #Aperture SemiMajor Axis length, in arcseconds. Same as provided in the input catalogue\n"))
newtable[[semimin.lab]] = cat.b; cat(paste0(semimin.lab," #Aperture SemiMinor Axis length, in arcseconds. Same as provided in the input catalogue\n"))
if (exists("contam")) { newtable[[contam.lab]] = contams; cat(paste0(contam.lab," #Contaminant Flag. Same as provided in the input catalogue\n")) }
if (exists("groups")) { newtable[[group.lab]] = groups; cat(paste0(group.lab," #Grouping Flag. Same as provided in the input catalogue\n")) }
# IMAGE PARAMETERS
newtable[["NX_PIX2EDGE"]] = dx.pix; cat(paste0("NX_PIX2EDGE"," #Number of Pixels to the Nearest Edge of the Image; X-Axis. Useful for avoiding selection effects at image edges\n"))
newtable[["NY_PIX2EDGE"]] = dy.pix; cat(paste0("NY_PIX2EDGE"," #Number of Pixels to the Nearest Edge of the Image; Y-Axis. Useful for avoiding selection effects at image edges\n"))
# APERTURE SUMS & INTERMEDIATE SUMS
newtable[["SumPSF"]] = spsf; cat(paste0("SumPSF"," #Integral of the PSF. Should be the same for every object\n"))
newtable[["SumSA"]] = ssa; cat(paste0("SumSA"," #Integral of the Catalogue Aperture (i.e. the 'Prior') in pixels\n"))
newtable[["SumSFA"]] = ssfa; cat(paste0("SumSFA"," #Integral of the Post-Convolution Aperture.\n"))
newtable[["SumDFA"]] = sdfa; cat(paste0("SumDFA"," #Integral of the Deblended Post-Convolution Aperture.\n"))
newtable[["SumPSFxData"]] = spsfd; cat(paste0("SumPSFxData"," #Integral of the PSF times the image.\n"))
if (do.sky.est | get.sky.rms) {
if (magnitudes) {
# SKY PARAMETERS: Jansky
newtable[["SkyLocal_Jy"]] = skylocal*janskyConv; cat(paste0("SkyLocal_Jy"," #The measured Median Sky Level, in Jansky.\n"))
newtable[["SkyLocal_Mean_Jy"]] = skylocal.mean*janskyConv; cat(paste0("SkyLocal_Mean_Jy"," #The measured Mean Sky Level, in Jansky.\n"))
newtable[["SkyFlux_Jy"]] = skyflux*janskyConv; cat(paste0("SkyFlux_Jy"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Uses the measured Median Sky Level.\n"))
newtable[["SkyFlux_Mean_Jy"]] = skyflux.mean*janskyConv; cat(paste0("SkyFlux_Mean_Jy"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Uses the measured Mean Sky Level.\n"))
newtable[["SkyError_Jy"]] = skyerr*janskyConv; cat(paste0("SkyError_Jy"," #Error on the Median Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Determined by measuring the Error on the Median Sky Level.\n"))
newtable[["SkyError_Mean_Jy"]] = skyerr.mean*janskyConv; cat(paste0("SkyError_Mean_Jy"," #Error on the Mean Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Determined by measuring the Error on the Mean Sky Level.\n"))
newtable[["SkyRMS_Jy"]] = skyrms*janskyConv; cat(paste0("SkyRMS_Jy"," #RMS of the Sky Pixels calculated during the Median Sky Level calculation, in Jansky.\n"))
newtable[["SkyRMS_Mean_Jy"]] = skyrms.mean*janskyConv; cat(paste0("SkyRMS_Mean_Jy"," #RMS of the Sky Pixels calculated during the Mean Sky Level calculation, in Jansky.\n"))
} else {
# SKY PARAMETERS: units
newtable[["SkyLocal_units"]] = skylocal*janskyConv; cat(paste0("SkyLocal_units"," #The measured Median Sky Level, in image units.\n"))
newtable[["SkyLocal_Mean_units"]] = skylocal.mean*janskyConv; cat(paste0("SkyLocal_Mean_units"," #The measured Mean Sky Level, in image units.\n"))
newtable[["SkyFlux_units"]] = skyflux*janskyConv; cat(paste0("SkyFlux_units"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Uses the measured Median Sky Level.\n"))
newtable[["SkyFlux_Mean_units"]] = skyflux.mean*janskyConv; cat(paste0("SkyFlux_Mean_units"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Uses the measured Mean Sky Level.\n"))
newtable[["SkyError_units"]] = skyerr*janskyConv; cat(paste0("SkyError_units"," #Error on the Median Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Determined by measuring the Error on the Median Sky Level.\n"))
newtable[["SkyError_Mean_units"]] = skyerr.mean*janskyConv; cat(paste0("SkyError_Mean_units"," #Error on the Mean Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Determined by measuring the Error on the Mean Sky Level.\n"))
newtable[["SkyRMS_units"]] = skyrms*janskyConv; cat(paste0("SkyRMS_units"," #RMS of the Sky Pixels calculated during the Median Sky Level calculation, in image units.\n"))
newtable[["SkyRMS_Mean_units"]] = skyrms.mean*janskyConv; cat(paste0("SkyRMS_Mean_units"," #RMS of the Sky Pixels calculated during the Mean Sky Level calculation, in image units.\n"))
}
}
if (!magnitudes) {
# FLUXES: Units
newtable[["PSFFlux_units"]] = psfflux; cat(paste0("PSFFlux_units"," #Final Point Source Flux, in image units.\n"))
newtable[["PSFErr_units"]] = psferr; cat(paste0("PSFErr_units"," #Error on Final Point Source Flux, in image units. Incorporates Sky Subtraction, and Sky RMS Uncertainty \n"))
newtable[["SFAFlux_units"]] = sfaflux; cat(paste0("SFAFlux_units"," #Final Blended Flux, in image units.\n"))
newtable[["SFAErr_units"]] = sfaerr; cat(paste0("SFAErr_units"," #Error on Final Blended Flux, in image units. Incorporates Shot Noise, Sky Subtraction, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DFAFlux_units"]] = dfaflux; cat(paste0("DFAFlux_units"," #Final Deblended Flux, in image units.\n"))
newtable[["DFAErr_units"]] = dfaerr; cat(paste0("DFAErr_units"," #Error on Final Deblended Flux, in image units. Incorporates Shot Noise, Sky Subtraction, Deblending, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DeblendErr_units"]] = deblerr; cat(paste0("DeblendErr_units"," #Absolute Flux Uncertainty caused by the Deblend of the Deblended Post-Convolution Aperture.\n"))
if (iterate.fluxes) {
cat(paste0(paste("DFAFlux_Iter<i>_units",sep="")," #Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. NB: These values are *not* sky subtracted and/or aperture corrected. In image units.\n"))
cat(paste0(paste("DFAErr_Iter<i>_units",sep="")," #Error on Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. In image units.\n"))
cat(paste0(paste("SumDFA_Iter<i>",sep="")," #Sum of the Deblended Post-Convolution Model after <i> iterations of Measurement, Fluxweighting, and Deblending. In pixels\n"))
if (length(dim(fluxiters))>1) {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_units",sep="")]] = fluxiters[,i];
newtable[[paste("DFAErr_Iter",i,"_units",sep="")]] = erriters[,i];
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[,i];
}
} else {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_units",sep="")]] = fluxiters[i];
newtable[[paste("DFAErr_Iter",i,"_units",sep="")]] = erriters[i];
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[i];
}
}
}
} else {
# FLUXES: Jansky
newtable[["PSFFlux_Jy"]] = psfflux*janskyConv; cat(paste0("PSFFlux_Jy"," #Final Point Source Flux, in Jansky.\n"))
newtable[["PSFErr_Jy"]] = psferr*janskyConv; cat(paste0("PSFErr_Jy"," #Error on Final Point Source Flux, in Jansky. Incorporates Sky Subtraction, and Sky RMS Uncertainty only \n"))
