dS = float(Dnoise[k][l])
dT = float(Dtemperr[k][l])
if S == 0:
mass[k][l] = 0
masserr[k][l] = 0
if S != 0:
mass[k][l] = massF(S,T,kappa,d,temp_mi)
masserr[k][l] = mass_errF(S,T,dS,dT,temp_mi,temperr_mi)
Imasserr.flush()
Imass.flush()
######
#MASS#
######
#convert back to sdf
ndf2fits.fits2ndf(massFITS)
ndf2fits.fits2ndf(masserrFITS)
mass = 'SMM/'+region+'/Mass'+str(I)+'.sdf'
masserr ='SMM/'+region+'/masserr'+str(I)+'.sdf'
#Extract TOTAL clump mass as number
cmd = '%s/stats ndf=%s %s'%(kapdir,mass,'> /dev/null')
os.system(cmd)
cmd = '%s/parget parname=%s applic=%s'%(kapdir,'total','stats')
status, output = commands.getstatusoutput(cmd)
mi = float(output)
del output
#calculate frac error on the mass and find its mean value, on which the mean mass error is based.
fracmass = 'SMM/'+region+'/temp/fracmass_clump'+str(I)+'.sdf'
cmd = '%s/div in1=%s in2=%s out=%s'%(kapdir,masserr,mass,fracmass)
########### Bulk Code ############# #Method A = RUMBLE #Method B = CHEN inA_fits = 'PerseusWest_20150317-autotemperatureWCSALN_SMT.fits' errA_fits = 'PerseusWest_20150317-autotemp_errorWCSALN_SMT.fits' inB_fits = 'tempMap_Her+850_clean.fits' errB_fits = 'TempMapErr_Her+850_clean.fits' Beta_fits = 'betaMap_Her+850_clean.fits' errBeta_fits = 'betaMapErr_Her+850_clean.fits' inA = ndf2fits.fits2ndf(inA_fits) inB = ndf2fits.fits2ndf(inB_fits) errA = ndf2fits.fits2ndf(errA_fits) errB = ndf2fits.fits2ndf(errB_fits) k = 0 TA = [] TB = [] EA = [] EB = [] Beta = [] eBeta = [] count_lo = 0 count_hi = 0
for i in range(0, row):
for j in range(0, column):
T = float(temp_data[i][j])
S = float(s850_data[i][j])
Mass_data[i][j] = massF(S,T,kappa,d)
Mass15_data[i][j] = massF(S,20,kappa,d)
#if Mass[i][j] > 0:
#print Mass[i][j]
#output new values back to FITS file and save
image_mass.flush()
image_mass.close()
image_mass15.flush()
image_mass15.close()
ndf2fits.fits2ndf(massFITS)
ndf2fits.fits2ndf(mass15FITS)
#CALCULATE Column density
#Convert map of mass (in solar masses) into column density (in H2 cm-2) and Extinction (mag)
M_x = 1.989E33 #g
N = 1
au = 14959787100000 #cm
m_h = 1.67262178E-24 #g
mu = 2.8 #333 #ratio of H2 to He (Kauffmann et al. 2008)
#pixel area
A = ((((a*d)*au)**2.0)*N) #in cm^2
f = M_x/(mu*m_h*A) #column density per cm^2
mass = 'CDmaps/mass/'+region+'_mass.sdf'
# freefree div2 = "%s/div in1=%s in2=%s out=%s" % (kapdir, mask450FF, mask850FF, ratioFF) os.system(div2) ndf2fits.ndf2fits(ratio) ndf2fits.ndf2fits(ratioFF) temperature(ratio, ratio_fits, ratio_fits, 1.8, "FALSE") temperature(ratioFF, ratioFF_fits, ratioFF_fits, 1.8, "FALSE") mv1 = "mv %s %s" % (ratio_fits, temp_fits) mv2 = "mv %s %s" % (ratioFF_fits, tempFF_fits) os.system(mv1) os.system(mv2) ndf2fits.fits2ndf(temp_fits) ndf2fits.fits2ndf(tempFF_fits) # compare temp maps submap = "maps/s21/submap.sdf" sub = "%s/sub in1=%s in2=%s out=%s" % (kapdir, tempFF, temp, submap) os.system(sub) """ ################################ #### calculate columndensity ### #see run26 ################################ #deffine constants kappa = 0.012 #cm^2 g^-1 d = 500 #pc