REDUCE Command List
last updated 07/1995
(ERRCMD is called if a typo or wrong command is entered)
(type in format of command, see in subroutines)
When user needs to type in something, "INPUT" is given.
Command What it does Calls on subroutine(s)
-----------------------------------------------------------------------------
term n set or print priority level of terminal misc.f eieio.f
prin n set or print priority level of printer misc.f eieio.f
page eject page on priority 2 printer misc.f page.f
line ? select which 16 lines of header to show misc.f hlines.f
leng n set array length to n pixels misc.f lentym.f
tzer t set minimum integration time to t secs. misc.f lentym.f
lati lat set latitude of observatory misc.f latude.f
disk# displays scan #s and name fields in DISK1 misc.f dsklst.f
or DISK2
head# n1 -n2 displays headers of individual scans misc.f hedsho.f
in list,from DISK1 (header1) or
DISK2 (header2)
edit# n1-n2 user edits indicated scan headers from misc.f editit.f
indicated files. edit1=DISK1;edit2=DISK2
(include details about commands for edit?)
dump# n1 -n2 displays data from indicated scans from misc.f dumpit.f
indicated file.
forget# n lose all DISK1 *or* DISK2 scans after n-1 misc.f forget.f
and pointer goes to n.
reset diskone clean DISK file, DISK1, DISK2, plot *or* misc.f reset.f
disktwo wavelength calibration file
lambda a,b,both
plot
flag displays flag #s,names and current values misc.f flag.f
blok examine contents of common blocks misc.f o1h.f
aero set variables and flags for aerobee misc.f observ.f
observatory, loads wing and thermal
correction files
pbo set variables and flags for PBO, misc.f observ.f
loads wing and thermal correction files
wupp set variables and flags for WUPPE, misc.f observ.f
loads wing and thermal correction files
reload accum brings in scans from the current misc.f dskrel.f
norm file of the reduced data *tape*
flux
offset
pol
detbkg
lambda a,b,both n set arrays wavelength cal.
to that found in header of
scan n
rema use rest of line as a remark misc.f
save save contents of common blocks in misc.f savecm.f
savecm.ret
flus save contents of common blocks in misc.f savecm.f
savecm.ret
fixa n fix PBO array A by replacing even number misc.f fixa.f
pixels by average of adjacent odd # pixels
in DISK1 scan n
fixb n fix PBO B array by replacing even number misc.f fixb.f
pixels by average of adjacent odd # pixels
in DISK1 scan n
ascd n1 -n2 displays DISK2 file for individual scans misc.f ascdmp.f
from individual file in text file format
to terminal and file; INPUT file name
dele just continue
mark gives x,y cursor posn. for emission line misc.f spectr.f
in scoped spectrum
cent finds centroid of emission line in scoped misc.f spectr.f
spectrum
read1 read DISK1 or DISK2 scan from another file misc.f read.f
read2 in another directory and put it in next
position in current DISK2 file. INPUT
name of file to use.
cont (only if lfresh not equal to 1): mark 4 misc.f contin.f
points for continuum calculation for
equivalent width.
widt (only if lfresh not equal to 1): calculate misc.f width.f
equivalent width.
flam n convert F-nu to F-lambda, set flag for misc.f flamit.f
F-lambda, save to DISK2
logf n convert F-nu to F-lambda, set flag for misc.f flamit.f
log F-lambda, save to DISK2
ylim n calculate min. and max. values for DISK1 misc.f ylimits.f
or DISK2 scans within given pscale limits.
dred n INPUT E(B-V) for scan n misc.f dreden.f
dereddens spectrum, save to DISK2 unred.f
dsks opens DISK1 and DISK2, acc., norm., and misc.f dskset.f
flux buffers. INPUT DISK1 and DISK2 file
names.
dats opens wavelength cal., extinction, flux misc.f datset.f
standards and wing corr. files; INPUT
names of files
vshi shifts PBO F-lambda to a given V magnitude misc.f vshift.f
Need to INPUT a V magnitude.
log n Logs DISK2 scan n and create a new one misc.f logit.f
offs n1 -n2 prepares acc. buffers for offset calc. proces.f offset.f
then does calculation
add n1 -n2 prepare acc. buffers for adding proces.f addset.f
addo n1 -n2 prepare acc. buffers for adding, clean proces.f addset.f
and subtract offset
norm normalize arrays, set flags proces.f b2c.f
stor n1 -n2 LSTATA = 0? print ERROR IN SEQUENCE proces.f strset.f
LDETB = 1? call detb.f, subtract detector
background
LSUBT NE 0? call subt.f,sub. background
LWING NE 0? call wing.f, removes scattered
light, HVPS, and noise
LTIME NE 0? call tyme.f, div. by exposure
time
LNORM NE 0? call norm.f, normalizes data
LTHRM NE 0? call thrm.f, thermal corr.