newtable[["SFAFlux_Jy"]] = sfaflux*janskyConv; cat(paste0("SFAFlux_Jy"," #Final Blended Flux, in Jansky.\n"))
newtable[["SFAErr_Jy"]] = sfaerr*janskyConv; cat(paste0("SFAErr_Jy"," #Error on Final Blended Flux, in Jansky. Incorporates Shot Noise, Sky Subtraction, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DFAFlux_Jy"]] = dfaflux*janskyConv; cat(paste0("DFAFlux_Jy"," #Final Deblended Flux, in Jansky.\n"))
newtable[["DFAErr_Jy"]] = dfaerr*janskyConv; cat(paste0("DFAErr_Jy"," #Error on Final Deblended Flux, in Jansky. Incorporates Shot Noise, Sky Subtraction, Deblend, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DeblendErr_Jy"]] = deblerr*janskyConv; cat(paste0("DeblendErr_Jy"," #Absolute Flux Uncertainty caused by the Deblend of the Deblended Post-Convolution Aperture, in Jansky.\n"))
if (iterate.fluxes) {
cat(paste0(paste("DFAFlux_Iter<i>_Jy",sep="")," #Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. NB: These values are *not* sky subtracted and/or aperture corrected. In Jansky.\n"))
cat(paste0(paste("DFAErr_Iter<i>_Jy",sep="")," #Error on Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. In Jansky.\n"))
cat(paste0(paste("SumDFA_Iter<i>",sep="")," #Sum of the Deblended Post-Convolution Model after <i> iterations of Measurement, Fluxweighting, and Deblending. In pixels\n"))
if (length(dim(fluxiters))>1) {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_Jy",sep="")]] = fluxiters[,i]*janskyConv;
newtable[[paste("DFAErr_Iter",i,"_Jy",sep="")]] = erriters[,i]*janskyConv;
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[,i];
}
} else {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_Jy",sep="")]] = fluxiters[i]*janskyConv;
newtable[[paste("DFAErr_Iter",i,"_Jy",sep="")]] = erriters[i]*janskyConv;
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[i];
}
}
}
newtable[["ABMagDFA"]] = mags; cat(paste0("ABMagDFA"," #AB Magnitude of Final Deblended Flux\n"))
newtable[["ABMagErrDFA"]] = (2.5/log(10))*(dfaerr/dfaflux); cat(paste0("ABMagErrDFA"," #Error on the AB Magnitude of Final Deblended Flux\n"))
}
# BLANKS CORRECTION
if (blank.cor) {
if (magnitudes) {
newtable[["BlanksMeanMean_Jy"]] = blanks$randMean.mean*janskyConv; cat(paste0("BlanksMeanMean_Jy"," #Mean Value of the Mean Pixel Values in <n> Blank Apertures. In Jansky.\n"))
newtable[["BlanksMeanSD_Jy"]] = blanks$randMean.SD*janskyConv; cat(paste0("BlanksMeanSD_Jy"," #Standard Deviation of the Mean Pixel Values in <n> Blank Apertures. In Jansky.\n"))
newtable[["BlanksMeanMAD_Jy"]] = blanks$randMean.MAD*janskyConv; cat(paste0("BlanksMeanMAD_Jy"," #Median Absolute Deviation from Median of the Mean Pixel Values in <n> Blank Apertures. In Jansky.\n"))
newtable[["BlanksApMean"]] = blanks$randAp.mean; cat(paste0("BlanksApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApSD"]] = blanks$randAp.SD; cat(paste0("BlanksApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApMAD"]] = blanks$randAp.MAD; cat(paste0("BlanksApMAD"," #Median Absolute Deviation from Median of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
} else {
newtable[["BlanksMeanMean_units"]] = blanks$randMean.mean; cat(paste0("BlanksMeanMean_units"," #Mean Value of the Mean Pixel Values in <n> Blank Apertures. In image units.\n"))
newtable[["BlanksMeanSD_units"]] = blanks$randMean.SD; cat(paste0("BlanksMeanSD_units"," #Standard Deviation of the Mean Pixel Values in <n> Blank Apertures. In image units.\n"))
newtable[["BlanksMeanMAD_units"]] = blanks$randMean.MAD; cat(paste0("BlanksMeanMAD_Jy"," #Median Absolute Deviation from Median of the Mean Pixel Values in <n> Blank Apertures.\n"))
newtable[["BlanksApMean"]] = blanks$randAp.mean; cat(paste0("BlanksApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApSD"]] = blanks$randAp.SD; cat(paste0("BlanksApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApMAD"]] = blanks$randAp.MAD; cat(paste0("BlanksApMAD"," #Median Absolute Deviation from Median of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
}
newtable[["NumberMeasuredBlanks"]] = blanks$nRand; cat(paste0("NumberMeasuredBlanks"," #Number of Blank Apertures measured per object. Varies object to object due to source masking.\n"))
}
if (ran.cor) {
if (magnitudes) {
newtable[["RandomsMeanMean_Jy"]] = randoms$randMean.mean*janskyConv; cat(paste0("RandomsMeanMean_Jy"," #Mean Value of the Mean Pixel Values in <n> Random Apertures. In Jansky.\n"))
newtable[["RandomsMeanSD_Jy"]] = randoms$randMean.SD*janskyConv; cat(paste0("RandomsMeanSD_Jy"," #Standard Deviation of the Mean Pixel Values in <n> Random Apertures. In Jansky.\n"))
newtable[["RandomsApMean"]] = randoms$randAp.mean; cat(paste0("RandomsApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
newtable[["RandomsApSD"]] = randoms$randAp.SD; cat(paste0("RandomsApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
} else {
newtable[["RandomsMeanMean_units"]] = randoms$randMean.mean; cat(paste0("RandomsMeanMean_units"," #Mean Value of the Mean Pixel Values in <n> Random Apertures. In image units.\n"))
newtable[["RandomsMeanSD_units"]] = randoms$randMean.SD; cat(paste0("RandomsMeanSD_units"," #Standard Deviation of the Mean Pixel Values in <n> Random Apertures. In image units.\n"))
newtable[["RandomsApMean"]] = randoms$randAp.mean; cat(paste0("RandomsApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
newtable[["RandomsApSD"]] = randoms$randAp.SD; cat(paste0("RandomsApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
}
}
if (!no.psf) {
newtable[["MinApCorr"]] = ApCorr; cat(paste0("MinApCorr"," #Value of the Multiplicative Minimum Aperture Correction. This correction is important, and can _only_ improve an objects flux determination.\n"))
newtable[["MaxApCorr"]] = WtCorr; cat(paste0("MaxApCorr"," #Value of the Multiplicative Maximum Aperture Correction. This correction can cause excess flux-boosting systematically as a function of object morphology, and is provided __as a guide only__\n"))
}
# Misc.
newtable[["PhotometryWarning"]] = photWarnFlag; cat(paste0(""," #Some Rudimentary Photometry Warnings. Read Carefully and Take Note!\n"))
cat(paste0(""," #PhotometryWarnings: Q - Quartered Photometry Warning; 70+% of source flux contained in a single quadrant\n"))
cat(paste0(""," S - Sky Estimate Warning; Sky estimate determined in by 3 or less bins\n"))
cat(paste0(""," X - Saturation Warning; Pixels in this object aperture are saturated\n"))
cat(paste0(""," I - Iteration Warning; This object was lost during iteration because its flux was measured to be <= 0.\n"))
newtable[["PhotometryBitWarning"]] = photWarnBitFlag; cat(paste0(""," #Photometry Warnings expressed as a bitflag := IXSQ; so if S only warning: bitflag := 0010 := 2 \n"))
write.csv(newtable,file=filename,na='NA',quote=FALSE,row.names=FALSE)
}
if (!is.null(env)) { detach(env) }
return=NULL
}
AngusWright/LAMBDAR documentation built on May 12, 2022, 1:49 a.m.
