#!/bin/csh -f # End-2-end reduction of data observed on 2004-04-8/9: # H2O masers at 658 GHz for several sources. # P.I. 690GHz campaign in 2004 spring. # The script was used for preparation of Miriad Users Guide # for the reduction of SMA data. # jhz 2005-02-02 #goto continue #continue # #load data and convert mir format to miriad format #the original data has 128 channels per chunk #smalod resamples the data to 64 channels per chunk # \rm -r h2o.lsb h2o.lsb.tsys smalod in=/home/miriad/SMAdata/040408:08:55:31/ \ rsnchan=64 out=h2o sideband=0 nscans=10,1430 #inspect data smauvplt vis=h2o.lsb axis=time,ampl device=/xs nxy=5,3 #tsys correction \rm -r h2o.lsb.tsys smafix vis=h2o.lsb out=h2o.lsb.tsys device=/xs xaxis=antel \ yaxis=systemp nxy=3,2 yrange=0,15000 rmsflag=2 dofit=2 \ options=tsyscorr,tsysswap smavarplt vis=h2o.lsb.tsys device=/xs xaxis=antel \ yaxis=systemp nxy=3,2 #inspect data again smauvplt vis=h2o.lsb.tsys axis=time,ampl device=/xs nxy=5,3 #inspect spectral data smauvspec vis=h2o.lsb.tsys \ select='source(why*)','time(9:30,10:20)' \ interval=100 \ hann=7 axis=freq,ampl device=/xs nxy=5,3 #flag data: ant 2 are flagged uvflag vis=h2o.lsb.tsys \ select='ant(2)' flagval=flag #determine bandpass. #Using weight=3 because calculation of #sigma from original systemp corrupts. smamfcal vis=h2o.lsb.tsys select='source(ve*,ne*)' \ weight=3 refant=3 polyfit=0,0 interval=60 # #check bandpass # smagpplt vis=h2o.lsb.tsys device=fig4.5.ps/vcps \ yaxis=amp,phase \ options=bandpass,opolyfit \ polyfit=2 nxy=1,5 # #flux scale and gains. The flux density of 53.4 Jy for #Callisto is assumed. Also, no phase calibrator is included #in the observation. mfcal vis=h2o.lsb.tsys select='source(cal*)' \ refant=3 interval=1000 \ options=nopassol flux=53.4 # #smablflag, to flag bad integrations smablflag vis=h2o.lsb.tsys device=/xs axis=time,ampl # #apply and select those spectral windows near/include #the masers only apply the gain scale not bpass and #time-dependent gains applied. # \rm -r h2o.lsb.tsys.cal uvaver vis=h2o.lsb.tsys out=h2o.lsb.tsys.cal \ select='window(11,12,13,14,15,16,17,18)' # #uvflag vis=h2o.lsb.tsys.cal flagval=flag #breaks the file into single source # \rm -r *.658128 uvsplit vis=h2o.lsb.tsys.cal options=nowindow # #plot the spectra of individual sources and make a hard copy # smauvspec vis=whya.658128 \ hann=7 interval=1000 axis=freq,ampl \ device=why.ps/vcps nxy=2,5 # #plot the spectra of individual sources on an x window device. # smauvspec vis=whya.658128 \ hann=7 interval=1000 axis=freq,ampl \ device=/xs nxy=2,5 # # cp whya data to a new one which will be further corrected # for the residual errors using selfcal. In fact, in this # observations, there were no adequate calibrator for antenna # gains. We use the maser spot for calculating the antenna # gains. # \rm -r whya.selfcal \cp -r whya.658128 whya.selfcal # #selfcal phase with point source model # selfcal vis=whya.selfcal select='window(4)' \ interval=10 options=pha \ refant=3 line=channel,16,24,1 # # make dirty map # \rm -r whya.map whya.beam whya.icmp invert vis=whya.selfcal map=whya.map beam=whya.beam \ imsize=512,512 cell=.2 sup=0 select='window(4)' \ line=channel,16,24,1 # clean map clean map=whya.map beam=whya.beam out=whya.icmp gain=0.1 \ cutoff=0 niters=500 \ region='boxes(225,225,287,287)(1,16)' # restore image \rm -r whya.icln restor model=whya.icmp beam=whya.beam map=whya.map \ out=whya.icln cgdisp in=whya.icln type=c xybin=1,1 device=/xs \ nxy=4,4 labtyp=arcsec,arcsec,absghz \ options=full,beambr,wedge,trlab,3val \ lines=1,2 csize=.8,.8,0.8 slev=a,200 \ levs1=-20,20,30,40,50,60,70,80,90 \ region='arcsec,boxes(-8,-8,8,8)(1,16)' selfcal vis=whya.selfcal select='window(4)' \ interval=7 options=pha \ refant=3 line=channel,16,24,1 model=whya.icmp # make dirty map again \rm -r whya.map whya.beam whya.icmp invert vis=whya.selfcal map=whya.map beam=whya.beam \ imsize=512,512 cell=.2 sup=0 select='window(4)' \ line=channel,16,24,1 # clean map clean map=whya.map beam=whya.beam out=whya.icmp gain=0.1 \ cutoff=0 niters=500 \ region='boxes(225,225,287,287)(1,16)' # restore image \rm -r whya.icln restor model=whya.icmp beam=whya.beam map=whya.map \ out=whya.icln cgdisp in=whya.icln type=c xybin=1,1 device=/xs \ nxy=4,4 labtyp=arcsec,arcsec,absghz \ options=full,beambr,wedge,trlab,3val \ lines=1,2 csize=.8,0.8,0.8 slev=a,200 \ levs1=-20,20,30,40,50,60,70,80,90 \ region=arcsec,'boxes(-8,-8,8,8)(1,16)' #selfcal amp with clean point model selfcal vis=whya.selfcal select='window(4)' \ interval=12 options=amp \ refant=3 line=channel,16,24,1 model=whya.icmp # make dirty map \rm -r whya.map whya.beam whya.icmp invert vis=whya.selfcal map=whya.map beam=whya.beam \ imsize=512,512 cell=.1 sup=0 select='window(4)' \ line=channel,16,24,1 # clean map clean map=whya.map beam=whya.beam out=whya.icmp gain=0.1 \ cutoff=0 niters=500 \ region='boxes(225,225,287,287)(1,16)' # restore image \rm -r whya.icln restor model=whya.icmp beam=whya.beam map=whya.map \ out=whya.icln # make contour images from the image cube cgdisp in=whya.icln,whya.icln type=p,c \ xybin=1,1 device=fig4.8.ps/vcps \ nxy=4,4 labtyp=arcsec,arcsec \ options=full,beambr,wedge,trlab,3val \ lines=1,2 csize=.8,.8,0.8 slev=a,1000 \ levs1=-30,30,40,50,60,70,80,90 \ region=arcsec,'boxes(-8,-8,8,8)(1,16)' \ range=20000,50000,lin,2 cols1=7 # do statistics on the image cubes imstat in=whya.icln region='boxes(10,10,50,50)' \ beam=whya.beam device=/xs exitThe Miriad command lines can be written in other shell scripts.