LEXTI NE 0? call exti.f, extinction corr.
LFLUX NE 0? call flux.f, flux calibration
NOGO NE 0? write to DISK2
addp n1 -n2 prepare acc. and pol. buffers for adding, proces.f addpol.f
clean and offset
pols n1 -n2? LSTATP = 0? print ERROR IN SEQUENCE proces.f polsto.f
LSTATA = 0? print ERROR IN SEQUENCE
LDETB = 1? call pdetb.f, subtract detector
background
LSUBT NE 0? call psubt.f,sub. background
LWING NE 0? call pwing.f, remove scattered
light, HVPS, and noise
LTIME NE 0? call ptime.f, div. by exposure
time
LNORM NE 0? call pnorm.f, normalizes data
LTHRM NE 0? call pthrm.f, thermal corr.
LEXTI NE 0? call pexti.f, extinction corr.
LFLUX NE 0? call pflux.f, flux calibration
NOGO NE 0? write to DISK2
detb n1 -n2 prepare ac. buffers for adding, find proces.f detbkgd.f
detector background, and put in buffers
drop INPUT keyword, drop range, drop scans proces.f drop.f
out of range
psca p1 p2,) INPUT pixel limits or select autoscale plotse.f pscale.f
wsca w1 w2,) INPUT wavelength limits or sel. autoscale plotse.f wscale.f
ysca y1 y2,) INPUT y limits or select autoscale plotse.f yscale.f
xbox n INPUT width of box in inches plotse.f boxdef.f
ybox n INPUT height of box in inches plotse.f boxdef.f
penup data plotted as points plotse.f pennup.f
pendown data plotted as histogram plotse.f pennup.f
capt INPUT caption to appear over box and on plotse.f pltcap.f
printer whenever the plot is executed
scop n clear plot, write caption, plot scan on plotse.f a2b.f
terminal
plot n clear plot, write caption, plot scan in plotse.f a2b.f
file
endp n clear and close plot device plotse.f a2b.f
clea n clear and close plot device plotse.f a2b.f
scru n1 -n2 INPUT Angstroms/pixel, and shift in specia.f f2a.f
Angstroms;resample spectra on to a
standard linear wavelength scale and store
comb opts n1-n2 combine scrunched scans together specia.f f2b.f
and write to DISK2
util cmd=syke? convert DISK1 scans from SYKES specia.f o1g.f
to 7 track pixel format by
shifting 48 pixels to right
cmd=pshi? INPUT pixel shift then shift
scans in list by this amount
cmd=glit? INPUT bad pixels or wavelengths
sets N pixels to mean of 2*N
on either side of bad ones
cmd=zap? INPUT bad pixels or wavelengths
then zeroes out pixels
cmd=addc? INPUT a constant; add constant
to scan and store scan
cmd=mulc? INPUT a constant; multiply
scan by constant and store scan
cmd=log? take log of data in DISK2 scan
and store in new DISK2 scan
tapi error message
tapo error message
lamb wavelength cal. subprocess;see below lambda.f
stan flux cal. subprocess;see below stand.f
oldp old pol. red. subprocess;see below ppolar.f
pola pol. red. subprocess;see below rpolar.f
back background subprocess;see below back.f
gauss Gaussian fit subprocess; see below gas.f
chan change subprocess;see below change.f
ripp ripple subprocess;see below ripple.f
exit go to exit
*******************************************************************************
lambda.f;wavelength calibration subprocess
User inputs command
Command What it does Calls on subroutine(s)
-----------------------------------------------------------------------------
retu Initializes matrices, variables, and setlam.f
clears the plots
opens savecm.ret and writes vars. putlcw.f
rese Resets and clears plot setlam.f
scan1 n1 -n2 Marks scans for use in wavelength cal. marklam.f e2a.f
scan2 n1 -n2 "" marklam.f e2b.f
lxx1 n1 -n2 "" stlam1.f e2d.f
flags lines; gives processor a fit for array
lxx2,uxx1 finishes start e2f.f
disp n displays array's calibration scan on displam.f e2c.f
terminal, marks and numbers pts. used
in fit
plot n sends to a plot file array's calibration displam.f e2c.f
scan, with marks and pts. used
endp clear and close plot displam.f e2c.f
rest n recalculate fit with specified lines worklam.f e2e.f
given full weight
stri n recalculate indicated array's fit with worklam.f e2e.f
specified line given 0 weight
dump dumps wavelength cal. blocks worklam.f e2e.f
acce n accept fit for array worklam.f e2e.f
******************************************************************************
stand.f; flux calibration subprocess.