R Package Documentation
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Defines functions write.flux.measurements.table
Documented in write.flux.measurements.table
write.flux.measurements.table <-
function(env=NULL,filename) {
#Write out a table containing the flux results for each galaxy
# Load Parameter Space
if(!is.null(env)) {
attach(env, warn.conflicts=FALSE)
}
sz=length(cat.ra)
janskyConv<-10^(-(mag.zp-8.9)/2.5)
#Get distance from image edge {{{
#X-axis {{{
#Distance from low side in pixels {{{
dx.pix.lo<-x.pix
#}}}
#Distance from high side in pixels {{{
dx.pix.hi<-astr.struc$NAXIS[1]-x.pix
#}}}
#Which apertures are closer to the high side {{{
index_x<-which(dx.pix.hi < dx.pix.lo)
#}}}
#Distances {{{
dx.pix<-dx.pix.lo
dx.pix[index_x]<-dx.pix.hi[index_x]
#}}}
#}}}
#Y-axis {{{
#Distance from low side in pixels {{{
dy.pix.lo<-y.pix
#}}}
#Distance from high side in pixels {{{
dy.pix.hi<-astr.struc$NAXIS[2]-y.pix
#}}}
#Which apertures are closer to the high side {{{
index_y<-which(dy.pix.hi < dy.pix.lo)
#}}}
#Distances {{{
dy.pix<-dy.pix.lo
dy.pix[index_y]<-dy.pix.hi[index_y]
#}}}
#}}}
#}}}
notes<-sub(".csv","_notes.txt",filename)
sink(type="output",file=notes)
on.exit(sink(type='output'),add=TRUE)
today <- Sys.Date()
cat(paste0("# Notes file for LAMBDAR (v ",packageVersion('LAMBDAR'),") Catalogue created ", format(today, format="%B %d %Y"),"\n"))
cat(paste0("# Below lists all parameters in the accompaning catalogue, and what they represent.\n"))
if (!psf.weighted) {
cat(paste0("# NB: This run of LAMBDAR did not request PSF Weighted Apertures. As such, each aperture was passed through a binary-filter which\n",
"# converted the contiguous apertures into TopHat apertures. The filter point was requested at ", paste(ap.limit),", which means that\n",
"# pixels contained within the ", paste(ap.limit*100),"% contour was set to 1, and the rest were set to 0.\n",
"# IMPORTANT: Because of this, all references below to the 'Post-Convolution Aperture' (i.e. SFA & DFA) are also after the aperture was binary-filtered.\n"))
}
if (magnitudes) {
cat(paste0("# As magnitudes were requested, all values below have been provided converted to Jansky from image units.\n",
"# The image-to-jansky conversion factor is ",janskyConv,"\n"))
}
if (verbose.out) {
####CATALOGUE PARAMETER
newtable<-data.frame(CATA_INDEX = cat.id)
colnames(newtable)<-cata.lab; cat(paste0(cata.lab," #Catalogue ID. Duplicates are prepended with 'DuplicatedID_'\n"))
newtable[[ra.lab]] = cat.ra; cat(paste0(ra.lab," #Right Ascention. Same as provided in the input catalogue\n"))
newtable[[dec.lab]] = cat.dec; cat(paste0(dec.lab," #Declination. Same as provided in the input catalogue\n"))
newtable[[theta.lab]] = cat.theta; cat(paste0(theta.lab," #Aperture Orientation Angle. Same as provided in the input catalogue\n"))
newtable[[semimaj.lab]] = cat.a; cat(paste0(semimaj.lab," #Aperture SemiMajor Axis length, in arcseconds. Same as provided in the input catalogue\n"))
newtable[[semimin.lab]] = cat.b; cat(paste0(semimin.lab," #Aperture SemiMinor Axis length, in arcseconds. Same as provided in the input catalogue\n"))
if (exists("contam")) { newtable[[contam.lab]] = contams; cat(paste0(contam.lab," #Contaminant Flag. Same as provided in the input catalogue\n")) }
if (exists("groups")) { newtable[[group.lab]] = groups; cat(paste0(group.lab," #Grouping Flag. Same as provided in the input catalogue\n")) }
# IMAGE PARAMETERS
newtable[["X.IMAGE"]] = cat.x; cat(paste0("X.IMAGE"," #Aperture Location in Image Coordinates; X-axis\n"))
newtable[["Y.IMAGE"]] = cat.y; cat(paste0("Y.IMAGE"," #Aperture Location in Image Coordinates; Y-axis\n"))
newtable[["NX_PIX2EDGE"]] = dx.pix; cat(paste0("NX_PIX2EDGE"," #Number of Pixels to the Nearest Edge of the Image; X-Axis. Useful for avoiding selection effects at image edges\n"))
newtable[["NY_PIX2EDGE"]] = dy.pix; cat(paste0("NY_PIX2EDGE"," #Number of Pixels to the Nearest Edge of the Image; Y-Axis. Useful for avoiding selection effects at image edges\n"))
newtable[["StampDiameter_pix"]] = stamplen; cat(paste0("StampDiameter_pix"," #Diameter of the Aperture Stamp, in Pixels.\n"))
# APERTURE SUMS & INTERMEDIATE SUMS
newtable[["SumPSF"]] = spsf; cat(paste0("SumPSF"," #Integral of the PSF. Should be the same for every object\n"))
newtable[["SumSA"]] = ssa; cat(paste0("SumSA"," #Integral of the Catalogue Aperture (i.e. the 'Prior') in pixels\n"))
newtable[["SumSFA"]] = ssfa; cat(paste0("SumSFA"," #Integral of the Post-Convolution Aperture.\n"))
newtable[["SumDFA"]] = sdfa; cat(paste0("SumDFA"," #Integral of the Deblended Post-Convolution Aperture.\n"))
if (diagnostic) {
newtable[["SumSFAsq"]] = ssfa2; cat(paste0("SumSFAsq"," #Integral of the Post-Convolution Aperture squared.\n"))
newtable[["SumDFAsq"]] = sdfa2; cat(paste0("SumDFAsq"," #Integral of the Deblended Post-Convolution Aperture squared.\n"))
}
newtable[["SumSFAxPSF"]] = ssfap; cat(paste0("SumSFAxPSF"," #Integral of the Post-Convolution Aperture times the PSF. Used in calculating the Minimum Aperture Correction.\n"))
newtable[["SumPSFxData"]] = spsfd; cat(paste0("SumPSFxData"," #Integral of the PSF times the Data Image. The point-source-estimated flux.\n"))
newtable[["SumSFAxData"]] = ssfad; cat(paste0("SumSFAxData"," #Integral of the Post-Convolution Aperture times the Data Image. The simplest flux LAMBDAR provides.\n"))
newtable[["SumDFAxData"]] = sdfad; cat(paste0("SumDFAxData"," #Integral of the Deblended Post-Convolution Aperture times the Data Image. The raw deblended flux LAMBDAR.\n"))
if (diagnostic) {
newtable[["SumSFAxError"]] = ssfae; cat(paste0("SumSFAxError"," #Integral of the Post-Convolution Aperture times the Error Image.\n"))
newtable[["SumDFAxError"]] = sdfae; cat(paste0("SumDFAxError"," #Integral of the Deblended Post-Convolution Aperture times the Error Image\n"))
newtable[["SumSFAxErrorsq"]] = ssfae2; cat(paste0("SumSFAxErrorsq"," #Integral of the Post-Convolution Aperture times the Error Image squared\n"))
newtable[["SumDFAxErrorsq"]] = sdfae2; cat(paste0("SumDFAxErrorsq"," #Integral of the Deblended Post-Convolution Aperture times the Error Image squared\n"))
}
if (magnitudes) {
newtable[["ApproxShot_Jy"]] = quick.shot*janskyConv; cat(paste0("ApproxShot"," #Approximate shot noise uncertainty sqrt(DFAFlux)/gain, in Jansky\n"))
} else {
newtable[["ApproxShot"]] = quick.shot; cat(paste0("ApproxShot"," #Approximate shot noise uncertainty sqrt(DFAFlux)/gain\n"))
}
newtable[["SumSFAsqxErrorsq"]] = ssfa2e2; cat(paste0("SumSFAsqxErrorsq"," #Integral of the Post-Convolution Aperture squared times the Error Image squared\n"))
newtable[["SumDFAsqxErrorsq"]] = sdfa2e2; cat(paste0("SumDFAsqxErrorsq"," #Integral of the Deblended Post-Convolution Aperture squared times the Error Image squared\n"))
if (do.sky.est | get.sky.rms) {
if (magnitudes) {
# SKY PARAMETERS: Jansky
newtable[["SkyLocal_Jy"]] = skylocal*janskyConv; cat(paste0("SkyLocal_Jy"," #The measured Median Sky Level, in Jansky.\n"))
newtable[["SkyLocal_Mean_Jy"]] = skylocal.mean*janskyConv; cat(paste0("SkyLocal_Mean_Jy"," #The measured Mean Sky Level, in Jansky.\n"))
newtable[["SkyFlux_Jy"]] = skyflux*janskyConv; cat(paste0("SkyFlux_Jy"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Uses the measured Median Sky Level.\n"))
newtable[["SkyFlux_Mean_Jy"]] = skyflux.mean*janskyConv; cat(paste0("SkyFlux_Mean_Jy"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Uses the measured Mean Sky Level.\n"))
newtable[["SkyError_Jy"]] = skyerr*janskyConv; cat(paste0("SkyError_Jy"," #Error on the Median Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Determined by measuring the Error on the Median Sky Level.\n"))
newtable[["SkyError_Mean_Jy"]] = skyerr.mean*janskyConv; cat(paste0("SkyError_Mean_Jy"," #Error on the Mean Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Determined by measuring the Error on the Mean Sky Level.\n"))
newtable[["SkyRMS_Jy"]] = skyrms*janskyConv; cat(paste0("SkyRMS_Jy"," #RMS of the Sky Pixels calculated during the Median Sky Level calculation, in Jansky.\n"))
newtable[["SkyRMS_Mean_Jy"]] = skyrms.mean*janskyConv; cat(paste0("SkyRMS_Mean_Jy"," #RMS of the Sky Pixels calculated during the Mean Sky Level calculation, in Jansky.\n"))
} else {
# SKY PARAMETERS: units
newtable[["SkyLocal_units"]] = skylocal; cat(paste0("SkyLocal_units"," #The measured Median Sky Level, in image units.\n"))
newtable[["SkyLocal_Mean_units"]] = skylocal.mean; cat(paste0("SkyLocal_Mean_units"," #The measured Mean Sky Level, in image units.\n"))
newtable[["SkyFlux_units"]] = skyflux; cat(paste0("SkyFlux_units"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Uses the measured Median Sky Level.\n"))
newtable[["SkyFlux_Mean_units"]] = skyflux.mean; cat(paste0("SkyFlux_Mean_units"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Uses the measured Mean Sky Level.\n"))
newtable[["SkyError_units"]] = skyerr; cat(paste0("SkyError_units"," #Error on the Median Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Determined by measuring the Error on the Median Sky Level.\n"))
newtable[["SkyError_Mean_units"]] = skyerr.mean; cat(paste0("SkyError_Mean_units"," #Error on the Mean Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Determined by measuring the Error on the Mean Sky Level.\n"))
newtable[["SkyRMS_units"]] = skyrms; cat(paste0("SkyRMS_units"," #RMS of the Sky Pixels calculated during the Median Sky Level calculation, in image units.\n"))
newtable[["SkyRMS_Mean_units"]] = skyrms.mean; cat(paste0("SkyRMS_Mean_units"," #RMS of the Sky Pixels calculated during the Mean Sky Level calculation, in image units.\n"))
}
# SKY PARAMETERS: General
newtable[["SkyRMSpval"]] = skypval; cat(paste0("SkyRMSpval"," #p-value resulting from a Pearson's Test of Normality on Sky Pixels used in Median Sky Level calculations. Useful in determining behaviour of sky pixels\n"))
newtable[["SkyRMSpval_Mean"]] = skypval.mean; cat(paste0("SkyRMSpval_Mean"," #p-value resulting from a Pearson's Test of Normality on Sky Pixels used in Mean Sky Level calculations. Useful in determining behaviour of sky pixels\n"))
newtable[["NearSkyBins"]] = skyNBinNear; cat(paste0("NearSkyBins"," #Number of Sky Bins equal to the Sky Estimate (within uncertainties), during Median Sky Level Calculations. Max 10.\n"))
newtable[["NearSkyBins_Mean"]] = skyNBinNear.mean; cat(paste0("NearSkyBins_Mean"," #Number of Sky Bins equal to the Sky Estimate (within uncertainties), during Mean Sky Level Calculations. Max 10.\n"))
}
if (!magnitudes) {
# FLUXES: Units
newtable[["PSFFlux_units"]] = psfflux; cat(paste0("PSFFlux_units"," #Final Point Source Flux, in image units.\n"))
newtable[["PSFErr_units"]] = psferr; cat(paste0("PSFErr_units"," #Error on Final Point Source Flux, in image units. Incorporates Sky Subtraction, and Sky RMS Uncertainty \n"))
newtable[["SFAFlux_units"]] = sfaflux; cat(paste0("SFAFlux_units"," #Final Blended Flux, in image units.\n"))
newtable[["SFAErr_units"]] = sfaerr; cat(paste0("SFAErr_units"," #Error on Final Blended Flux, in image units. Incorporates Shot Noise, Sky Subtraction, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DFAFlux_units"]] = dfaflux; cat(paste0("DFAFlux_units"," #Final Deblended Flux, in image units.\n"))
newtable[["DFAErr_units"]] = dfaerr; cat(paste0("DFAErr_units"," #Error on Final Deblended Flux, in image units. Incorporates Shot Noise, Sky Subtraction, Deblending, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DeblendErr_units"]] = deblerr; cat(paste0("DeblendErr_units"," #Absolute Flux Uncertainty caused by the Deblend of the Deblended Post-Convolution Aperture.\n"))
if (iterate.fluxes) {
cat(paste0(paste("DFAFlux_Iter<i>_units",sep="")," #Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. NB: These values are *not* sky subtracted and/or aperture corrected. In image units.\n"))
cat(paste0(paste("DFAErr_Iter<i>_units",sep="")," #Error on Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. In image units.\n"))
cat(paste0(paste("SumDFA_Iter<i>",sep="")," #Sum of the Deblended Post-Convolution Model after <i> iterations of Measurement, Fluxweighting, and Deblending. In pixels\n"))
if (length(dim(fluxiters))>1) {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_units",sep="")]] = fluxiters[,i];
newtable[[paste("DFAErr_Iter",i,"_units",sep="")]] = erriters[,i];
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[,i];
}
} else {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_units",sep="")]] = fluxiters[i];
newtable[[paste("DFAErr_Iter",i,"_units",sep="")]] = erriters[i];