User inputs commands
Command What it does Calls on subroutine(s)
-----------------------------------------------------------------------------
retu Clear and close plot then setstd.f
save flux cal. variables to savecm.ret putlcf.f
capt INPUT caption, write on plot pltcap.f
rese reinitialize as if starting again setstd.f stdset.f
scan1 prepare buffers for adding then d2a.f
subtract background, wing and thermal d2b.f
correction, extinction corr. then
process data and put std. curve in buffer stdpro.f
scan2 process data, put std. curve in buffer d2c.f
acce n accepts standard curve, writes to buffer finstd.f stdyep.f
dump dumps data in local common blocks finstd.f stddmp.f
disp n close plot, display response wave of array workst.f d2d.f
plot n clear and close plot, save response wave workst.f d2d.f
of array to a plot file
shif n? display response curve, enter shift mode, workst.f d2d.f
INPUT from user=perform action with cursor:
multiply shift curves
stri n? display response curve, enter strike mode, workst.f d2d.f
INPUT from user=strike with cursor points
to delete.
drop n? display response curve, enter drop mode, workst.f d2d.f
INPUT from user=mark with cursor curves to
be deleted
endp clear and close plot workst.f d2d.f
******************************************************************************
ppolar.f; old polar. reduction subprocess.
User inputs commands
Command What it does Calls on subroutine(s)
-----------------------------------------------------------------------------
retu clear and close plot, saves vars. to file
rema use rest of line as a remark
rese clear plot, initialize variables plset.f
reca S F clear plot, reload scan S and plin.f plfrin.f
fit F into calibration buffer
pola S F print polarization for scan S, fit F plout.f
resi S F compute residuals of scan S, fit F plout.f
minus fringes;store in DISK2
frin clear screen of plot, load scans for fit; plin.f
do fringe cal., load cal. buffer; plfrin.f
evaluate fringe, store data in DISK2 plout.f
save local common blocks to savecm.ret
fit clear plot, load scans for fitting; plin.f
load fringes then fit using current cal.; plfit.f
evaluate fit, store data on DISK2; plout.f
save local common blocks to savecm.ret
diff S1 S2 calculate diffsum (S1-S2)/(S1+S2) and plin.f
store in reduced data disk file
now l1 l2 set weights for wavelengths plutil.f
l1 to l2 to 0
grid n set up spline grid n intervals from plutil.f
lambda1 to lambda2, equally space in
1/lambda
flat n1 -n2 INPUT order of flattening polynomial 1-5 plutil.f
and divide DISK2 scans by fitted polynomial
smoo n1 -n2 INPUT FWHM of smoothing Gaussian in pixels plutil.f
and smooth DISK2 scans n1 to n2
grey n n1 -n2 grey shift scan list to match plutil.f
scan n and store list in DISK2
dump writes out values of vars. in chosen plutil.f
common blocks
gang n gang together n pixels in plotting plpset.f
logx set flags for log plotting in x,y axes plpset.f
capt input caption for plotting plpset.f pltcap.f
forg n delete DISK1 or DISK2 scans after n-1 plpset.f forget.f
and reset pointer to n
psca p1 p2, ) set pixel limits or autoscale plpset.f pscale.f
wsca w1 w2, ) set wavelength limits or autoscale plpset.f wscale.f
ysca y1 y2, ) set y limits or autoscale plpset.f yscale.f
penup data plotted as points plpset.f pennup.f
pendown data plotted as histogram plpset.f pennup.f
plot(over) n set flag for plot, clear, plot scan plpset.f
scop(eover) n set flag for scop, clear, plot scan plpset.f
endp clear and close plot plpset.f
clea clear and close plot plpset.f
util see above o1g.f
******************************************************************************
rpolar.f; polar. reduction subprocess.