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[i];
}
}
}
} else {
# FLUXES: Jansky
newtable[["PSFFlux_Jy"]] = psfflux*janskyConv; cat(paste0("PSFFlux_Jy"," #Final Point Source Flux, in Jansky.\n"))
newtable[["PSFErr_Jy"]] = psferr*janskyConv; cat(paste0("PSFErr_Jy"," #Error on Final Point Source Flux, in Jansky. Incorporates Sky Subtraction, and Sky RMS Uncertainty \n"))
newtable[["SFAFlux_Jy"]] = sfaflux*janskyConv; cat(paste0("SFAFlux_Jy"," #Final Blended Flux, in Jansky.\n"))
newtable[["SFAErr_Jy"]] = sfaerr*janskyConv; cat(paste0("SFAErr_Jy"," #Error on Final Blended Flux, in Jansky. Incorporates Shot Noise, Sky Subtraction, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DFAFlux_Jy"]] = dfaflux*janskyConv; cat(paste0("DFAFlux_Jy"," #Final Deblended Flux, in Jansky.\n"))
newtable[["DFAErr_Jy"]] = dfaerr*janskyConv; cat(paste0("DFAErr_Jy"," #Error on Final Deblended Flux, in Jansky. Incorporates Shot Noise, Sky Subtraction, Deblending, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DeblendErr_Jy"]] = deblerr*janskyConv; cat(paste0("DeblendErr_Jy"," #Absolute Flux Uncertainty caused by the Deblend of the Deblended Post-Convolution Aperture, in Jansky.\n"))
if (iterate.fluxes) {
cat(paste0(paste("DFAFlux_Iter<i>_Jy",sep="")," #Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. NB: These values are *not* sky subtracted and/or aperture corrected. In Jansky.\n"))
cat(paste0(paste("DFAErr_Iter<i>_Jy",sep="")," #Error on Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. In Jansky.\n"))
cat(paste0(paste("SumDFA_Iter<i>",sep="")," #Sum of the Deblended Post-Convolution Model after <i> iterations of Measurement, Fluxweighting, and Deblending. In pixels\n"))
if (length(dim(fluxiters))>1) {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_Jy",sep="")]] = fluxiters[,i]*janskyConv;
newtable[[paste("DFAErr_Iter",i,"_Jy",sep="")]] = erriters[,i]*janskyConv;
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[,i];
}
} else {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_Jy",sep="")]] = fluxiters[i]*janskyConv;
newtable[[paste("DFAErr_Iter",i,"_Jy",sep="")]] = erriters[i]*janskyConv;
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[i];
}
}
}
newtable[["ABMagDFA"]] = mags; cat(paste0("ABMagDFA"," #AB Magnitude of Final Deblended Flux\n"))
newtable[["ABMagErrDFA"]] = (2.5/log(10))*(dfaerr/dfaflux); cat(paste0("ABMagErrDFA"," #Error on the AB Magnitude of Final Deblended Flux\n"))
}
# BLANKS CORRECTION
if (blank.cor) {
if (magnitudes) {
newtable[["BlanksMeanMean_Jy"]] = blanks$randMean.mean*janskyConv; cat(paste0("BlanksMeanMean_Jy"," #Mean Value of the Mean Pixel Values in <n> Blank Apertures. In Jansky.\n"))
newtable[["BlanksMeanSD_Jy"]] = blanks$randMean.SD*janskyConv; cat(paste0("BlanksMeanSD_Jy"," #Standard Deviation of the Mean Pixel Values in <n> Blank Apertures. In Jansky.\n"))
newtable[["BlanksMeanMAD_Jy"]] = blanks$randMean.MAD*janskyConv; cat(paste0("BlanksMeanMAD_Jy"," #Median Absolute Deviation from Median of the Mean Pixel Values in <n> Blank Apertures. In Jansky.\n"))
newtable[["BlanksApMean"]] = blanks$randAp.mean; cat(paste0("BlanksApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApSD"]] = blanks$randAp.SD; cat(paste0("BlanksApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApMAD"]] = blanks$randAp.MAD; cat(paste0("BlanksApMAD"," #Median Absolute Deviation from Median of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
} else {
newtable[["BlanksMeanMean_units"]] = blanks$randMean.mean; cat(paste0("BlanksMeanMean_units"," #Mean Value of the Mean Pixel Values in <n> Blank Apertures. In image units.\n"))
newtable[["BlanksMeanSD_units"]] = blanks$randMean.SD; cat(paste0("BlanksMeanSD_units"," #Standard Deviation of the Mean Pixel Values in <n> Blank Apertures. In image units.\n"))
newtable[["BlanksMeanMAD_units"]] = blanks$randMean.MAD; cat(paste0("BlanksMeanMAD_Jy"," #Median Absolute Deviation from Median of the Mean Pixel Values in <n> Blank Apertures.\n"))
newtable[["BlanksApMean"]] = blanks$randAp.mean; cat(paste0("BlanksApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApSD"]] = blanks$randAp.SD; cat(paste0("BlanksApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApMAD"]] = blanks$randAp.MAD; cat(paste0("BlanksApMAD"," #Median Absolute Deviation from Median of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
}
newtable[["NumberMeasuredBlanks"]] = blanks$nRand; cat(paste0("NumberMeasuredBlanks"," #Number of Blank Apertures measured per object. Varies object to object due to source masking.\n"))
}
if (ran.cor) {
if (magnitudes) {
newtable[["RandomsMeanMean_Jy"]] = randoms$randMean.mean*janskyConv; cat(paste0("RandomsMeanMean_Jy"," #Mean Value of the Mean Pixel Values in <n> Random Apertures. In Jansky.\n"))
newtable[["RandomsMeanSD_Jy"]] = randoms$randMean.SD*janskyConv; cat(paste0("RandomsMeanSD_Jy"," #Standard Deviation of the Mean Pixel Values in <n> Random Apertures. In Jansky.\n"))
newtable[["RandomsApMean"]] = randoms$randAp.mean; cat(paste0("RandomsApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
newtable[["RandomsApSD"]] = randoms$randAp.SD; cat(paste0("RandomsApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
} else {
newtable[["RandomsMeanMean_units"]] = randoms$randMean.mean; cat(paste0("RandomsMeanMean_units"," #Mean Value of the Mean Pixel Values in <n> Random Apertures. In image units.\n"))
newtable[["RandomsMeanSD_units"]] = randoms$randMean.SD; cat(paste0("RandomsMeanSD_units"," #Standard Deviation of the Mean Pixel Values in <n> Random Apertures. In image units.\n"))
newtable[["RandomsApMean"]] = randoms$randAp.mean; cat(paste0("RandomsApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
newtable[["RandomsApSD"]] = randoms$randAp.SD; cat(paste0("RandomsApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
}
}
if (!no.psf) {
newtable[["MinApCorr"]] = ApCorr; cat(paste0("MinApCorr"," #Value of the Multiplicative Minimum Aperture Correction. This correction is important, and can _only_ improve an objects flux determination.\n"))
newtable[["MaxApCorr"]] = WtCorr; cat(paste0("MaxApCorr"," #Value of the Multiplicative Maximum Aperture Correction. This correction can cause excess flux-boosting systematically as a function of object morphology, and is provided __as a guide only__\n"))
}
# Misc.
if (magnitudes) {
newtable[["DetecThres_5sig_Jy"]] = detecthres*janskyConv; cat(paste0("DetecThres_5sig"," #Flux contained in this aperture, assuming a 5-sigma Detection, in Jansky\n"))
newtable[["DetecThres_5sig_Mag"]] = detecthres.mag; cat(paste0("DetecThres_5sig_Mag"," #AB Magnitude of an object in this aperture assimung a 5-sigma Detection.\n"))
} else {
newtable[["DetecThres_5sig_units"]] = detecthres; cat(paste0("DetecThres_5sig"," #Flux contained in this aperture, assuming a 5-sigma Detection, in image units\n"))
}
if (magnitudes) {
cat(paste0("QuarteredPhot#_Jy"," #Flux contained in Four Quadrants of the Post-Convolution aperture, split along the stamp centre in x & y directions, in Jansky. Useful in diagnosis of bad apertures/deblends.\n"))
cat(paste0("QuarteredPhot#_Deblended_Jy"," #Flux contained in Four Quadrants of the Deblended Post-Convolution aperture, split along the stamp centre in x & y directions, in Jansky. Useful in diagnosis of bad apertures/deblends.\n"))
if (length(dim(qssfad))>1) {
newtable[["QuarteredPhot1_Jy"]] = qssfad[,1]*janskyConv;
newtable[["QuarteredPhot2_Jy"]] = qssfad[,2]*janskyConv;
newtable[["QuarteredPhot3_Jy"]] = qssfad[,3]*janskyConv;
newtable[["QuarteredPhot4_Jy"]] = qssfad[,4]*janskyConv;
newtable[["QuarteredPhot1_Deblended_Jy"]] = qsdfad[,1]*janskyConv;
newtable[["QuarteredPhot2_Deblended_Jy"]] = qsdfad[,2]*janskyConv;
newtable[["QuarteredPhot3_Deblended_Jy"]] = qsdfad[,3]*janskyConv;
newtable[["QuarteredPhot4_Deblended_Jy"]] = qsdfad[,4]*janskyConv;
} else {
newtable[["QuarteredPhot1_Jy"]] = qssfad[1]*janskyConv;
newtable[["QuarteredPhot2_Jy"]] = qssfad[2]*janskyConv;
newtable[["QuarteredPhot3_Jy"]] = qssfad[3]*janskyConv;
newtable[["QuarteredPhot4_Jy"]] = qssfad[4]*janskyConv;
newtable[["QuarteredPhot1_Deblended_Jy"]] = qsdfad[1]*janskyConv;
newtable[["QuarteredPhot2_Deblended_Jy"]] = qsdfad[2]*janskyConv;
newtable[["QuarteredPhot3_Deblended_Jy"]] = qsdfad[3]*janskyConv;
newtable[["QuarteredPhot4_Deblended_Jy"]] = qsdfad[4]*janskyConv;
}
newtable[["PixelFlux_Jy"]] = pixflux*janskyConv; cat(paste0("PixelFlux_Jy"," #Pixel Flux at the object RA/DEC, in Jansky.\n"))
} else {
cat(paste0("QuarteredPhot#_units"," #Flux contained in Four Quadrants of the Post-Convolution aperture, split along the stamp centre in x & y directions, in image units. Useful in diagnosis of bad apertures/deblends.\n"))
cat(paste0("QuarteredPhot#_Deblended_units"," #Flux contained in Four Quadrants of the Deblended Post-Convolution aperture, split along the stamp centre in x & y directions, in image units. Useful in diagnosis of bad apertures/deblends.\n"))
if (length(dim(qssfad))>1) {
newtable[["QuarteredPhot1_units"]] = qssfad[,1];
newtable[["QuarteredPhot2_units"]] = qssfad[,2];
newtable[["QuarteredPhot3_units"]] = qssfad[,3];
newtable[["QuarteredPhot4_units"]] = qssfad[,4];
newtable[["QuarteredPhot1_Deblended_units"]] = qsdfad[,1];
newtable[["QuarteredPhot2_Deblended_units"]] = qsdfad[,2];
newtable[["QuarteredPhot3_Deblended_units"]] = qsdfad[,3];
newtable[["QuarteredPhot4_Deblended_units"]] = qsdfad[,4];
} else {
newtable[["QuarteredPhot1_units"]] = qssfad[1];
newtable[["QuarteredPhot2_units"]] = qssfad[2];
newtable[["QuarteredPhot3_units"]] = qssfad[3];
newtable[["QuarteredPhot4_units"]] = qssfad[4];
newtable[["QuarteredPhot1_Deblended_units"]] = qsdfad[1];
newtable[["QuarteredPhot2_Deblended_units"]] = qsdfad[2];
newtable[["QuarteredPhot3_Deblended_units"]] = qsdfad[3];
newtable[["QuarteredPhot4_Deblended_units"]] = qsdfad[4];
}
newtable[["PixelFlux_units"]] = pixflux; cat(paste0("PixelFlux_units"," #Pixel Flux at the object RA/DEC, in image units\n"))
}
newtable[["PhotometryWarning"]] = photWarnFlag; cat(paste0(""," #Some Rudimentary Photometry Warnings. Read Carefully and Take Note!\n"))
cat(paste0(""," #PhotometryWarnings: Q - Quartered Photometry Warning; 70+% of source flux contained in a single quadrant\n"))
cat(paste0(""," S - Sky Estimate Warning; Sky estimate determined in by 3 or less bins\n"))
cat(paste0(""," X - Saturation Warning; Pixels in this object aperture are saturated\n"))
cat(paste0(""," I - Iteration Warning; This object was lost during iteration because its flux was measured to be <= 0.\n"))
newtable[["PhotometryBitWarning"]] = photWarnBitFlag; cat(paste0(""," #Photometry Warnings expressed as a bitflag := IXSQ; so if S only warning: bitflag := 0010 := 2 \n"))
write.csv(newtable,file=filename,na='NA',quote=FALSE,row.names=FALSE)
} else {
####CATALOGUE PARAMETER
newtable<-data.frame(CATA_INDEX = cat.id)
colnames(newtable)<-cata.lab; cat(paste0(cata.lab," #Catalogue ID. Duplicates are prepended with 'DuplicatedID_'\n"))
newtable[[ra.lab]] = cat.ra; cat(paste0(ra.lab," #Right Ascention. Same as provided in the input catalogue\n"))
newtable[[dec.lab]] = cat.dec; cat(paste0(dec.lab," #Declination. Same as provided in the input catalogue\n"))
newtable[[theta.lab]] = cat.theta; cat(paste0(theta.lab," #Aperture Orientation Angle. Same as provided in the input catalogue\n"))
newtable[[semimaj.lab]] = cat.a; cat(paste0(semimaj.lab," #Aperture SemiMajor Axis length, in arcseconds. Same as provided in the input catalogue\n"))
newtable[[semimin.lab]] = cat.b; cat(paste0(semimin.lab," #Aperture SemiMinor Axis length, in arcseconds. Same as provided in the input catalogue\n"))
if (exists("contam")) { newtable[[contam.lab]] = contams; cat(paste0(contam.lab," #Contaminant Flag. Same as provided in the input catalogue\n")) }
if (exists("groups")) { newtable[[group.lab]] = groups; cat(paste0(group.lab," #Grouping Flag. Same as provided in the input catalogue\n")) }
# IMAGE PARAMETERS
newtable[["NX_PIX2EDGE"]] = dx.pix; cat(paste0("NX_PIX2EDGE"," #Number of Pixels to the Nearest Edge of the Image; X-Axis. Useful for avoiding selection effects at image edges\n"))
newtable[["NY_PIX2EDGE"]] = dy.pix; cat(paste0("NY_PIX2EDGE"," #Number of Pixels to the Nearest Edge of the Image; Y-Axis. Useful for avoiding selection effects at image edges\n"))
# APERTURE SUMS & INTERMEDIATE SUMS
newtable[["SumPSF"]] = spsf; cat(paste0("SumPSF"," #Integral of the PSF. Should be the same for every object\n"))
newtable[["SumSA"]] = ssa; cat(paste0("SumSA"," #Integral of the Catalogue Aperture (i.e. the 'Prior') in pixels\n"))
newtable[["SumSFA"]] = ssfa; cat(paste0("SumSFA"," #Integral of the Post-Convolution Aperture.\n"))