User inputs commands
Command What it does Calls on subroutine(s)
-----------------------------------------------------------------------------
lcal name Lyot fourier red.; read calibration file lrpolar.f
name.lcal into buffers
lrec CAL n1-n2 Lyot fourier red.; change calib. for lrpolar.f
pol. scans from that in header to
cal. file CAL.cal
lpol n Lyot fourier red.; compute Q,U,V, and lrpolar.f
error scans from diffsum calc. (n),
chi-square it and save to DISK2
diff S1 S2 Lyot fourier red.; compute diffsum lrpolar.f
(S1-S2)/(S1+S2) and store in DISK2
lred Lyot fourier red. lrpolar.f
lnew name Lyot cal.; create new lcal file NAME.cal lcalib.f
lsim n Lyot cal.; create simulated diffsum scan lcalib.f
using scan n's header as template
lpre n Lyot cal.; use diffsum n and scrunch it lcalib.f lprepare.f
lsig n Lyot cal.; calculate Lyot signal lcalib.f
functions for diffsum scan n, store LDAT
lcev n l Lyot cal.; evaluate demodulation shift and lcalib.f
ratio cal. functions from Lyot envelopes
for fringe calculation of scan n, and level
l=-1,0,1,2
lexp n fn Lyot cal.; expand Lyot functions and store lcalib.f
in DISK2;fn no. is 1-15
lres ldat n Lyot cal.; calculate residual between LDAT lcalib.f
and diffsum scan n
hcal name 1/2 wave;load cal. file name.hcal hrpolar.f
hrec cal n1-n2 1/2 wave; change cal. for Q,U,Error from hrpolar.f
one in header to cal.hcal for scans n1 to n2
hpol n1 -n2 1/2 wave; compute Q,U,Error from raw DISK2 hrpolar.f
spectra in scan list n1 to n2
hrot n 1/2 wave; INPUT degrees to rotate hrpolar.f
pscan n;saves new pol. scan
hpri n1 -n2 1/2 wave;print out (v), Q,U,E,P,PA for hrpolar.f
pol scans n1 to n2 between pscale and
wscale limits. for unbinned printouts of
all pixels, print average only
hcom n1 -n2 1/2 wave; do error weighted combinations hrpolar.f
of polarization scans n1 and n2....
hadd n1 -n2 1/2 wave; do vector addition of pol. scans hrpolar.f
n1 and n2 and ...
hred (o) s1-s2 1/2 wave;go from DISK1 scan hrpolar.f
pair lists to Q,U,E DISK2 scans; options (o)
include WUPPE addpol (pcor,ycor,pycor); this
option must come first.
hsco(peover) n 1/2 wave;scope pol. scan n hrpolar.f
with optional signal dependent binning
hplo(tover) n 1/2 wave;plot pol. scan n hrpolar.f
with optional signal dependent binning
xylo 0,1 0,1 1/2 wave; rquest linear(0) or hrpolar.f
log(1) plotting for x,y, axes, linear for Q,U
endp 1/2 wave; clear and close plot hrpolar.f
INPUTs as with other occurrence of cmd
capt 1/2 wave; INPUT caption for plot hrpolar.f pltcap.f
INPUTs as with other occurrence of cmd
penup 1/2 wave; do points on plot hrpolar.f pennup.f
INPUTs as with other occurrence of cmd
pendown 1/2 wave; do histogram on plot hrpolar.f pennup.f
INPUTs as with other occurrence of cmd
symb l1 s l2.. 1/2 wave; request alternate hrpolar.f
plotting symbols (s=1 char.) for Q,U
plot between wavelengths l1 and l2....
psca p1 p2,) 1/2 wave;set pixel limits or autoscale hrpolar.f pscale.f
INPUTs as with other occurrence of cmd
wsca w1 w2,) 1/2 wave;set wave. limits or autoscale hrpolar.f wscale.f
INPUTs as with other occurrence of cmd
xsca x1 x2,) 1/2 wave;set x limits or autoscale hrpolar.f xscale.f
INPUTs as with other occurrence of cmd
ysca y1 y2,) 1/2 wave;set y limits or autoscale hrpolar.f yscale.f
INPUTs as with other occurrence of cmd
xbox F 1/2 wave;set box to be F inches wide hrpolar.f boxdef.f
ybox F 1/2 wave;set box to be F inches high hrpolar.f boxdef.f
hasc n s 1/2 wave;print out s=(V), Q,U,E,P,PA for hrpolar.f
pol scan n between pscale and wscale limits.