newtable[["SumDFA"]] = sdfa; cat(paste0("SumDFA"," #Integral of the Deblended Post-Convolution Aperture.\n"))
newtable[["SumPSFxData"]] = spsfd; cat(paste0("SumPSFxData"," #Integral of the PSF times the image.\n"))
if (do.sky.est | get.sky.rms) {
if (magnitudes) {
# SKY PARAMETERS: Jansky
newtable[["SkyLocal_Jy"]] = skylocal*janskyConv; cat(paste0("SkyLocal_Jy"," #The measured Median Sky Level, in Jansky.\n"))
newtable[["SkyLocal_Mean_Jy"]] = skylocal.mean*janskyConv; cat(paste0("SkyLocal_Mean_Jy"," #The measured Mean Sky Level, in Jansky.\n"))
newtable[["SkyFlux_Jy"]] = skyflux*janskyConv; cat(paste0("SkyFlux_Jy"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Uses the measured Median Sky Level.\n"))
newtable[["SkyFlux_Mean_Jy"]] = skyflux.mean*janskyConv; cat(paste0("SkyFlux_Mean_Jy"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Uses the measured Mean Sky Level.\n"))
newtable[["SkyError_Jy"]] = skyerr*janskyConv; cat(paste0("SkyError_Jy"," #Error on the Median Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Determined by measuring the Error on the Median Sky Level.\n"))
newtable[["SkyError_Mean_Jy"]] = skyerr.mean*janskyConv; cat(paste0("SkyError_Mean_Jy"," #Error on the Mean Sky Flux contained in the Deblended Post-Convolution Aperture, in Jansky. Determined by measuring the Error on the Mean Sky Level.\n"))
newtable[["SkyRMS_Jy"]] = skyrms*janskyConv; cat(paste0("SkyRMS_Jy"," #RMS of the Sky Pixels calculated during the Median Sky Level calculation, in Jansky.\n"))
newtable[["SkyRMS_Mean_Jy"]] = skyrms.mean*janskyConv; cat(paste0("SkyRMS_Mean_Jy"," #RMS of the Sky Pixels calculated during the Mean Sky Level calculation, in Jansky.\n"))
} else {
# SKY PARAMETERS: units
newtable[["SkyLocal_units"]] = skylocal*janskyConv; cat(paste0("SkyLocal_units"," #The measured Median Sky Level, in image units.\n"))
newtable[["SkyLocal_Mean_units"]] = skylocal.mean*janskyConv; cat(paste0("SkyLocal_Mean_units"," #The measured Mean Sky Level, in image units.\n"))
newtable[["SkyFlux_units"]] = skyflux*janskyConv; cat(paste0("SkyFlux_units"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Uses the measured Median Sky Level.\n"))
newtable[["SkyFlux_Mean_units"]] = skyflux.mean*janskyConv; cat(paste0("SkyFlux_Mean_units"," #Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Uses the measured Mean Sky Level.\n"))
newtable[["SkyError_units"]] = skyerr*janskyConv; cat(paste0("SkyError_units"," #Error on the Median Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Determined by measuring the Error on the Median Sky Level.\n"))
newtable[["SkyError_Mean_units"]] = skyerr.mean*janskyConv; cat(paste0("SkyError_Mean_units"," #Error on the Mean Sky Flux contained in the Deblended Post-Convolution Aperture, in image units. Determined by measuring the Error on the Mean Sky Level.\n"))
newtable[["SkyRMS_units"]] = skyrms*janskyConv; cat(paste0("SkyRMS_units"," #RMS of the Sky Pixels calculated during the Median Sky Level calculation, in image units.\n"))
newtable[["SkyRMS_Mean_units"]] = skyrms.mean*janskyConv; cat(paste0("SkyRMS_Mean_units"," #RMS of the Sky Pixels calculated during the Mean Sky Level calculation, in image units.\n"))
}
}
if (!magnitudes) {
# FLUXES: Units
newtable[["PSFFlux_units"]] = psfflux; cat(paste0("PSFFlux_units"," #Final Point Source Flux, in image units.\n"))
newtable[["PSFErr_units"]] = psferr; cat(paste0("PSFErr_units"," #Error on Final Point Source Flux, in image units. Incorporates Sky Subtraction, and Sky RMS Uncertainty \n"))
newtable[["SFAFlux_units"]] = sfaflux; cat(paste0("SFAFlux_units"," #Final Blended Flux, in image units.\n"))
newtable[["SFAErr_units"]] = sfaerr; cat(paste0("SFAErr_units"," #Error on Final Blended Flux, in image units. Incorporates Shot Noise, Sky Subtraction, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DFAFlux_units"]] = dfaflux; cat(paste0("DFAFlux_units"," #Final Deblended Flux, in image units.\n"))
newtable[["DFAErr_units"]] = dfaerr; cat(paste0("DFAErr_units"," #Error on Final Deblended Flux, in image units. Incorporates Shot Noise, Sky Subtraction, Deblending, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DeblendErr_units"]] = deblerr; cat(paste0("DeblendErr_units"," #Absolute Flux Uncertainty caused by the Deblend of the Deblended Post-Convolution Aperture.\n"))
if (iterate.fluxes) {
cat(paste0(paste("DFAFlux_Iter<i>_units",sep="")," #Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. NB: These values are *not* sky subtracted and/or aperture corrected. In image units.\n"))
cat(paste0(paste("DFAErr_Iter<i>_units",sep="")," #Error on Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. In image units.\n"))
cat(paste0(paste("SumDFA_Iter<i>",sep="")," #Sum of the Deblended Post-Convolution Model after <i> iterations of Measurement, Fluxweighting, and Deblending. In pixels\n"))
if (length(dim(fluxiters))>1) {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_units",sep="")]] = fluxiters[,i];
newtable[[paste("DFAErr_Iter",i,"_units",sep="")]] = erriters[,i];
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[,i];
}
} else {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_units",sep="")]] = fluxiters[i];
newtable[[paste("DFAErr_Iter",i,"_units",sep="")]] = erriters[i];
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[i];
}
}
}
} else {
# FLUXES: Jansky
newtable[["PSFFlux_Jy"]] = psfflux*janskyConv; cat(paste0("PSFFlux_Jy"," #Final Point Source Flux, in Jansky.\n"))
newtable[["PSFErr_Jy"]] = psferr*janskyConv; cat(paste0("PSFErr_Jy"," #Error on Final Point Source Flux, in Jansky. Incorporates Sky Subtraction, and Sky RMS Uncertainty only \n"))
newtable[["SFAFlux_Jy"]] = sfaflux*janskyConv; cat(paste0("SFAFlux_Jy"," #Final Blended Flux, in Jansky.\n"))
newtable[["SFAErr_Jy"]] = sfaerr*janskyConv; cat(paste0("SFAErr_Jy"," #Error on Final Blended Flux, in Jansky. Incorporates Shot Noise, Sky Subtraction, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DFAFlux_Jy"]] = dfaflux*janskyConv; cat(paste0("DFAFlux_Jy"," #Final Deblended Flux, in Jansky.\n"))
newtable[["DFAErr_Jy"]] = dfaerr*janskyConv; cat(paste0("DFAErr_Jy"," #Error on Final Deblended Flux, in Jansky. Incorporates Shot Noise, Sky Subtraction, Deblend, and Blanks (pref) or Sky RMS Uncertainty \n"))