for unbinned printouts of all pixels.
hnew name 1/2 wave cal.;create new cal. file using hcalib.f
current one as default; can INPUT new #s
makes name.cal
hdeb p c 1/2 wave cal.; set parameters for hpol hcalib.f
debug printout;p=pixel for full printout,
c=min. chi-squared for large chi-sq printout
hopt l p wts (more) 1/2 wave cal.;optimization cmd for hcalib.f
1/2 wave filter cal.; INPUT variables and
amount to vary; print residuals and write
optimized data to temp. file; l=logfile,
p=polfile, wts (optional)=weights for optimization
and more is set for more than one hpol set.
wfil n 1/2 wave cal.;filter scan n for high freq. hcalib.f
noise. INPUT Gaussian signal width in freq.
channels; get scan, mult. by Fourier filter,
transform back and store
wopt (A,B,W) SA... 1/2 wave cal.; optimization cmd for hcalib.f
scattered light calib.;INPUT polarizer
model name (?choices) and pixel boundaries.
A,B,W=A or B array, WUPPE. SA=1st scan of 6
for each star. Calculate scat. fns. and save
wabx 1/2 wave cal.; calculate Fourier wing fns. hcalib.f
using exponential and delta fns, includes
high freq. noise suppression. INPUT values for
exp. and delta fns.; put in buffers
wmod 1/2 wave cal.; INPUT parameters of Fourier hcalib.f
wing filter;computes transform of model
line, divide scan transform by filter
transform;transform back and store.
syn n l 1/2 wave cal.; creat synthetic spectrum from hcalib.f
model using Gaussian;write to DISK2;n=scan,
l=linelist.
wsyn n s 1/2 wave cal.;create Fourier filter by hcalib.f
dividing transform of scan n by
transform of syn. spectrum s
wing n f 1/2 wave cal.;compute scattering corr. hcalib.f
in scan n with Fourier filter f
wlod t c n.. 1/2 wave cal.;load file c=calname.ret with hcalib.f
filter fns. in scan n...;t=type
pmak n Reads in mongo-like file of wavelength, panlyz.f
bin,Q, U,Err (plus V, if 'lyot' mode).
Uses header from named Q or V scan (n).
isre p1 -p2 removes Serkowski-law interstellar pol. panlyz.f
from INPUTTED pol. scans and stores results
as new scans of same typein DISK2. INPUT
PA(deg),Pmax (%), WMAX(Ang), DPA (deg), and
and K'. DPA is in deg/inverse micron
isfi p1 -p2 perform fit of Serkowski ISP to scans in panlyz.f
pol. scan list. INPUT PA, P, Wmax,DPA, K1
and which ones to vary;fit parameter is sum
of chisq(Q)+chisq(U) for all scans
stfi p1 -p2 perform fit of Serkowski IS pol to scans panlyz.f
in pol. scan list. Residual is "intrinsic
pol." having same PA at all wavelengths.
INPUT is same as for isfi.
pflu q f output polarized flux in F*Q, F*U, and panlyz.f
F*ERR scan set from Q scan q and flux scan f
psep n separate pol. scan n into 2 pol. scans panlyz.f
with specified PAs. Results have all
linear pol. rotated into Q
pfew q f compute flux and pol. flux equivalent panlyz.f
width for lines in specified scan;q=Q scan,
f=flux scan. INPUT cont, line, cont
wavelength, EW0 (the underlying line to
be removed first)
pfil q f computes filter pol. data from Q scan q panlyz.f
and flux scan f. Reads in filter bandpass curve
from file FILE.fil in USERDATA dir.
INPUT file name and weights for filter index
phar q does a weighted least-squares fit of a panlyz.f
series of Q,U,Err scans to the second
harmonic of a known binary eph.
make n MAKE2;creates a new scan with anything panlyz.f
you want in it. Uses header of scan n as
template; INPUT model where model is a file
in current dir. with data in mongo format
OR INPUT poly coefficients: y=a+b*x+...
up to 6 coeff.
psim p1 -p2 generate an artifical spectrum; INPUT time psim.f
spcmag,mode, model parameters;load in cal.
and generate spectrum
rema store rest of line as remark
retu return to main program
****************************************************************************
back.f: Background/noise statistics subprocess
User inputs commands
Command What it does Calls on subroutine(s)
-----------------------------------------------------------------------------
pixl p n1 -n2 list value of pixel p in scan list noise.f
gang n gang n pixels together in noise.f
pixlist and noise
nois d n1 -n2 calculate avg, rms, skew, dev. dist noise.f
of scans, store in DISK2;d=despike; if
requested, remove pixels with dev>x RMS
drif on/off turn on or off drift compensation in noise.f
noise
four n1 -n2 INPUT window apodization factor;apodize noise.f
from ends of data;for each scan, store
real, imag., and power in Fourier trans-
form in next 3 DISK2 scans
stat n1 -n2 print out avg., rms, pixel #s of 32 noise.f
largest values, and number of pixels in
ranges 0-AVG/4...AVG*31/4-8*AVG
corr n1 n2 cross-correlate scan1 and scan2 and noise.f
store in DISK2
adds n1 -n2 performs 'add S store' on every scan noise.f
in series
time n1 -n2 auto-correlate a time-series of n scans noise.f
in DISK2 and create a new scan
effi calc. system efficiency from norm and noise.f
flux buffers and store in DISK2
offs set n1-n2 get offset per frame from scans and dark.f
remo n1-n2 put in DISK1 scan, remove if desired
dark n1 -n2 assume DISK1 scans are pure diode dark, dark.f
correct for non-linearity
pyse n1 -n2 set/restore pitch, yaw errors in listed wpycor.f
D1 headers
pyad n1 -n2 add/stores A/B scans for one filter pair wpycor.f
sep. for each of 32 Y bins in DISK1 scan list
pyco n1 -n2 combine corr. A/B flatfield ratio vs. yaw wpycor.f
for different stars/filter pairs in DISK2
scan list
pylo A/B B-NORM load FFCOR file and compute stellar Ap2 wpycor.f
and diffuse Ap2,4,6,7,8 NORMS from B NORM and
A/B D2 scans
pyso n1 -n2 read scans in D1 list from another D1 wpycor.f
list, sorted by any keyword in header
pspc n1 -n2 update pitch estimate from spect. data wpycor.f
using auto-corr. of B array for DISK1 scans
in list
yspc n1 -n2 update yaw error based on A/B glitch wpycor.f
indices in header in DISK1 scan list
xtin n1 -n2 reads extinction curve file FILE.xtc, anlyz.f
normalize it and apply to scan list
matc S0 n1-n2 match scans in scan list to flux anlyz.f
between 2 wavelengths. INPUT W1 and
W2 for match interval
muls S1 S2 compute S1*S2, store in DISK2 anlyz.f
div S1 S2 compute S1/S2, store in DISK2 anlyz.f
lins S1 S2 compute S1+const*S2, store in DISK2 anlyz.f
back return to back subprocess
retu return to main program
******************************************************************
gas.f Gaussian subprocess
Calls gasset.f first.
User inputs commands
Command What it does Calls on subroutine(s)
-----------------------------------------------------------------------------
) restarts
C restarts
rese resets variables and restarts
retu clear and close plot,go back to main
program
scop n clear 'scope' and plot buffer ga1.f
Inputs as earlier
plot n clear 'plot' and plot buffer ga1.f
Inputs as earlier
psca p1 p2, ) set pixel limits or autoscale ga1.f pscale.f
Inputs as earlier
wsca w1 w2, ) set wavelength limits or autoscale ga1.f wscale.f
Inputs as earlier
ysca y1 y2, ) set y limits or autoscale ga1.f yscale.f
Inputs as earlier
capt INPUT text for caption ga1.f pltcap.f
Inputs as earlier
line n wave put cursor on wavelength for scan n ga1.f
mark use cursor to mark pos. of line for scan n
base cursor marks 4 pos. and set baseline ga1.f
for Gaussian
endp clear and close plot ga1.f
sigm n x INPUT x=sigma of Gaussian for each ga2.f
marked line n
shif x INPUT shift of Gaussian in Angstroms ga2.f
fit( each) fit Gaussian ga2.f
iter x,all iterate fit of Gaussian until fit OK ga2.f
stat write status of variables ga2.f
disp plot (display) Guassian ga2.f
endd clear and close plot ga2.f
****************************************************************************
change.f Change plotting variables subprocess
setchg.f called before commands put in.