newtable[["DeblendErr_Jy"]] = deblerr*janskyConv; cat(paste0("DeblendErr_Jy"," #Absolute Flux Uncertainty caused by the Deblend of the Deblended Post-Convolution Aperture, in Jansky.\n"))
if (iterate.fluxes) {
cat(paste0(paste("DFAFlux_Iter<i>_Jy",sep="")," #Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. NB: These values are *not* sky subtracted and/or aperture corrected. In Jansky.\n"))
cat(paste0(paste("DFAErr_Iter<i>_Jy",sep="")," #Error on Deblended Flux after <i> iterations of Measurement, Fluxweighting, and Deblending. In Jansky.\n"))
cat(paste0(paste("SumDFA_Iter<i>",sep="")," #Sum of the Deblended Post-Convolution Model after <i> iterations of Measurement, Fluxweighting, and Deblending. In pixels\n"))
if (length(dim(fluxiters))>1) {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_Jy",sep="")]] = fluxiters[,i]*janskyConv;
newtable[[paste("DFAErr_Iter",i,"_Jy",sep="")]] = erriters[,i]*janskyConv;
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[,i];
}
} else {
for (i in 1:num.iterations) {
newtable[[paste("DFAFlux_Iter",i,"_Jy",sep="")]] = fluxiters[i]*janskyConv;
newtable[[paste("DFAErr_Iter",i,"_Jy",sep="")]] = erriters[i]*janskyConv;
newtable[[paste("SumDFA_Iter",i,sep="")]] = sdfaiters[i];
}
}
}
newtable[["ABMagDFA"]] = mags; cat(paste0("ABMagDFA"," #AB Magnitude of Final Deblended Flux\n"))
newtable[["ABMagErrDFA"]] = (2.5/log(10))*(dfaerr/dfaflux); cat(paste0("ABMagErrDFA"," #Error on the AB Magnitude of Final Deblended Flux\n"))
}
# BLANKS CORRECTION
if (blank.cor) {
if (magnitudes) {
newtable[["BlanksMeanMean_Jy"]] = blanks$randMean.mean*janskyConv; cat(paste0("BlanksMeanMean_Jy"," #Mean Value of the Mean Pixel Values in <n> Blank Apertures. In Jansky.\n"))
newtable[["BlanksMeanSD_Jy"]] = blanks$randMean.SD*janskyConv; cat(paste0("BlanksMeanSD_Jy"," #Standard Deviation of the Mean Pixel Values in <n> Blank Apertures. In Jansky.\n"))
newtable[["BlanksMeanMAD_Jy"]] = blanks$randMean.MAD*janskyConv; cat(paste0("BlanksMeanMAD_Jy"," #Median Absolute Deviation from Median of the Mean Pixel Values in <n> Blank Apertures. In Jansky.\n"))
newtable[["BlanksApMean"]] = blanks$randAp.mean; cat(paste0("BlanksApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApSD"]] = blanks$randAp.SD; cat(paste0("BlanksApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApMAD"]] = blanks$randAp.MAD; cat(paste0("BlanksApMAD"," #Median Absolute Deviation from Median of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
} else {
newtable[["BlanksMeanMean_units"]] = blanks$randMean.mean; cat(paste0("BlanksMeanMean_units"," #Mean Value of the Mean Pixel Values in <n> Blank Apertures. In image units.\n"))
newtable[["BlanksMeanSD_units"]] = blanks$randMean.SD; cat(paste0("BlanksMeanSD_units"," #Standard Deviation of the Mean Pixel Values in <n> Blank Apertures. In image units.\n"))
newtable[["BlanksMeanMAD_units"]] = blanks$randMean.MAD; cat(paste0("BlanksMeanMAD_Jy"," #Median Absolute Deviation from Median of the Mean Pixel Values in <n> Blank Apertures.\n"))
newtable[["BlanksApMean"]] = blanks$randAp.mean; cat(paste0("BlanksApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApSD"]] = blanks$randAp.SD; cat(paste0("BlanksApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
newtable[["BlanksApMAD"]] = blanks$randAp.MAD; cat(paste0("BlanksApMAD"," #Median Absolute Deviation from Median of the Integral of the <n> _Individually Masked_ Blank Apertures.\n"))
}
newtable[["NumberMeasuredBlanks"]] = blanks$nRand; cat(paste0("NumberMeasuredBlanks"," #Number of Blank Apertures measured per object. Varies object to object due to source masking.\n"))
}
if (ran.cor) {
if (magnitudes) {
newtable[["RandomsMeanMean_Jy"]] = randoms$randMean.mean*janskyConv; cat(paste0("RandomsMeanMean_Jy"," #Mean Value of the Mean Pixel Values in <n> Random Apertures. In Jansky.\n"))
newtable[["RandomsMeanSD_Jy"]] = randoms$randMean.SD*janskyConv; cat(paste0("RandomsMeanSD_Jy"," #Standard Deviation of the Mean Pixel Values in <n> Random Apertures. In Jansky.\n"))
newtable[["RandomsApMean"]] = randoms$randAp.mean; cat(paste0("RandomsApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
newtable[["RandomsApSD"]] = randoms$randAp.SD; cat(paste0("RandomsApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
} else {
newtable[["RandomsMeanMean_units"]] = randoms$randMean.mean; cat(paste0("RandomsMeanMean_units"," #Mean Value of the Mean Pixel Values in <n> Random Apertures. In image units.\n"))
newtable[["RandomsMeanSD_units"]] = randoms$randMean.SD; cat(paste0("RandomsMeanSD_units"," #Standard Deviation of the Mean Pixel Values in <n> Random Apertures. In image units.\n"))
newtable[["RandomsApMean"]] = randoms$randAp.mean; cat(paste0("RandomsApMean"," #Mean Value of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
newtable[["RandomsApSD"]] = randoms$randAp.SD; cat(paste0("RandomsApSD"," #Standard Deviation of the Integral of the <n> _Individually Masked_ Random Apertures.\n"))
}
}
if (!no.psf) {
newtable[["MinApCorr"]] = ApCorr; cat(paste0("MinApCorr"," #Value of the Multiplicative Minimum Aperture Correction. This correction is important, and can _only_ improve an objects flux determination.\n"))
newtable[["MaxApCorr"]] = WtCorr; cat(paste0("MaxApCorr"," #Value of the Multiplicative Maximum Aperture Correction. This correction can cause excess flux-boosting systematically as a function of object morphology, and is provided __as a guide only__\n"))
}
# Misc.
newtable[["PhotometryWarning"]] = photWarnFlag; cat(paste0(""," #Some Rudimentary Photometry Warnings. Read Carefully and Take Note!\n"))
cat(paste0(""," #PhotometryWarnings: Q - Quartered Photometry Warning; 70+% of source flux contained in a single quadrant\n"))
cat(paste0(""," S - Sky Estimate Warning; Sky estimate determined in by 3 or less bins\n"))
cat(paste0(""," X - Saturation Warning; Pixels in this object aperture are saturated\n"))
cat(paste0(""," I - Iteration Warning; This object was lost during iteration because its flux was measured to be <= 0.\n"))
newtable[["PhotometryBitWarning"]] = photWarnBitFlag; cat(paste0(""," #Photometry Warnings expressed as a bitflag := IXSQ; so if S only warning: bitflag := 0010 := 2 \n"))
write.csv(newtable,file=filename,na='NA',quote=FALSE,row.names=FALSE)
}
if (!is.null(env)) { detach(env) }
return=NULL
}
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