User inputs commands
Command What it does Calls on subroutine(s)
-----------------------------------------------------------------------------
retu clear and close plot, return to main
program
rese re-initializes variables
xlin l,rl set flags and labels for linear xycord.f
x axis;specify lambda or rlambda (1/lambda)
xlog l,rl set flags and labels for log xycord.f
x axis;specify lambda or rlambda (1/lambda)
ylin fl,fn,lfl set flags and labels for linear xycord.f
y axis
ylog fl,fn set flags and labels for log xycord.f
y axis
xsca x1 x2,) set x and wavelength limits for plot scalex.f
ysca y1 y2,) set y limits for plot scaley.f
capt INPUT text for caption pltcap.f
dump write variables on screen diag.f
keep n1 -n2 write buffer to DISK2 keep.f
smoo INPUT width of smoothing in Angstroms smooth.f
and DISK2 scans
plot(over) n1-n2 clear and open plot, write capt., u2b.f
plot buffer
scop(eover) n1-n2 clear and open scope, write capt., u2b.f
plot buffer
endp clear and close plot u2b.f
rema use rest of command line for remark
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ripple.f ripple subprocess
User inputs commands
Command What it does Calls on subroutine(s)
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four n1 -n2 normalized window fn.;for each fourie.f
scan, store real, imag., and power
in Fourier transform in next 3 DISK2 scans
hdmp2 n q,p print out Q,U,Err (q) or P,PA, Err (p)
for pol scan n between pscale and wscale limits.
hpri n1 -n2 print out (V), Q,U,E,P,PA for pol hrpolar.f
scans between pscale and wscale limits.
for unbinned printouts of all pixels.
hrec name n1 -n2 change cal. for Q,U,Error from hrpolar.f
one in header to name.hcal
lcal name read calibration file name.lcal lrpolar.f
into buffers
lrec name n1 -n2 change calib. for pol. scans from that lrpolar.f
in header to cal. file name.cal
mark gives x,y cursor posn. for emission line spectr.f
oldc cmd=cent;centroid around line spectr.f
oldf n1 -n2 cmd=four;for each scan, store real, noise.f
imag., and power in Fourier transform in
next 3 DISK2 scans
pow1 name n1 -n2 find power spectrum of PA dist. pow1.f
for scans in list; use lcal file name.lcal
pow3 name n1 -n2 analyze PA ripple for scans pow3.f
in list using lcal file name.lcal; INPUT
maximum pixel shift
samp n1 -n2 samples wavelength onto a linear sample.f
retardation scale, scrunch and store
on DISK2
serk n create Q,U,Err data for Serkowski curve serkow.f
INPUT PA,Pmax,Wmax,DPA, and K', calc.
curve and store in DISK2
slid x n1 -n2 Change C0 to C(1) coeff. by x= slide.f
XSHIFT for all scans, store in DISK2
capt INPUT caption to be used pltcap.f
penup do points on plot pennup.f
pendown do histogram on plot pennup.f
psca p1 p2,) set pixel limits or autoscale pscale.f
wsca w1 w2,) set wave. limits or autoscale wscale.f
ysca y1 y2,) set y limits or autoscale yscale.f
scop n clear and open scope device, write a2b.f
caption and plot buffer contents
plot n clear&open plot device, write caption a2bf.
and plot buffer contents
endp clear and close plot a2b.f
clea clear and close plot a2b.f
read (options) read in 2 echelle text files (A&B reade.f
arrays), store in DISK2; INPUT name,
starslit, 1/2 wave filter, exp. time,
A array and B array files
bufs print values of variables in buffers bufstat.f
crza (ops) n1-n2 eliminate negative pixels and ones crzap.f
over and under threshold in DISK1 scanlist
pbo load thermal and scat. light corr. tmpobserv.f
comb n1 -n2 combines scrunched spectra, store tmpf2b.f
in DISK2
fakb n create fake background and store in fakbkg.f
DISK1; use scan n as header template
seti set int. frame time; INPUT value of setifr.f
frametime
retu return to main program
rema use rest of line as remark